FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Kosugi, T Matsuzaki, K Sakao, T Shimizu, T Sone, Y Tachikawa, S Hashimoto, T Minesugi, K Ohnishi, A Yamada, T Tsuneta, S Hara, H Ichimoto, K Suematsu, Y Shimojo, M Watanabe, T Shimada, S Davis, JM Hill, LD Owens, JK Title, AM Culhane, JL Harra, LK Doschek, GA Golub, L AF Kosugi, T. Matsuzaki, K. Sakao, T. Shimizu, T. Sone, Y. Tachikawa, S. Hashimoto, T. Minesugi, K. Ohnishi, A. Yamada, T. Tsuneta, S. Hara, H. Ichimoto, K. Suematsu, Y. Shimojo, M. Watanabe, T. Shimada, S. Davis, J. M. Hill, L. D. Owens, J. K. Title, A. M. Culhane, J. L. Harra, L. K. Doschek, G. A. Golub, L. TI The Hinode (Solar-B) mission: An overview SO SOLAR PHYSICS LA English DT Article ID MAGNETIC RECONNECTION; FLARE; CORONA; POINT; LOOPS AB The Hinode satellite (formerly Solar-B) of the Japan Aerospace Exploration Agency's Institute of Space and Astronautical Science (ISAS/JAXA) was successfully launched in September 2006. As the successor to the Yohkoh mission, it aims to understand how magnetic energy gets transferred from the photosphere to the upper atmosphere and results in explosive energy releases. Hinode is an observatory style mission, with all the instruments being designed and built to work together to address the science aims. There are three instruments onboard: the Solar Optical Telescope (SOT), the EUV Imaging Spectrometer (EIS), and the X-Ray Telescope (XRT). This paper provides an overview of the mission, detailing the satellite, the scientific payload, and operations. It will conclude with discussions on how the international science community can participate in the analysis of the mission data. C1 Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. Natl Astron Observ, Tokyo 1818588, Japan. Mitsubishi Electr Corp, Kamakura Works, Kanagawa 2478520, Japan. NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Shimizu, T (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. EM shimizu@solar.isas.jaxa.jp RI Shimojo, Masumi/J-2605-2016; OI Shimojo, Masumi/0000-0002-2350-3749; Harra, Louise/0000-0001-9457-6200; Golub, Leon/0000-0001-9638-3082 NR 23 TC 958 Z9 965 U1 7 U2 56 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2007 VL 243 IS 1 BP 3 EP 17 DI 10.1007/s11207-007-9014-6 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 215JB UT WOS:000249803500002 ER PT J AU Golub, L DeLuca, E Austin, G Bookbinder, J Caldwell, D Cheimets, P Cirtain, J Cosmo, M Reid, P Sette, A Weber, M Sakao, T Kano, R Shibasaki, K Hara, H Tsuneta, S Kumagai, K Tamura, T Shimojo, M McCracken, J Carpenter, J Haight, H Siler, R Wright, E Tucker, J Rutledge, H Barbera, M Peres, G Varisco, S AF Golub, L. DeLuca, E. Austin, G. Bookbinder, J. Caldwell, D. Cheimets, P. Cirtain, J. Cosmo, M. Reid, P. Sette, A. Weber, M. Sakao, T. Kano, R. Shibasaki, K. Hara, H. Tsuneta, S. Kumagai, K. Tamura, T. Shimojo, M. McCracken, J. Carpenter, J. Haight, H. Siler, R. Wright, E. Tucker, J. Rutledge, H. Barbera, M. Peres, G. Varisco, S. TI The X-ray telescope (XRT) for the Hinode mission SO SOLAR PHYSICS LA English DT Article ID I TELESCOPE; ABERRATION AB The X-ray Telescope (XRT) of the Hinode mission provides an unprecedented combination of spatial and temporal resolution in solar coronal studies. The high sensitivity and broad dynamic range of XRT, coupled with the spacecraft's onboard memory capacity and the planned downlink capability will permit a broad range of coronal studies over an extended period of time, for targets ranging from quiet Sun to X-flares. This paper discusses in detail the design, calibration, and measured performance of the XRT instrument up to the focal plane. The CCD camera and data handling are discussed separately in a companion paper. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. Natl Astron Observ, Tokyo 1818588, Japan. Natl Astron Observ, Nobeyama Solar Radio Observ, Minamisa Ku, Nagano 3841305, Japan. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Osservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy. RP Golub, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lgolub@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013; Shimojo, Masumi/J-2605-2016; OI DeLuca, Edward/0000-0001-7416-2895; Shimojo, Masumi/0000-0002-2350-3749; Barbera, Marco/0000-0002-3188-7420; PERES, Giovanni/0000-0002-6033-8180; Varisco, Salvatore/0000-0002-6891-8390 NR 11 TC 393 Z9 397 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2007 VL 243 IS 1 BP 63 EP 86 DI 10.1007/s11207-007-0182-1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 215JB UT WOS:000249803500004 ER PT J AU Matsuzaki, K Shimojo, M Tarbell, TD Harra, LK Deluca, EE AF Matsuzaki, K. Shimojo, M. Tarbell, T. D. Harra, L. K. Deluca, E. E. TI Data archive of the Hinode mission SO SOLAR PHYSICS LA English DT Article ID SYSTEM DARTS; FITS; ISAS AB All of the Hinode telemetry data are to be reformatted and archived in the DARTS system at ISAS and mirrored to data centers around the word. The archived data are distributed to users through the Internet. This paper gives an overview of the files in the archive, including the file formats. All formats are portable and have heritage from the previous missions. From the reformatted files, index information is created for faster data search. Users can perform queries based on information contained in the index. This allows for searches to return observations that conform to particular observing conditions. C1 Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. Natl Astron Observ, Nobeyama Solar Radio Observ, Nagano 3841305, Japan. Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94204 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Matsuzaki, K (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. EM matuzaki@solar.isas.ac.jp RI DeLuca, Edward/L-7534-2013; Shimojo, Masumi/J-2605-2016; OI DeLuca, Edward/0000-0001-7416-2895; Shimojo, Masumi/0000-0002-2350-3749; Harra, Louise/0000-0001-9457-6200 NR 10 TC 10 Z9 10 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2007 VL 243 IS 1 BP 87 EP 92 DI 10.1007/s11207-006-0303-2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 215JB UT WOS:000249803500005 ER PT J AU Valcu, B Smith, PL Gardner, LD Raymond, JC Miralles, MP Kohl, JL AF Valcu, Bogdan Smith, Peter L. Gardner, Larry D. Raymond, John C. Miralles, Mari-Paz Kohl, John L. TI Tracking UVCS/SOHO responsivity with observations of zeta Tau SO SOLAR PHYSICS LA English DT Article ID SOHO MISSION; UVCS; INSTRUMENTATION; CALIBRATION; SATELLITE; DETECTORS; SOLAR AB We have tracked the spectral responsivity of the ultraviolet channels of the UVCS ( Ultraviolet Coronagraph Spectrometer) instrument on SOHO by repeated observations of a stable hot star. We demonstrate first that the ultraviolet spectral irradiance of the Be star. Tau ( HD 37202) for the 100- to 125- nm wavelength range has been sufficiently constant for our purposes when measured periodically over the course of the SOHO mission. We then use. Tau as a radiometric transfer standard to determine an average decrease beginning in November of 1998 of 13.0% per year in the responsivity of the UVCS O VI channel for wavelengths near H I Ly alpha and for a particular UVCS unvignetted aperture used for science observations. The calibration tracking method involves separating two. Tau spectral regions that are overlapped on part of the detector. The change in the responsivity of UVCS/SOHO began in late 1998 as determined by comparison of simultaneous observations of the corona carried out with UVCS/SOHO and the freshly-calibrated UVCS instrument on the Spartan 201 satellite in early November of 1998. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Muskingum Coll, New Concord, OH 43762 USA. RP Gardner, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bogdan.valcu@brainlab.com; plsmith@cfa.harvard.edu; lgardner@cfa.harvard.edu; mmiralles@cfa.harvard.edu; jkohl@cfa.harvard.edu NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2007 VL 243 IS 1 BP 93 EP 104 DI 10.1007/s11207-007-0377-5 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 215JB UT WOS:000249803500006 ER PT J AU Slavin, JD Frisch, PC AF Slavin, Jonathan D. Frisch, Priscilla C. TI The chemical composition of interstellar matter at the solar location SO SPACE SCIENCE REVIEWS LA English DT Review DE ISM : abundances; ISM : individual (Local Interstellar Cloud) ID IONIZATION; SPECTRA AB The Local Interstellar Cloud (LIC) surrounds the Solar System and sets the boundary conditions for the heliosphere. Using both in situ and absorption line data towards epsilon CMa we are able to constrain both the ionization and the gas phase abundances of the LIC gas at the Solar Location. We find that the abundances are consistent with all of the carbonaceous dust grains having been destroyed, and in fact with a supersolar abundance of C. The constituents of silicate grains, Si, Mg, and Fe, appear to be sub-solar, indicating that silicate dust is present in the LIC. N, O and S are close to the solar values. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Slavin, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 83, Cambridge, MA 02138 USA. EM jslavin@cfa.harvard.edu OI Slavin, Jonathan/0000-0002-7597-6935 NR 12 TC 15 Z9 15 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUN PY 2007 VL 130 IS 1-4 BP 409 EP 414 DI 10.1007/s11214-007-9186-2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 213GA UT WOS:000249653200041 ER PT J AU Marvin, U AF Marvin, Ursula TI Charles Darwin, geologist SO VICTORIAN STUDIES LA English DT Book Review C1 [Marvin, Ursula] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marvin, U (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU INDIANA UNIV PRESS PI BLOOMINGTON PA 601 N MORTON STREET, BLOOMINGTON, IN 47404-3797 USA SN 0042-5222 J9 VICTORIAN STUD JI Vic. Stud. PD SUM PY 2007 VL 49 IS 4 BP 712 EP 714 DI 10.2979/VIC.2007.49.4.712 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 244BJ UT WOS:000251840700021 ER PT J AU Qin, Q Loeffler, IK Li, M Tian, KG Wei, FW AF Qin, Qin Loeffler, I. Kati Li, Ming Tian, Kegong Wei, Fuwen TI Sequence analysis of a canine parvovirus isolated from a red panda (Ailurus fulgens) in China SO VIRUS GENES LA English DT Article DE canine parvovirus; VP2 gene; red panda; Ailurus fulgens ID HOST-RANGE; FELINE; EVOLUTION AB Canine parvovirus (CPV) was first recognized in the late 1970 s in dogs and has mutated and spread throughout the world in canid and felid species since then. In this study, a novel CPV was isolated from the endangered red panda (Ailurus fulgens) in China. Nucleotide and phylogenetic analysis of the capsid protein VP2 gene classified the red panda parvovirus (RPPV) as a CPV-2a type. Substitution of Val for Gly at the conserved 300 residue in RPPV presents an unusual variation in the CPV-2a amino acid sequence and is further evidence for the continuing evolution of the virus. The 300 residue is important in distinguishing the antigenicity and host range of CPVs. The clinical significance and population impact of RPPV infection in captive red pandas in China is unknown and is an important topic for future research. C1 Chinese Acad Sci, Inst Zool, Beijing 100080, Peoples R China. Chinese Acad Sci, Grad Sch, Beijing 100080, Peoples R China. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Minist Agr People Republ China, Natl Vet Diagnost Ctr, Beijing 100094, Peoples R China. RP Loeffler, IK (reprint author), Chinese Acad Sci, Inst Zool, 25 Beisihuan Xilu, Beijing 100080, Peoples R China. EM katiloffler@yahoo.com; tiankg@263.net NR 10 TC 13 Z9 15 U1 2 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0920-8569 J9 VIRUS GENES JI Virus Genes PD JUN PY 2007 VL 34 IS 3 BP 299 EP 302 DI 10.1007/s11262-006-0023-6 PG 4 WC Genetics & Heredity; Virology SC Genetics & Heredity; Virology GA 149WJ UT WOS:000245177300008 PM 16927123 ER PT J AU Kushlan, JA Angehr, GR AF Kushlan, James A. Angehr, George R. TI Seaside tiger herons SO WATERBIRDS LA English DT Article DE behavior; coastal; display; foraging; gulf of Panama; herons; marine; nesting; Pearl Islands; Republic of Panama; territoriality; tiger herons AB Tiger Herons (Tigrisoma) are little studied and generally characterized in the literature as being relatively uncommon birds of forested streams and wetlands. Contrary to these expectations, we found Bare-throated Tiger Herons (Tigrisoma lineatum) on the Pearl Islands of the Gulf of Panama to be birds of open, wave-exposed rocky seashores. We also found them to be common birds, inhabiting most shoreline coves. They fed over much of the tidal cycle along beaches and rocky shores, especially on and near surf-washed rocks. They caught crabs and fish by standing and walking slowly and methodically. Feeding efficiency was low, averaging about one prey item per hour. Plumage coloration is highly cryptic against shore rocks; but, in contrast, the bird becomes quite obvious when it expands its bare yellow throat, especially when accentuating a distinctive stretch display used to claim shoreline territory and for within-pair interactions. Tiger herons in the Pearls nested high in trees on ocean-facing cliffs. The habitat choice and behavior of this population of tiger herons that we report extend understanding of the biological scope of the subfamily of tiger herons. C1 Smithsonian Trop Res Inst, STRI Unit 0948, APO, AA 34002 USA. RP Kushlan, JA (reprint author), POB 2008, Key Biscayne, FL 33149 USA. EM jkushlan@earthlink.net NR 4 TC 3 Z9 3 U1 1 U2 4 PU WATERBIRD SOC PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 1524-4695 J9 WATERBIRDS JI Waterbirds PD JUN PY 2007 VL 30 IS 2 BP 278 EP 283 DI 10.1675/1524-4695(2007)30[278:STH]2.0.CO;2 PG 6 WC Ornithology SC Zoology GA 191KN UT WOS:000248130200015 ER PT J AU Deutsch, J AF Deutsch, James TI Who is Bozo Texino?: The secret history of hobo graffiti SO WESTERN FOLKLORE LA English DT Book Review C1 [Deutsch, James] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 1 PU CALIFORNIA FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD SUM-FAL PY 2007 VL 66 IS 3-4 BP 417 EP 418 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA 285HH UT WOS:000254767400021 ER PT J AU Cornell, JA Craft, CB Megonigal, JP AF Cornell, Jeff A. Craft, Christopher B. Megonigal, J. Patrick TI Ecosystem gas exchange across a created salt marsh chronosequence SO WETLANDS LA English DT Article DE carbon cycle; created marsh; gas exchange; Spartina alterniflora; succession ID CORDGRASS SPARTINA-FOLIOSA; ORGANIC-CARBON; ALTERNIFLORA; NITROGEN; WETLANDS; PHOSPHORUS; PROGRESS; LITTER; GROWTH; BAY AB Salt marshes created on dredge spoil were compared to natural marshes to evaluate the capacity of created marshes to perform carbon cycle functions. Several carbon cycle attributes were measured in eight created Spartina alterniflora Loisel salt marshes that ranged from one to 28 years, each paired with a nearby mature natural reference marsh. The attributes measured included gross primary production, respiration, net ecosystem exchange, potential microbial respiration (CH4 and CO2), and above ground biomass. In situ exchange rates of CO2 and plant biomass in created marshes met or exceeded those of reference marshes in three to four years. There was some evidence that ecosystem gas exchange in created marshes developed slightly faster than aboveground biomass production. Soil carbon mineralization per gram carbon was generally higher in the created marshes than reference marshes, suggesting higher carbon quality and/or nutrient availability in the created marshes. However, carbon mineralization rates per gram soil were relatively low in the created marshes due to lower soil organic matter content. With proper construction, we suggest most major carbon fluxes can be established in created salt marshes in less than five years. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Indiana Univ, Sch Publ & Environm Affairs, Bloomington, IN 47405 USA. George Mason Univ, Fairfax, VA 22030 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contess Wharf Rd, Edgewater, MD 21037 USA. EM megonigalp@si.edu NR 33 TC 18 Z9 20 U1 2 U2 33 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 2007 VL 27 IS 2 BP 240 EP 250 DI 10.1672/0277-5212(2007)27[240:EGEAAC]2.0.CO;2 PG 11 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 181FS UT WOS:000247423000004 ER PT J AU Zanol, J Fauchald, K Paiva, PC AF Zanol, Joana Fauchald, Kristian Paiva, Paulo C. TI A phylogenetic analysis of the genus Eunice (Eunicidae, polychaete, Annelida) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE branchial distribution; Eunicida; jaw; Leodice; mandible; maxillae; phylogeny; subacicular hooks ID BOOTSTRAP; LIMITS; REEFS AB Species of Eunice are distributed worldwide, inhabiting soft and hard marine bottoms. Some of these species play significant roles in coral reef communities and others are commercially important. Eunice is the largest and most poorly defined genus in Eunicidae. It has traditionally been subdivided in taxonomically informal groups based on the colour and dentition of subacicular hooks, and branchial distribution. The monophyly of Eunice and of its informal subgroups is tested here using cladistic analyses of 24 ingroup species based on morphological data. In the phylogenetic hypothesis resulting from the present analyses Eunice and its subgroups are paraphyletic; the genus may be divided in at least two monophyletic groups, Eunice s.s. and Leodice, but several species do not fall inside these two groups. Most of the traditional characters used in the taxonomy of Eunice are homoplasies; however, characters used for the first time in this study, such as certain jaw characters and characters derived from a close examination of chaetal variation along the body, are promising sources of phylogenetic signal. (c) 2007 The Linnean Society of London, Zoological Journal of the Linnean Society, 2007, 150, 413-434. C1 Univ Fed Rio de Janeiro, Pos Grad Zool, Museu Nacl, BR-20940040 Rio De Janeiro, Brazil. Smithsonian Inst, Dept Invertebrate Zool, NMNH, NHB MRC 0163, Washington, DC 20013 USA. Univ Fed Rio de Janeiro, Inst Biol, Dept Zool, BR-2240590 Rio De Janeiro, RJ, Brazil. RP Zanol, J (reprint author), George Washington Univ, Dept Biol Sci, 2023 G St NW, Washington, DC 20052 USA. EM jzanol@gwu.edu RI Paiva, Paulo/I-6174-2012; Zanol, Joana/J-6263-2016; OI Zanol, Joana/0000-0002-2178-791X; Paiva, Paulo Cesar de/0000-0003-1061-6549 NR 75 TC 13 Z9 14 U1 1 U2 9 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 JUN PY 2007 VL 150 IS 2 BP 413 EP 434 DI 10.1111/j.1096-3642.2007.00302.x PG 22 WC Zoology SC Zoology GA 178FL UT WOS:000247206500005 ER PT J AU Cisneros-Heredia, DF Meza-Ramos, P AF Cisneros-Heredia, Diego F. Meza-Ramos, Paul TI An enigmatic new species of glassfrog (Amphibia : Anura : Centrolenidae) from the Amazonian Andean slopes of Ecuador SO ZOOTAXA LA English DT Article DE Cochranella amelie; new species; taxonomy; Oglan River; Pastaza; Ecuador ID FROG ANURA; SYSTEMATICS AB We describe a new species of frog of the family Centrolenidae, Cochranella amelie n. sp., from the central Amazonian Andean slopes, collected at the Oglan River, Province of Pastaza, Ecuador. This new species shows a very unusual combination of characters ( lavender dorsum in preservative, absence of a humeral spine in adult males, transparent parietal peritoneum, white visceral peritonea, and bulbous liver). The relationships of this new species of Glassfrog are uncertain, and its assignment to Cochranella is preliminary. C1 Univ San Francisco Quito, Coll Biol & Environm Sci, Quito, Ecuador. Smithsonian Inst, Natl Museum Nat Hist, Res Training Program 2002, Washington, DC 20560 USA. Museo Ecuatoriano Ciencias Nat, Secc Vertebrados, Div Herpetol, Quito, Ecuador. RP Cisneros-Heredia, DF (reprint author), Kings Coll London, Dept Geog, London WC2R 2LS, England. EM diegofrancisco_cisneros@yahoo.com; diegofrancisco.cisneros@gmail.com RI Cisneros-Heredia, Diego/D-1744-2011 OI Cisneros-Heredia, Diego/0000-0002-6132-2738 NR 34 TC 4 Z9 6 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 28 PY 2007 IS 1485 BP 33 EP 41 PG 9 WC Zoology SC Zoology GA 172DE UT WOS:000246783500003 ER PT J AU Puebla, O Bermingham, E Guichard, F Whiteman, E AF Puebla, Oscar Bermingham, Eldredge Guichard, Frederic Whiteman, Elizabeth TI Colour pattern as a single trait driving speciation in Hypoplectrus coral reef fishes? SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE speciation; coral reef fishes; colour pattern; population genetics; assortative mating; aggressive mimicry ID HAMLETS HYPOPLECTRUS; REPRODUCTIVE ISOLATION; CLEANING SYMBIOSIS; SERRANIDAE; EVOLUTION; DIFFERENTIATION; DIVERGENCE; SELECTION; MIMICRY AB Theory shows that speciation in the presence of gene flow occurs only under narrow conditions. One of the most favourable scenarios for speciation with gene flow is established when a single trait is both under disruptive natural selection and used to cue assortative mating. Here, we demonstrate the potential for a single trait, colour pattern, to drive incipient speciation in the genus Hypoplectrus (Serranidae), coral reef fishes known for their striking colour polymorphism. We provide data demonstrating that sympatric Hypoplectrus colour morphs mate assortatively and are genetically distinct. Furthermore, we identify ecological conditions conducive to disruptive selection on colour pattern by presenting behavioural evidence of aggressive mimicry, whereby predatory Hypoplectrus colour morphs mimic the colour patterns of non-predatory reef fish species to increase their success approaching and attacking prey. We propose that colour-based assortative mating, combined with disruptive selection on colour pattern, is driving speciation in Hypoplectrus coral reef fishes. C1 Smithsonian Trop Res Inst, Balboa, Panama. McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Univ E Anglia, Sch Biol Sci, Ctr Ecol Evolut & Conservat, Norwich NR4 7TJ, Norfolk, England. RP Puebla, O (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Panama. EM oscar.puebla@mcgill.ca RI Guichard, Frederic/B-6188-2015 OI Guichard, Frederic/0000-0002-7369-482X NR 37 TC 74 Z9 78 U1 6 U2 32 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD MAY 22 PY 2007 VL 274 IS 1615 BP 1265 EP 1271 DI 10.1098/rspb.2006.0435 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 151PE UT WOS:000245301900004 PM 17360287 ER PT J AU Gottlieb, CA Brunken, S McCarthy, MC Thaddeus, P AF Gottlieb, C. A. Brunken, S. McCarthy, M. C. Thaddeus, P. TI The rotational spectrum of CN- SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SPECTROSCOPIC PROPERTIES; ELECTRON-ATTACHMENT; NEGATIVE-IONS; MILLIMETER; ANIONS; CLOUDS; CS AB The rotational spectrum of the molecular negative ion CN- has been detected in the laboratory at high resolution. The four lowest transitions were observed in a low pressure glow discharge through C2N2 and N-2. Conclusive evidence for the identification was provided by well-resolved nitrogen quadrupole hyperfine structure in the lowest rotational transition, and a measurable Doppler shift owing to ion drift in the positive column of the discharge. Three spectroscopic constants (B, D, and eQq) reproduce the observed spectrum to within one part in 10(7) or better, allowing the entire rotational spectrum to be calculated well into the far IR to within 1 km s(-1) in equivalent radial velocity. CN- is an excellent candidate for astronomical detection, because the CN radical is observed in many galactic molecular sources, the electron binding energy of CN- is large, and calculations indicate CN- should be detectable in IRC+10216-the carbon star where C6H- has recently been observed. The fairly high concentration of CN- in the discharge implies that other molecular anions containing the nitrile group may be within reach. (C) 2007 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Gottlieb, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; McCarthy, Michael/0000-0001-9142-0008 NR 25 TC 22 Z9 22 U1 3 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 21 PY 2007 VL 126 IS 19 AR 191101 DI 10.1063/1.2737442 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 170EZ UT WOS:000246646600001 PM 17523781 ER PT J AU Dobler, G Keeton, CR Wambsganss, J AF Dobler, Gregory Keeton, Charles R. Wambsganss, Joachim TI Microlensing of central images in strong gravitational lens systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; galaxies : stellar content ID QUASAR ACCRETION DISK; PROBABILITY-DISTRIBUTIONS; LIGHT CURVES; HIGH-MAGNIFICATION; MASS FUNCTION; BLACK-HOLES; GALAXIES; VARIABILITY; STATISTICS; FLUCTUATIONS AB We study microlensing of the faint images that form close to the centres of strong gravitational lens galaxies. These central images, which have finally begun to yield to observations, naturally appear in dense stellar fields and may be particularly sensitive to fine granularity in the mass distribution. The microlensing magnification maps for overfocused (i.e. demagnified) images differ strikingly from those for magnified images. In particular, the familiar 'fold' and 'cusp' features of maps for magnified images are only present for certain values of the fraction f of the surface mass density contained in stars. For central images, the dispersion in microlensing magnifications is generally larger than for normal (minimum and saddle) images, especially when the source is comparable to or larger than the stellar Einstein radius. The dispersion depends in a complicated way on f; this behaviour may hold the key to using microlensing as a probe of the relative densities of stars and dark matter in the cores of distant galaxies. Quantitatively, we predict that the central image C in PMN J1632-0033 has a magnification dispersion of 0.6 mag for R-src/R-E less than or similar to 1, or 0.3 mag for R-src/R-E = 10. For comparison, the dispersions are 0.5-0.6 mag for image B and 0.05-0.1 mag for image A, if R-src/R-E less than or similar to 1; and just 0.1 mag for B and 0.008 mag for A if R-src/R-E = 10. (The dispersions can be extrapolated to larger sources sizes as sigma proportional to R-src(-1).) Thus, central images are more susceptible than other lensed images to microlensing and hence good probes for measuring source sizes. C1 Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Univ Heidelberg, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. RP Dobler, G (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. EM gdobler@cfa.harvard.edu NR 63 TC 7 Z9 7 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 MAY 21 PY 2007 VL 377 IS 3 BP 977 EP 986 DI 10.1111/j.1365-2966.2007.11695.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166GS UT WOS:000246367000003 ER PT J AU McQuinn, M Lidz, A Zahn, O Dutta, S Hernquist, L Zaldarriaga, M AF McQuinn, Matthew Lidz, Adam Zahn, Oliver Dutta, Suvendra Hernquist, Lars Zaldarriaga, Matias TI The morphology of HII regions during reionization SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : formation; intergalactic medium; cosmology : theory; diffuse radiation; large-scale structure of Universe; radio lines : galaxies ID SIMULATING COSMIC REIONIZATION; 21 CENTIMETER FLUCTUATIONS; GUNN-PETERSON TROUGH; ALPHA EMISSION-LINES; DARK-MATTER HALOES; HIGH-REDSHIFT; STAR-FORMATION; STELLAR SOURCES; COSMOLOGICAL REIONIZATION; HYDROGEN REIONIZATION AB It is possible that the properties of H II regions during reionization depend sensitively on many poorly constrained quantities [the nature of the ionizing sources, the clumpiness of the gas in the intergalactic medium (IGM), the degree to which photoionizing feedback suppresses the abundance of low-mass galaxies, etc.], making it extremely difficult to interpret upcoming observations of this epoch. We demonstrate that the actual situation is more encouraging, using a suite of radiative transfer simulations, post-processed on outputs from a 10243, 94-Mpc N-body simulation. Analytic prescriptions are used to incorporate small-scale structures that affect reionization, yet remain unresolved in the N-body simulation. We show that the morphology of the H II regions for reionization by POPII-like stars is most dependent on the global ionization fraction (x) over bar (i). Changing other parameters by an order of magnitude for fixed (x) over bar (i) often results in similar bubble sizes and shapes. The next most important dependence is on the properties of the ionizing sources. The rarer the sources, the larger and more spherical the H II regions become. The typical bubble size can vary by as much as a factor of 4 at fixed (x) over bar (i) xi between different possible source prescriptions. The final relevant factor is the abundance of minihaloes or of Lyman-limit systems. These systems suppress the largest bubbles from growing, and the magnitude of this suppression depends on the thermal history of the gas as well as the rate at which these systems are photo-evaporated. We find that neither source suppression owing to photo-heating nor small-scale gas clumping significantly affects the large-scale structure of the H II regions, with the ionization fraction power spectrum at fixed (x) over bar (i) differing by less than 20 per cent for k < 5 Mpc(-1) between all the source suppression and clumping models we consider. Analytic models of reionization are successful at predicting many of the features seen in our simulations. We discuss how observations of the 21-cm line with the Mileura Widefield Array (MWA) and the Low Frequency Array (LOFAR) can constrain properties of reionization, and we study the effect patchy reionization has on the statistics of Ly alpha emitting galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Heidelberg, Inst Theoret Astrophys, D-69117 Heidelberg, Germany. Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP McQuinn, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmcquinn@cfa.harvard.edu NR 83 TC 198 Z9 198 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 MAY 21 PY 2007 VL 377 IS 3 BP 1043 EP 1063 DI 10.1111/j.1365-2966.2007.11489.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166GS UT WOS:000246367000009 ER PT J AU Tang, SM Zhang, SN Hopkins, PF AF Tang, Su Min Zhang, Shuang Nan Hopkins, Philip F. TI Is the dependence of spectral index on luminosity real in optically selected AGN samples ? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : statistical; galaxies : active; quasars : general; X-rays : galaxies ID SOFT-X-RAY; ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; COSMOLOGICAL EVOLUTION; ENERGY-DISTRIBUTION; QUASAR SURVEY; RADIO-QUIET; CHANDRA; EMISSION; REGRESSION AB We critically examine the dependence of spectral index on luminosity in optically selected AGN samples. An analysis of optically selected high-z quasars showed an anticorrelation of alpha(OX), the spectral index between the rest-frame 2500 angstrom and 2 keV, with optical luminosity. We examine this relationship by means of Monte Carlo simulations and conclude that a constant alpha(OX) independent of optical luminosity is still consistent with this high-z sample. We further find that contributions of large dispersions and narrow range of optical luminosity are most important for the apparent, yet artificial, alpha(OX)-l(o) correlation reported. We also examine another, but more complete, low-z optical selected AGN sub-sample from Steffen et al., and our analysis shows that a constant alpha(OX) independent of optical luminosity is also consistent with the data. By comparing X-ray and optical luminosity functions, we find that a luminosity-independent alpha(OX) is in fact more preferred than the luminosity-dependent alpha(OX) model. We also discuss the selection effects caused by flux limits, which might systematically bias the l(X)-l(o) relation and cause discrepancy in optically selected and X-ray selected AGN samples. To correctly establish a dependence of alpha(OX) of AGNs on their luminosity, a larger and more complete sample is needed and consequences of luminosity dispersions and selection effects in flux-limited samples must be taken into account properly. C1 Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35812 USA. Chinese Acad Sci, Inst High Energy Phys, Beijing 100039, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tang, SM (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM stang@cfa.harvard.edu; zhangsn@tsinghua.edu.cn NR 33 TC 14 Z9 14 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2007 VL 377 IS 3 BP 1113 EP 1121 DI 10.1111/j.1365-2966.2007.11589.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166GS UT WOS:000246367000013 ER PT J AU Jonker, PG Bassa, CG Wachter, S AF Jonker, P. G. Bassa, C. G. Wachter, S. TI The quasi-persistent neutron star soft X-ray transient 1M 1716-315 in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion : accretion discs; stars : individual; 1M 1716-315; binaries : general; stars : neutron; X-rays : binaries ID ULTRACOMPACT BINARIES; CHANDRA OBSERVATIONS; CATALOG; BURST; LUMINOSITIES; KS-1731-260; EMISSION; PULSARS; EXOSAT AB We report on our analysis of a 20 ks Chandra X-ray observation of the quasi-persistent neutron star soft X-ray transient (SXT) 1M 1716-315 in quiescence. Only one source was detected in the HEAO-1 error region. Its luminosity is 1.6 x 10(32)-1.3 x 10(33) erg s(-1). In this, the range is dominated by the uncertainty in the source distance. The source spectrum is well described by an absorbed soft spectrum, e.g. a neutron star atmosphere or blackbody model. No optical or near-infrared counterpart is present at the location of the X-ray source, down to a magnitude limit of I empty set 23.5 and K-s empty set 19.5. The positional evidence, the soft X-ray spectrum together with the optical and near-infrared non-detections provide strong evidence that this source is the quiescent neutron star SXT. The source is 10-100 times too bright in X-rays in order to be explained by stellar coronal X-ray emission. Together with the interstellar extinction measured in outburst and estimates for the source distance, the reported optical and near-infrared limit give an upper limit on the absolute magnitude of the counterpart of I > 8.6 and K-s > 5.1. This implies that the system is either an ultra-compact X-ray binary having P-orb < 1 h or the companion star is an M-dwarf. We reconstructed the long-term X-ray light curve of the source. 1M 1716-315 has been active for more than 12 yr before returning to quiescence, the reported Chandra observation started 16.9 +/- 4.1 yr after the outburst ended. C1 SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl NR 41 TC 9 Z9 9 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2007 VL 377 IS 3 BP 1295 EP 1300 DI 10.1111/j.1365-2966.2007.11689.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166GS UT WOS:000246367000030 ER PT J AU Bowman, JD Morales, MF Hewitt, JN AF Bowman, Judd D. Morales, Miguel F. Hewitt, Jacqueline N. TI Constraints on fundamental cosmological parameters with upcoming redshifted 21 cm observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; intergalactic medium; radio lines : general; techniques : interferometric ID MICROWAVE BACKGROUND ANISOTROPIES; PROBING DARK ENERGY; CENTIMETER FLUCTUATIONS; POWER SPECTRUM; REIONIZATION OBSERVATORIES; EPOCH; GAS; FOREGROUNDS; TOMOGRAPHY; EMISSION AB Constraints on cosmological parameters from upcoming measurements with the Mileura Wide-field Array Low Frequency Demonstrator (MWALFD) of the redshifted 21 cm power spectrum are forecasted assuming a flat Lambda CDM cosmology and assuming that the reionization of neutral hydrogen in the intergalactic medium occurs below a redshift of z = 8. We find that observations with the MWA LFD cannot constrain the underlying cosmology in this scenario. In principle, a similar experiment with a 10-fold increase in collecting area could provide useful constraints on the slope of the inflationary power spectrum, n(s), and the running of the spectral index, alpha(s), but these constraints are subject to the caveat that even a small reionization contribution could be confused with the cosmological signal. In addition to the redshifted 21 cm signal, we include two nuisance components in our analysis related to the systematics and astrophysical foregrounds present in low-frequency radio observations. These components are found to be well separated from the signal and contribute little uncertainty (< 30%) to the measured values of the cosmological model parameters. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bowman, JD (reprint author), MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. NR 46 TC 42 Z9 42 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2007 VL 661 IS 1 BP 1 EP 9 DI 10.1086/516560 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EE UT WOS:000246574700001 ER PT J AU Gugliucci, NE Taylor, GB Peck, AB Giroletti, M AF Gugliucci, N. E. Taylor, G. B. Peck, A. B. Giroletti, M. TI Polarimetry of 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; SCALE ROTATION MEASURES; FARADAYS FOG; COINS SAMPLE; AGES; JETS; IDENTIFICATIONS; ABSORPTION; EVOLUTION AB We present multifrequency VLBA observations of two polarized Compact Symmetric Objects (CSOs), J0000+ 4054 and J1826+1831, and a polarized CSO candidate, J1915+ 6548. Using the wavelength-squared dependence of Faraday rotation, we obtained rotation measures (RMs) of - 180 +/- 10 rad m(-2) and 1540 +/- 7 rad m(-2) for the latter two sources. These are lower than what is expected of CSOs (several 1000 rad m(-2)) and, depending on the path length of the Faraday screens, require magnetic fields from 0.03 to 6 mu G. These CSOs may be more heavily affected by Doppler boosting than their unpolarized counterparts, suggesting that a jet-axis orientation more inclined toward the line of sight is necessary to detect any polarization. This allows for low RMs if the polarized components are oriented away from the depolarizing circumnuclear torus. These observations also add a fourth epoch to the proper-motion studies of J0000+4054 and J1826+1831, constraining their kinematic age estimates to > 610 and 2600 +/- 490 yr, respectively. The morphology, spectrum, and component motions of J1915+6548 are discussed in light of its new classification as a CSO candidate, and its angle to the line of sight (similar to 50 degrees) is determined from relativistic beaming arguments. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. Harvard Smithsonian Ctr Astrophys, SAO SMA Project, Hilo, HI 96720 USA. INAF, Inst Radioastron, I-40129 Bologna, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Gugliucci, NE (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. EM neg9j@virginia.edu; gbtaylor@unm.edu; apeck@cfa.harvard.edu; giroletti@ira.inaf.it OI Giroletti, Marcello/0000-0002-8657-8852 NR 39 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2007 VL 661 IS 1 BP 78 EP 87 DI 10.1086/515560 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EE UT WOS:000246574700009 ER PT J AU Zezas, A Fabbiano, G Baldi, A Schweizer, F King, AR Rots, AH Ponman, TJ AF Zezas, A. Fabbiano, G. Baldi, A. Schweizer, Francois King, A. R. Rots, A. H. Ponman, T. J. TI Chandra monitoring observations of the antennae galaxies. II. Ray luminosity functions SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : interactions; galaxies : peculiar; X-rays : galaxies ID THICK ACCRETION DISKS; BLACK-HOLES; STATISTICAL PROPERTIES; LIKELIHOOD ESTIMATION; NEARBY GALAXIES; RADIO-SOURCES; BINARIES; NUMBER; NGC-4038/4039; POPULATIONS AB We present the X-ray luminosity functions (XLFs) of the X-ray source population detected in the Chandra monitoring observations of NGC 4038/4039 (the Antennae). The seven individual XLFs are well described by a flat power law with a cumulative slope alpha similar to 0.5-0.8. A similar slope ( similar to = 0.48(-0.08)(+0.09)) is measured for the sources detected in the co-added observation, which reaches a limiting luminosity of similar to 10(37) erg s(-1). In our analysis we account for observational biases by deriving incompleteness functions and including them in the fitting process. We do not detect significant variations between the shape of the XLF of the seven observations. The two shorter exposures appear to have steeper XLFs, but these are still consistent with the other observations. These results indicate that the XLFs of star-forming galaxies are indeed flatter than those of more evolved stellar populations, even down to the typical luminosities of X-ray binaries. Based on this, as well as the X-ray variability and spectral properties of the X-ray sources, we suggest that the observed population down to our detection limit consists predominantly of X-ray binaries accreting close to their Eddington limit, similar to the high or very high states of Galactic X-ray binaries. In the case of ultraluminous X-ray sources (L-X > 10(39) erg s(-1)), we cannot rule out the contribution of a beamed component (because of either mechanical focusing or Doppler boosting) in their observed emission. However, even without beaming, we estimate that the maximum observed luminosity (L-X similar to 10(40) erg s(-1)) could be produced by a similar to 80 M-circle dot black hole accreting at its Eddington limit; such black holes can be the result of regular stellar evolution of double stellar systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Observ, Pasadena, CA 91101 USA. Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Zezas, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Rots, Arnold/0000-0003-2377-2356 NR 48 TC 27 Z9 27 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 2007 VL 661 IS 1 BP 135 EP 148 DI 10.1086/513091 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EE UT WOS:000246574700014 ER PT J AU Liu, JF Bregman, J Miller, J Kaaret, P AF Liu, Ji-Feng Bregman, Joel Miller, Jon Kaaret, Philip TI Optical studies of the ultraluminous X-ray source NGC 1313 X-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual ( NGC 1313); X-rays : binaries ID MASS BLACK-HOLES; GLOBULAR-CLUSTERS; SOURCE POPULATION; SPIRAL GALAXIES; SYSTEMS; X-2; COUNTERPART; STARBURST; STELLAR; GROWTH AB NGC 1313 X-2 was among the first ultraluminous X-ray sources discovered, and has been a frequent target of X-ray and optical observations. Using the HSTACS multiband observations, this source is identified with a unique counterpart within an error circle of 0.2 ''. The counterpart is a blue star on the edge of a young cluster of <= 10(7) yr amid a dominant old stellar population. Its spectral energy distribution is consistent with that for a Z = 0.004 star with 8.5 M-circle dot about 5 x 10(6) yr old, or for an O7 V star at solar metallicity. The counterpart exhibited significant variability of Delta m = 0.153 +/- 0.033 mag between two F555W observations separated by 3 months, reminiscent of the ellipsoidal variability due to the orbital motion of this ULX binary. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Iowa, Iowa City, IA 52242 USA. RP Liu, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 48 TC 30 Z9 31 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 2007 VL 661 IS 1 BP 165 EP 172 DI 10.1086/516624 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EE UT WOS:000246574700016 ER PT J AU Kaplan, DL Levine, AM Chakrabarty, D Morgan, EH Erb, DK Gaensler, BM Moon, DS Cameron, PB AF Kaplan, David L. Levine, Alan M. Chakrabarty, Deepto Morgan, Edward H. Erb, Dawn K. Gaensler, Bryan M. Moon, Dae-Sik Cameron, P. Brian TI Lost and found: A new position and infrared counterpart for the X-ray binary scutum X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; pulsars : general; stars : individual (Sct X-1); X-rays : binaries ID PHOTOMETRIC STANDARD STARS; IGR J16318-4848; GALACTIC PLANE; GX 301-2; SPECTROSCOPY; PULSARS; EMISSION; OPHIUCHI; GALAXIES; SPECTRA AB Using archival X-ray data, we find that the catalog location of the X-ray binary Scutum X-1 (Sct X-1) is incorrect and that the correct location is that of the X-ray source AX J183528- 0737, which is 15' to the west. Our identification is made on the basis of the 112 s pulse period for this object detected in an XMM-Newton observation, as well as spatial coincidence between AX J183528-0737 and previous X-ray observations. Based on the XMM-Newton data and archival RXTE data, we confirm secular spin-down over 17 yr with period derivative P approximate to 3.9 x 10(-9) s s(-1), but do not detect a previously reported X-ray iron fluorescence line. We identify a bright (K-s = 6.55) red (J - K-s = 5.51) optical and infrared counterpart to AX J183528-0737 from 2MASS, a number of mid-IR surveys, and deep optical observations, which we use to constrain the extinction to and distance of Sct X-1. From these data, as well as limited near-IR spectroscopy, we conclude that Sct X-1 is most likely a binary system composed of a late-type giant or supergiant and a neutron star. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Kaplan, DL (reprint author), MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM dlk@space.mit.edu; aml@space.mit.edu; deepto@space.mit.edu; ehm@space.mit.edu; derb@cfa.harvard.edu; bgaensler@usyd.edu.au; moon@astro.utoronto.ca; pbc@astro.caltech.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 51 TC 15 Z9 16 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 2007 VL 661 IS 1 BP 437 EP 446 DI 10.1086/513712 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EE UT WOS:000246574700038 ER PT J AU Cooper, RL Narayan, R AF Cooper, Randall L. Narayan, Ramesh TI Hydrogen-triggered type I X-ray bursts in a two-zone model SO ASTROPHYSICAL JOURNAL LA English DT Article DE dense matter; nuclear reactions, nucleosynthesis, abundances; stars : neutron; X-rays : binaries; X-rays : bursts ID ACCRETING NEUTRON-STARS; FIELD CAMERAS OBSERVATIONS; SHELL FLASHES; BLACK-HOLES; DISCOVERY; RATES; TRANSIENTS; EVOLUTION; PHYSICS; FLOWS AB We use the two-zone model of Cooper & Narayan to study the onset and time evolution of hydrogen-triggered type I X-ray bursts on accreting neutron stars. At the lowest accretion rates, thermally unstable hydrogen burning ignites helium as well and produces a mixed hydrogen and helium burst. For somewhat higher accretion rates, thermally unstable hydrogen burning does not ignite helium and thus triggers only a weak hydrogen flash. For our choice of model parameters, these weak hydrogen flashes occur for 10(-3) less than or similar to M/M-Edd less than or similar to 3x10(-3). The peak luminosities of weak hydrogen flashes are typically much lower than the accretion luminosity. These results are in accord with previous theoretical work. We find that a series of weak hydrogen flashes generates a massive layer of helium that eventually ignites in an energetic pure helium flash. Although previously conjectured, this is the first time such bursting behavior has been actually demonstrated in a theoretical model. For yet higher accretion rates, hydrogen burning is thermally stable and thus steadily generates a layer of helium that ultimately ignites in a pure helium flash. We find that, for a narrow range of accretion rates between the mixed hydrogen and helium burst and weak hydrogen flash regimes, unstable hydrogen burning ignites helium only after a short series of weak hydrogen flashes has generated a sufficiently deep layer of helium. These bursts have fluences that are intermediate between those of normal mixed hydrogen and helium bursts and energetic pure helium flashes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cooper, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rcooper@cfa.harvard.edu; rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 62 TC 19 Z9 19 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 2007 VL 661 IS 1 BP 468 EP 476 DI 10.1086/513461 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EE UT WOS:000246574700041 ER PT J AU Ford, EB Chiang, EI AF Ford, Eric B. Chiang, Eugene I. TI The formation of ice giants in a packed oligarchy: Instability and aftermath SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; Kuiper Belt; planets and satellites : formation; solar system : formation ID PLANET FORMATION; SOLAR-SYSTEM; KUIPER-BELT; NEPTUNE; DISKS; PLANETESIMALS; ACCRETION; DYNAMICS; URANUS; MODEL AB As many as five ice giants - Neptune-mass planets composed of similar to 90% ice and rock and similar to 10% hydrogen - are thought to form at heliocentric distances of similar to 10 - 25 AU on closely packed orbits spaced similar to 5 Hill radii apart. Such oligarchies are ultimately unstable. Once the parent disk of planetesimals is sufficiently depleted, oligarchs perturb one another onto crossing orbits. We explore both the onset and outcome of the instability through numerical integrations, including dynamical friction cooling of planets by a planetesimal disk whose properties are held fixed. To trigger instability and the ejection of the first ice giant in systems having an original surface density in oligarchs of Sigma similar to 1 g cm similar to 2, the disk surface density similar to must fall below similar to 0.1 g cm similar to 2. Ejections are predominantly by Jupiter and occur within similar to 107 yr. To eject more than one oligarch requires similar to P0: 03 g cm similar to 2. For certain choices of sigma and initial semimajor axes of planets, systems starting with up to four oligarchs in addition to Jupiter and Saturn can readily yield solar system - like outcomes in which two surviving ice giants lie inside 30 AU and have their orbits circularized by dynamical friction. Our findings support the idea that planetary systems begin in more crowded and compact configurations, like those of shear-dominated oligarchies. In contrast to previous studies, we identify similar to P0: 1 similar to as the regime relevant for understanding the evolution of the outer solar system, and we encourage future studies to concentrate on this regime while relaxing our assumption of a fixed planetesimal disk. Whether evidence of the instability can be found in Kuiper Belt objects (KBOs) is unclear, since in none of our simulations do marauding oligarchs excite as large a proportion of KBOs having inclinations greater than or similar to 20 similar to as is observed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Ctr Integrat Planetary Sci, Berkeley, CA 94720 USA. RP Ford, EB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM eford@cfa.harvard.edu; echiang@astron.berkeley.edu OI /0000-0001-6545-639X NR 40 TC 51 Z9 51 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 20 PY 2007 VL 661 IS 1 BP 602 EP 615 DI 10.1086/513598 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EE UT WOS:000246574700056 ER PT J AU Ebeling, H Barrett, E Donovan, D Ma, CJ Edge, AC van Speybroeck, L AF Ebeling, H. Barrett, E. Donovan, D. Ma, C.-J. Edge, A. C. van Speybroeck, L. TI A complete sample of 12 very X-ray luminous galaxy clusters at z > 0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : general; X-rays : general ID CONSTRAINTS; SCALE; MACS AB We present the statistically complete and cosmologically most relevant subset of the 12 most distant galaxy clusters detected at z > 0.5 by the Massive Cluster Survey ( MACS). Ten of these systems are new discoveries; only two (MACS J0018+1626, aka Cl 0016+1609, and MACS J0454-0300, aka MS 0451.6-0305) were previously known. We provide fundamental cluster properties derived from our optical and X- ray follow-up observations as well as the selection function in tabulated form to facilitate cosmological studies using this sample. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Durham, Dept Phys, Durham DH1 3LE, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ebeling, H (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. NR 11 TC 159 Z9 159 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 2007 VL 661 IS 1 BP L33 EP L36 DI 10.1086/518603 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EH UT WOS:000246575000009 ER PT J AU Seu, R Phillips, RJ Biccari, D Orosei, R Masdea, A Picardi, G Safaeinili, A Campbell, BA Plaut, JJ Marinangeli, L Smrekar, SE Nunes, DC AF Seu, Roberto Phillips, Roger J. Biccari, Daniela Orosei, Roberto Masdea, Arturo Picardi, Giovanni Safaeinili, Ali Campbell, Bruce A. Plaut, Jeffrey J. Marinangeli, Lucia Smrekar, Suzanne E. Nunes, Daniel C. TI SHARAD sounding radar on the Mars Reconnaissance Orbiter SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID TERRA-MERIDIANI; GROUND ICE; ART.; SUBSURFACE; LOWLANDS; SURFACE; ORIGIN AB [1] SHARAD (SHAllow RADar) is a sounding radar provided by Agenzia Spaziale Italiana (ASI) as a Facility Instrument on the Mars Reconnaissance Orbiter mission. Its 20-MHz center frequency and 10-MHz bandwidth complement the lower-frequency, relatively narrower bandwidth capability of the MARSIS sounding radar. A joint Italian-U.S. team has guided the experiment development and is responsible for data analysis and interpretation. The radar transmits signals at a 700 Hz pulse repetition frequency (PRF) and collects reflections from both the surface and near subsurface of Mars. Vertical and horizontal resolutions are, respectively, 15 m ( free-space) and 3 - 6 km (cross-track) by 0.3 - 1 km ( along- track). The scientific objective of SHARAD is to map, in selected locales, dielectric interfaces to at least several hundred meters depth in the Martian subsurface and to interpret these results in terms of the occurrence and distribution of expected materials, including competent rock, soil, water, and ice. A signal-to-noise ratio of similar to 50 dB ( for a specular surface return) is achieved with 10 W of radiated power by using range and azimuth focusing in ground data processing. Preprocessed data as well as range- and azimuth-focused data will be formatted according to Planetary Data System (PDS) standards and be made available from the ASI Science Data Center (ASDC) and from the Geosciences Node of the Planetary Data System ( PDS). Important targets for SHARAD include the polar layered deposits, sedimentary stacks ( especially in Terra Meridiani), buried channel systems, buried impact craters, volcanic complexes, and shallow ice deposits in equilibrium with the atmosphere. C1 Univ Roma La Sapienza, INFOCOM, I-00184 Rome, Italy. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Univ G DAnnunzio, IRSPS, I-65127 Pescara, Italy. Lunar & Planetary Inst, Houston, TX 77058 USA. Ist Astrofis Spaziale & Fis Cosmica, Rome, Italy. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Seu, R (reprint author), Univ Roma La Sapienza, INFOCOM, Via Eudossiana 18, I-00184 Rome, Italy. EM phillips@wustite.wustl.edu NR 30 TC 85 Z9 86 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY 18 PY 2007 VL 112 IS E5 AR E05S05 DI 10.1029/2006JE002745 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 172YI UT WOS:000246840300001 ER PT J AU Gomendio, M Malo, AF Soler, AJ Garde, J Roldan, ERS AF Gomendio, Montserrat Malo, Aurelio F. Soler, Ana J. Garde, Julian Roldan, Eduardo R. S. TI Testosterone and male fertility in red deer - Response SO SCIENCE LA English DT Letter ID ANTLER GROWTH; STAGS C1 CSIC, Museo Nacl Ciencias Nat, Reprod Ecol & Biol Grp, Dept Evolut Ecol, E-28006 Madrid, Spain. Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. Univ Castilla La Mancha Junta Comunidades Castill, CSIC, Inst Invest Recursos Cinegeticos, Albacete 02071, Spain. RP Gomendio, M (reprint author), CSIC, Museo Nacl Ciencias Nat, Reprod Ecol & Biol Grp, Dept Evolut Ecol, E-28006 Madrid, Spain. RI Malo, Aurelio/D-3973-2011; Evolutionary Ecology, Ecologia Evolutiva/M-3553-2014 OI Malo, Aurelio/0000-0002-0846-2096; NR 5 TC 2 Z9 2 U1 0 U2 7 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAY 18 PY 2007 VL 316 IS 5827 BP 981 EP 981 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 168WF UT WOS:000246554000020 ER PT J AU McEwen, AS Eliason, EM Bergstrom, JW Bridges, NT Hansen, CJ Delamere, WA Grant, JA Gulick, VC Herkenhoff, KE Keszthelyi, L Kirk, RL Mellon, MT Squyres, SW Thomas, N Weitz, CM AF McEwen, Alfred S. Eliason, Eric M. Bergstrom, James W. Bridges, Nathan T. Hansen, Candice J. Delamere, W. Alan Grant, John A. Gulick, Virginia C. Herkenhoff, Kenneth E. Keszthelyi, Laszlo Kirk, Randolph L. Mellon, Michael T. Squyres, Steven W. Thomas, Nicolas Weitz, Catherine M. TI Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE) SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID POLAR LAYERED DEPOSITS; MARTIAN GEOLOGIC RECORD; ART. NO. 5111; GROUND ICE; VALLES-MARINERIS; LANDING SITE; NEAR-SURFACE; NORTHERN PLAINS; CLIMATE-CHANGE; SLOPE STREAKS AB [1] The HiRISE camera features a 0.5 m diameter primary mirror, 12 m effective focal length, and a focal plane system that can acquire images containing up to 28 Gb (gigabits) of data in as little as 6 seconds. HiRISE will provide detailed images (0.25 to 1.3 m/pixel) covering similar to 1% of the Martian surface during the 2-year Primary Science Phase (PSP) beginning November 2006. Most images will include color data covering 20% of the potential field of view. A top priority is to acquire similar to 1000 stereo pairs and apply precision geometric corrections to enable topographic measurements to better than 25 cm vertical precision. We expect to return more than 12 Tb of HiRISE data during the 2-year PSP, and use pixel binning, conversion from 14 to 8 bit values, and a lossless compression system to increase coverage. HiRISE images are acquired via 14 CCD detectors, each with 2 output channels, and with multiple choices for pixel binning and number of Time Delay and Integration lines. HiRISE will support Mars exploration by locating and characterizing past, present, and future landing sites, unsuccessful landing sites, and past and potentially future rover traverses. We will investigate cratering, volcanism, tectonism, hydrology, sedimentary processes, stratigraphy, aeolian processes, mass wasting, landscape evolution, seasonal processes, climate change, spectrophotometry, glacial and periglacial processes, polar geology, and regolith properties. An Internet Web site (HiWeb) will enable anyone in the world to suggest HiRISE targets on Mars and to easily locate, view, and download HiRISE data products. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Delamere Support Syst, Boulder, CO 80304 USA. Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Moffett Field, CA 94035 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. Planetary Sci Inst, Tucson, AZ 85719 USA. RP McEwen, AS (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM mcewen@pirl.lpl.arizona.edu RI Mellon, Michael/C-3456-2016; Bridges, Nathan/D-6341-2016 NR 243 TC 162 Z9 165 U1 6 U2 63 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY 17 PY 2007 VL 112 IS E5 AR E05S02 DI 10.1029/2005JE002605 PG 40 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 172YH UT WOS:000246840200001 ER PT J AU de Santana, CD Crampton, WGR AF de Santana, Carlos David Crampton, William G. R. TI Revision of the deep-channel electric fish genus Sternarchogiton (Gymnotiformes : Apteronotidae) SO COPEIA LA English DT Article ID AMAZON BASIN; TELEOSTEI AB The Neotropical ghost knifefish genus Sternarchogiton is revised on the basis of morphology and pigmentation. A new diagnosis for the genus is provided. Two new deep-channel taxa from the lowland portions of the Amazon basin are described: S. labiatus and S. preto. Sternarchogiton labiatus is diagnosed by the possession of a hard, prominent, three-lobed structure on the lower lips, two rows of teeth on the dentary, a second hypobranchial with a medial bridge, an ossified first basibranchial, and cartilaginous posterior basibranchials. Sternarchogiton preto is diagnosed by black or very dark brown body coloration, five long and conical teeth on the premaxilla, a dentary with one row of conical teeth pointing toward inside of mouth, the fusion of the supracleithrum and posttemporal, and anterior portion of coracoid not reaching anterior edge of cleithrum. A dichotomous key to species of the genus is provided. C1 Natl Museum Nat Hist, Div Fishes, Smithsonian Inst, Washington, DC 20013 USA. Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. RP de Santana, CD (reprint author), Natl Museum Nat Hist, Div Fishes, Smithsonian Inst, Washington, DC 20013 USA. EM apteronotidae@ig.com.br NR 27 TC 7 Z9 9 U1 1 U2 3 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 16 PY 2007 IS 2 BP 387 EP 402 DI 10.1643/0045-8511(2007)7[387:ROTDEF]2.0.CO;2 PG 16 WC Zoology SC Zoology GA 170BY UT WOS:000246637600013 ER PT J AU Wishnie, MH Dent, DH Mariscal, E Deago, J Cedeno, N Ibarra, D Condit, R Ashton, PMS AF Wishnie, M. H. Dent, D. H. Mariscal, E. Deago, J. Cedeno, N. Ibarra, D. Condit, R. Ashton, P. M. S. TI Initial performance and reforestation potential of 24 tropical tree species planted across a precipitation gradient in the Republic of Panama SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Central America; forestry; rainfall; restoration; silvopastoral systems; timber ID NATIVE FOREST REGENERATION; COSTA-RICA; ABANDONED PASTURE; RAIN-FOREST; PLANTATIONS; RESTORATION; LANDS; RECOVERY; ESTABLISHMENT; ECOSYSTEMS AB Decades of deforestation and unsustainable land use have created large expanses of degraded lands across Central America. Reforestation may offer one means of mitigating these processes of degradation while sustaining resident human communities. However, a lack of information regarding tree species performance has been identified as an important limitation on the success and adoption of diversified reforestation strategies. We analyzed the initial growth of 22 native and 2 exotic tree species planted at three sites across a precipitation gradient in the Republic of Panama (1100-2200 mm year(-1)), and identify promising species for use in forest restoration, timber production and on-farm systems. At all sites, Acacia mangium, Diphysa robinoides, Gliricidia sepium, Guazuma ulmifolia and Ochroma 1,pyramidale rapidly developed large, dense crowns and attained canopy closure after just 2 years. These species might be used in restoration efforts to rapidly stabilize soils and establish crown cover. As nitrogen-fixing legumes, D. robinoides and G. sepium may also have the potential to increase soil fertility. Several species valued for their timber performed well at all sites attaining high wood volume indices, these species included Tectona grandis, Pachira quinata and Tabebuia rosea. Albizia guachapele and Samanea saman were among the best performers at the driest site. The most promising species for use in silvopastoral systems varied among sites; A. guachapele, G. sepium, S. saman and G. ulmifolia performed best at the driest site, while G. sepium, G. ulmifolia and Spondias mombin were the top performers at the two wetter sites. It is hoped that the results of this trial will improve the success of reforestation efforts by allowing landholders to select species based upon both local site conditions and their specific reforestation objectives. (c) 2007 Elsevier B.V. All rights reserved. C1 Smithsonian Trop Res Inst, Unit 0948, Ctr Trop Forest Sci, PRORENA,Nat Species Reforestat Project, Miami, FL 34002 USA. Yale Univ, Sch Forestry & Environm Studies, PORENA, Nat Species Reforestat Project, New Haven, CT 06511 USA. RP Dent, DH (reprint author), Royal Bot Gardens, Richmond TW9 3AB, Surrey, England. EM d.dent@kew.org NR 58 TC 61 Z9 67 U1 3 U2 36 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2007 VL 243 IS 1 BP 39 EP 49 DI 10.1016/j.foreco.2007.02.001 PG 11 WC Forestry SC Forestry GA 165YK UT WOS:000246343500005 ER PT J AU Martin, RV Sauvage, B Folkins, I Sioris, CE Boone, C Bernath, P Ziemke, J AF Martin, Randall V. Sauvage, Bastien Folkins, Ian Sioris, Christopher E. Boone, Christopher Bernath, Peter Ziemke, Jerry TI Space-based constraints on the production of nitric oxide by lightning SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review ID TROPICAL TROPOSPHERIC OZONE; OPTICAL TRANSIENT DETECTOR; UNITED-STATES; SATELLITE-OBSERVATIONS; ATMOSPHERIC CHEMISTRY; MAPPING SPECTROMETER; NOX PRODUCTION; MONITORING INSTRUMENT; AIRCRAFT MEASUREMENTS; GLOBAL DISTRIBUTION AB We interpret observations of trace-gases from three satellite platforms to provide top-down constraints on the production of NO by lightning. The space-based observations are tropospheric NO2 columns from SCIAMACHY, tropospheric O-3 columns from OMI and MLS, and upper tropospheric HNO3 from ACE-FTS. A global chemical transport model ( GEOS-Chem) is used to identify locations and time periods in which lightning would be expected to dominate the trace gas observations. The satellite observations are sampled at those locations and time periods. All three observations exhibit a maximum in the tropical Atlantic region and a minimum in the tropical Pacific. This wave-1 pattern is driven by injection of lightning NO into the upper troposphere over the tropical continents, followed by photochemical production of NO2, HNO3, and O-3 during transport. Lightning produces a broad enhancement over the tropical Atlantic and Africa of 2-6 x 10(14) molecules NO2 cm(-2), 4 x 10(17) molecules O-3 cm(-2) ( 15 Dobson Units), and 125 pptv of upper tropospheric HNO3. The lightning background is 25-50% weaker over the tropical Pacific. A global source of 6 +/- 2 Tg N yr(-1) from lightning in the model best represents the satellite observations of tropospheric NO2, O-3, and HNO3. C1 Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Saskatchewan, Dept Phys & Engn, Saskatoon, SK B3H 3J5, Canada. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Martin, RV (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM randall.martin@dal.ca RI Martin, Randall/A-2051-2008; Bernath, Peter/B-6567-2012; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; OI Bernath, Peter/0000-0002-1255-396X; Martin, Randall/0000-0003-2632-8402; Sioris, Christopher/0000-0003-1168-8755 NR 104 TC 108 Z9 110 U1 1 U2 33 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 MAY 11 PY 2007 VL 112 IS D9 AR D09309 DI 10.1029/2006JD007831 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 168AR UT WOS:000246494900005 ER PT J AU Puccetti, S Fiore, F Risaliti, G Capalbi, M Elvis, M Nicastro, F AF Puccetti, S. Fiore, F. Risaliti, G. Capalbi, M. Elvis, M. Nicastro, F. TI Rapid N-H changes in NGC 4151 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : NGC 4151; galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY ASTRONOMY; LINE REGION SIZES; SEYFERT-GALAXIES; NGC 4151; COLUMN DENSITIES; ACCRETION DISK; CENTRAL MASSES; ON-BOARD; SPECTRUM AB We have analysed the two longest (elapsed time greater than or similar to 3 d) BeppoSAX observations of the X-ray brightest Seyfert galaxy, NGC 4151, to search for spectral variability on time-scales from a few tens of kiloseconds to years. We found in both cases highly significant spectral variability below approximate to 6 keV down to the shortest time-scales investigated. These variations can be naturally explained in terms of variations in the low energy cut-off due to obscuring matter along the line of sight. If the cut-off is modelled by two neutral absorption components, one fully covering the source and the second covering only a fraction of the source, the shortest time-scale of variability of a few days constrains the location of the obscuring matter to within 3.4 x 10(4) Schwarzschild radii from the central X-ray source. This is consistent with the distance of the broad emission-line region, as inferred from reverberation mapping, and difficult to reconcile with the parsec scale dusty molecular torus of Krolik & Begelman. We have also explored a more complex absorption structure, namely the presence of an ionized absorber. Although the behaviour of the ionization parameter is nicely consistent with the expectations, the results are not completely satisfactory from the statistical point of view. The overall absorption during the 2001 December observation is lower than in all other historical observations with similar 2-10 keV flux. This suggests that absorption variability plays a crucial role in the observed flux variability of this source. C1 ASI Sci Data Ctr, I-00044 Frascati, Italy. INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Puccetti, S (reprint author), ASI Sci Data Ctr, Via Galileo Galileo, I-00044 Frascati, Italy. EM puccetti@asdc.asi.it OI Risaliti, Guido/0000-0002-3556-977X; Puccetti, Simonetta/0000-0002-2734-7835; Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 58 TC 69 Z9 69 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2007 VL 377 IS 2 BP 607 EP 616 DI 10.1111/j.1365-2966.2007.11634.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 161RE UT WOS:000246032400013 ER PT J AU Mori, K Ho, WCG AF Mori, Kaya Ho, Wynn C. G. TI Modelling mid-Z element atmospheres for strongly magnetized neutron stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atomic processes; magnetic fields; stars : atmospheres; stars : neutron ID X-RAY-SPECTRUM; ANISOTROPIC THERMAL EMISSION; BROAD ABSORPTION FEATURE; COHERENT TIMING SOLUTION; EQUATION-OF-STATE; XMM-NEWTON; TEMPERATURE DISTRIBUTION; HYDROGEN ATMOSPHERES; RX J185635-3754; RADIATION AB We construct models for strongly magnetized neutron star atmospheres composed of mid-Z elements (carbon, oxygen and neon) with magnetic fields B = 10(12)-10(13) G and effective temperatures T-eff = (1 - 5) x 10(6) K; this is done by first addressing the physics relevant to strongly magnetized plasmas and calculating the equation of state and polarization-dependent opacities. We then obtain the atmosphere structure and spectrum by solving the radiative transfer equations in hydrostatic and radiative equilibrium. In contrast to hydrogen opacities at the relevant temperatures, mid-Z element opacities are dominated by numerous bound-bound and bound-free transitions. Consequently, temperature profiles are closer to grey profiles, and photosphere densities are lower than in the hydrogen case. Mid-Z element atmosphere spectra are significantly softer than hydrogen atmosphere spectra and show numerous absorption lines and edges. The atmosphere spectra depend strongly on surface composition and magnetic field but weakly on surface gravity. Absorption lines are primarily broadened by motional Stark effects and the (unknown) surface magnetic field distribution. When magnetic field variation is not severe, substructure in broad absorption features can be resolved by (phase-resolved) CCD spectroscopy from Chandra and XMM-Newton. Given the multiple absorption features seen in several isolated neutron stars (INSs), it is possible to determine the surface composition, magnetic field, temperature and gravitational redshift with existing X-ray data; we present qualitative comparisons between our model spectra and the neutron stars 1E1207.4-5209 and RX J1605.3+3249. Future high-resolution X-ray missions such as Constellation-X will measure the gravitational redshift with high accuracy by resolving narrow absorption features; when combined with radius measurements, it will be possible to uniquely determine the mass and radius of INSs. C1 Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Mori, K (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM kaya@cita.utoronto.ca; wynnho@slac.stanford.edu NR 90 TC 47 Z9 47 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 MAY 11 PY 2007 VL 377 IS 2 BP 905 EP 919 DI 10.1111/j.1365-2966.2007.11663.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 161RE UT WOS:000246032400038 ER PT J AU Tamisiea, ME Mitrovica, JX Davis, JL AF Tamisiea, M. E. Mitrovica, J. X. Davis, J. L. TI GRACE gravity data constrain ancient ice geometries and continental dynamics over Laurentia SO SCIENCE LA English DT Article ID PLEISTOCENE DEGLACIATION; MANTLE VISCOSITY; FIELD; EARTH; MODEL; LEVEL; SEA AB The free-air gravity trend over Canada, derived from the Gravity Recovery and Climate Experiment ( GRACE) satellite mission, robustly isolates the gravity signal associated with glacial isostatic adjustment (GIA) from the longer-time scale mantle convection process. This trend proves that the ancient Laurentian ice complex was composed of two large domes to the west and east of Hudson Bay, in accord with one of two classes of earlier reconstructions. Moreover, GIA models that reconcile the peak rates contribute similar to 25 to similar to 45% to the observed static gravity field, which represents an important boundary condition on the buoyancy of the continental tectosphere. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02143 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Tamisiea, ME (reprint author), Proudman Oceanog Lab, 6 Brownlow St, Liverpool L3 5DA, Merseyside, England. EM mtamisiea@cfa.harvard.edu RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 24 TC 97 Z9 100 U1 3 U2 15 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 MAY 11 PY 2007 VL 316 IS 5826 BP 881 EP 883 DI 10.1126/science.1137157 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 166HM UT WOS:000246369800035 PM 17495169 ER PT J AU Furlanetto, SR Lidz, A AF Furlanetto, Steven R. Lidz, Adam TI The cross-correlation of high-redshift 21 cm and galaxy surveys SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : high-redshift; intergalactic medium ID LYMAN-BREAK GALAXIES; DARK-MATTER HALOES; LY-ALPHA EMITTERS; SUBARU DEEP FIELD; CENTIMETER FLUCTUATIONS; INTERGALACTIC MEDIUM; EARLIEST GALAXIES; NEUTRAL HYDROGEN; REIONIZATION; EPOCH AB We study the detectability of the cross- correlation between 21 cm emission from the intergalactic medium and the galaxy distribution during (and before) reionization. We show that first-generation 21 cm experiments, such as the Mileura Widefield Array (MWA), can measure the cross-correlation to a precision of several percent on scales k similar to 0.1 Mpc(-1) if combined with a deep galaxy survey detecting all galaxies with m > 1010 M-circle dot over the entire similar to 800 deg(2) field of view of the MWA. LOFAR can attain even better limits with galaxy surveys covering its similar to 50 deg(2) field of view. The errors on the cross power spectrum scale with the square root of the overlap volume, so even reasonably modest surveys of several square degrees should yield a positive detection with either instrument. In addition to the obvious scientific value, the cross-correlation has four key advantages over the 21 cm signal alone: (1) its signal-to-noise ratio exceeds that of the 21 cm power spectrum by a factor of several, allowing it to probe smaller spatial scales and perhaps to detect inhomogeneous reionization more efficiently; (2) it allows a cleaner division of the redshift-space distortions (although only if the galaxy redshifts are known precisely); (3) by correlating with the high-redshift galaxy population, the cosmological nature of the 21 cm fluctuations can be determined unambiguously; and (4) the required level of foreground cleaning for the 21 cm signal is vastly reduced. C1 Yale Univ, Ctr Astron & Astrophys, New Haven, CT 06520 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), Yale Univ, Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. EM steven.furlanetto@yale.edu NR 57 TC 19 Z9 19 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 10 PY 2007 VL 660 IS 2 BP 1030 EP 1038 DI 10.1086/513009 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169CW UT WOS:000246571300011 ER PT J AU Gitti, M McNamara, BR Nulsen, PEJ Wise, MW AF Gitti, M. McNamara, B. R. Nulsen, P. E. J. Wise, M. W. TI Cosmological effects of powerful AGN outbursts in galaxy clusters: Insights from an XMM-Newton observation of MS 0735+7421 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; cosmology : miscellaneous; galaxies : clusters : general; galaxies : clusters : individual (MS 0735.7+7421); intergalactic medium; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; MASS-TEMPERATURE RELATION; HYDRA-A CLUSTER; COOLING FLOWS; INTRACLUSTER MEDIUM; THERMAL CONDUCTION; T RELATION; METALLICITY GRADIENTS; CHANDRA OBSERVATION; RADIO OBSERVATIONS AB We report on the results of an analysis of XMM-Newton observations of MS 0735+7421, the galaxy cluster that hosts the most energetic AGN outburst currently known. The previous Chandra image shows twin giant X-ray cavities (similar to 200 kpc diameter) filled with radio emission and surrounded by a weak shock front. XMM data are consistent with these findings. The total energy in cavities and shock (similar to 6; 10(61) ergs) is enough to quench the cooling flow and, since most of the energy is deposited outside the cooling region (similar to 100 kpc), to heat the gas within 1 Mpc by similar to 1/4 keV per particle. The cluster exhibits an upward departure (factor similar to 2) from the mean L-T relation. The boost in emissivity produced by the ICM compression in the bright shells due to the cavity expansion may contribute to explain the high luminosity and high central gas mass fraction that we measure. The scaled temperature and metallicity profiles are in general agreement with those observed in relaxed clusters. Also, the quantities we measure are consistent with the observed M-T relation. We conclude that violent outbursts such as the one in MS 0735+7421 do not cause dramatic instantaneous departures from cluster scaling relations (other than the L-T relation). However, if they are relatively common they may play a role in creating the global cluster properties. C1 Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Inst Astron, NL-1098 SJ Amsterdam, Netherlands. RP Gitti, M (reprint author), Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. OI Gitti, Myriam/0000-0002-0843-3009 NR 86 TC 36 Z9 36 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 10 PY 2007 VL 660 IS 2 BP 1118 EP 1136 DI 10.1086/512800 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169CW UT WOS:000246571300018 ER PT J AU Xiang, JG Lee, JC Nowak, MA AF Xiang, Jingen Lee, Julia C. Nowak, Michael A. TI Using the X-ray dust scattering halo of 4U 1624-490 to determine distance and dust distributions SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; scattering; X-rays : ISM ID INTERSTELLAR GRAINS; POINT SOURCES; BIG-DIPPER; ABSORPTION; X-1624-490; X1624-490; BINARIES; MODEL AB We present X-ray dust scattering halo results based on our 76 ks Chandra ACIS-S/HETGS observation of the LMXB dipping source 4U 1624 - 490. Through analysis of the halo light curves with 2 - 6 keV spectra over the persistent and dipping periods, we estimate a geometric distance of - 15 kpc to 4U 1624 - 490. We also fit halo radial profiles with different ISM dust grain models to assess the location, uniformity, and density of the halo. Our analysis shows that the dust spatial distribution is not uniform along the line of sight; rather, it is consistent with the spiral arm structure mapped in H II. The large difference between the absorption hydrogen column ( Nabs H - 8; 1022 cm - 2; probes all gas along the line of sight) derived from broadband spectral fitting and the scattering hydrogen column ( Nsca H - 4; 1022 cm - 2; probes only Galactic gas) derived from our studies of the 4U 1624 - 490 X-ray halo suggests that a large fraction of the column is local to the X-ray binary. We also present ( and apply) a new method for assessing the Chandra point-spread function at large (> 50") angles, through use of the time delays from the observed dips. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Chandra Xray Sci Ctr, Cambridge, MA 02139 USA. Kavli Inst Space Res, Cambridge, MA 02139 USA. RP Xiang, JG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jxiang@cfa.harvard.edu; jclee@cfa.harvard.edu; mnowak@space.mit.edu RI Lee, Julia/G-2381-2015 OI Lee, Julia/0000-0002-7336-3588 NR 32 TC 18 Z9 18 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 10 PY 2007 VL 660 IS 2 BP 1309 EP 1318 DI 10.1086/513308 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169CW UT WOS:000246571300035 ER PT J AU Heinke, CO Jonker, PG Wijnands, R Taam, RE AF Heinke, C. O. Jonker, P. G. Wijnands, R. Taam, R. E. TI Constraints on thermal X-ray radiation from SAX J1808.4-3658 and implications for neutron star neutrino emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE dense matter; neutrinos; stars : neutron; X-rays : binaries ID ACCRETING MILLISECOND PULSAR; GLOBULAR-CLUSTER TERZAN-5; ACTIVE RADIO PULSAR; SAX J1808.4-3658; QUIESCENT SPECTRUM; AQUILA X-1; XMM-NEWTON; TRANSIENT; MODEL; LUMINOSITIES AB Thermal X-ray radiation from neutron star soft X-ray transients in quiescence provides the strongest constraints on the cooling rates of neutron stars and thus on the interior composition and properties of matter in the cores of neutron stars. We analyze new ( 2006) and archival ( 2001) XMM-Newton observations of the accreting millisecond pulsar SAX J1808.4-3658 in quiescence, which provide the most stringent constraints to date. The X-ray spectrum of SAX J1808.4-3658 in the 2006 observation is consistent with a power law of photon index 1: 83 - 0: 17, without requiring the presence of a blackbody-like component from a neutron star atmosphere. Our 2006 observation shows a slightly lower 0.5-10 keV X-ray luminosity, at a level of 68(-13)(+15)% of that inferred from the 2001 observation. Simultaneous fitting of all available XMM-Newton data allows a constraint on the quiescent neutron star ( 0.01-10 keV) luminosity of L-NS < 1.1 x 10(31) ergs s(-1). This limit excludes some current models of neutrino emission mediated by pion condensates and provides further evidence of additional cooling processes, such as neutrino emission via direct Urca processes involving nucleons and/or hyperons, in the cores of massive neutron stars. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Heinke, CO (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. EM cheinke@northwestern.edu OI Heinke, Craig/0000-0003-3944-6109 NR 46 TC 60 Z9 60 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2007 VL 660 IS 2 BP 1424 EP 1427 DI 10.1086/513140 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169CW UT WOS:000246571300047 ER PT J AU Schmelz, JT Kashyap, VL Weber, MA AF Schmelz, J. T. Kashyap, V. L. Weber, M. A. TI Coronal heat: Solar loop temperatures from TRACE triple-filter data SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : fundamental parameters; Sun : UV radiation ID TRANSITION-REGION; DENSITY STRUCTURE; SPECTRA; PLASMA; EIT; TELESCOPE; EXPLORER; MODEL AB The Transition Region and Coronal Explorer ( TRACE) has state-of-the-art spatial resolution and shows the most detailed images of coronal loops ever observed. The temperatures of these loops are primarily derived from the 171 to 195 angstrom filter ratio, with data from the third filter at 284 angstrom used by several authors to improve the precision of the derived temperatures. Most of these studies assume that the plasma is isothermal and model the loops primarily as uniform temperature structures with footpoint-dominated heating. However, these triple-filter data are insufficient to constrain the plasma temperature and cannot be used to determine the isothermality or otherwise of coronal loop structures. We show this explicitly by constructing differential emission measures with these same triple-filter data using a sophisticated Markov-chain Monte Carlo - based reconstruction algorithm. We find that these TRACE data cannot, in general, limit the temperature distribution for coronal loop plasma. In other words, many different temperature distributions ( isothermal, broad, sloped, etc.) can reproduce the observed fluxes, and the TRACE coronal data alone cannot determine which of these distributions represents the actual coronal plasma. C1 Univ Memphis, Dept Phys, Memphis, TN 38152 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu; kashyap@head.cfa.harvard.edu; mweber@head.cfa.harvard.edu NR 25 TC 16 Z9 16 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 10 PY 2007 VL 660 IS 2 BP L157 EP L160 DI 10.1086/518363 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169EB UT WOS:000246574400020 ER PT J AU Knutson, HA Charbonneau, D Allen, LE Fortney, JJ Agol, E Cowan, NB Showman, AP Cooper, CS Megeath, ST AF Knutson, Heather A. Charbonneau, David Allen, Lori E. Fortney, Jonathan J. Agol, Eric Cowan, Nicolas B. Showman, Adam P. Cooper, Curtis S. Megeath, S. Thomas TI A map of the day-night contrast of the extrasolar planet HD 189733b SO NATURE LA English DT Article ID SPITZER-SPACE-TELESCOPE; HOT JUPITERS; LIGHT CURVES; THERMAL EMISSION; GIANT PLANETS; ATMOSPHERES; 209458B; HD-189733; DYNAMICS; SPECTRA AB 'Hot Jupiter' extrasolar planets are expected to be tidally locked because they are close (< 0.05 astronomical units, where 1 AU is the average Sun - Earth distance) to their parent stars, resulting in permanent daysides and nightsides. By observing systems where the planet and star periodically eclipse each other, several groups have been able to estimate the temperatures of the daysides of these planets(1-3). A key question is whether the atmosphere is able to transport the energy incident upon the dayside to the nightside, which will determine the temperature at different points on the planet's surface. Here we report observations of HD 189733, the closest of these eclipsing planetary systems(4-6), over half an orbital period, from which we can construct a 'map' of the distribution of temperatures. We detected the increase in brightness as the dayside of the planet rotated into view. We estimate a minimum brightness temperature of 973 +/- 33 K and a maximum brightness temperature of 1,212 +/- 11K at a wavelength of 8 mm, indicating that energy from the irradiated dayside is efficiently redistributed throughout the atmosphere, in contrast to a recent claim for another hot Jupiter 7. Our data indicate that the peak hemisphereintegrated brightness occurs 16 +/- 6 degrees before opposition, corresponding to a hotspot shifted east of the substellar point. The secondary eclipse ( when the planet moves behind the star) occurs 120 +/- 24 s later than predicted, which may indicate a slightly eccentric orbit. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. RP Knutson, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hknutson@cfa.harvard.edu RI Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Charbonneau, David/0000-0002-9003-484X NR 30 TC 406 Z9 411 U1 4 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 MAY 10 PY 2007 VL 447 IS 7141 BP 183 EP 186 DI 10.1038/nature05782 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 165WT UT WOS:000246338700037 PM 17495920 ER PT J AU Kim, TW Christy, JH Choe, JC AF Kim, Tae Won Christy, John H. Choe, Jae C. TI A Preference for a Sexual Signal Keeps Females Safe SO PLOS ONE LA English DT Article ID MALE FIDDLER-CRABS; SENSORY TRAP HYPOTHESIS; PREDATION RISK; MATE CHOICE; MATING-BEHAVIOR; SELECTION; BENEFITS; ATTRACTIVENESS; COURTSHIP; COSTS AB Predation is generally thought to constrain sexual selection by female choice and limit the evolution of conspicuous sexual signals. Under high predation risk, females usually become less choosy, because they reduce their exposure to their predators by reducing the extent of their mate searching. However, predation need not weaken sexual selection if, under high predation risk, females exhibit stronger preferences for males that use conspicuous signals that help females avoid their predators. We tested this prediction in the fiddler crab Uca terpsichores by increasing females' perceived predation risk from crab-eating birds and measuring the attractiveness of a courtship signal that females use to find mates. The sexual signal is an arching mound of sand that males build at the openings of their burrows to which they attract females for mating. We found that the greater the risk, the more attractive were males with those structures. The benefits of mate preferences for sexual signals are usually thought to be linked to males' reproductive contributions to females or their young. Our study provides the first evidence that a female preference for a sexual signal can yield direct survival benefits by keeping females safe as they search for mates. C1 [Choe, Jae C.] Ewha Womans Univ, Grad Program EcoSci, Seoul, South Korea. [Kim, Tae Won] Seoul Natl Univ, Sch Biol Sci, Seoul, South Korea. [Christy, John H.] Smithsonian Trop Res Inst, Naos Lab, Balboa, Ancon, Panama. RP Choe, JC (reprint author), Ewha Womans Univ, Grad Program EcoSci, Seoul, South Korea. EM jaechoe@ewha.ac.kr FU Korean Government (MOEHRD) [KRF-2005-213-D00043]; Ewha Womans University FX This research was supported by a Korean Research Foundation Grant funded by the Korean Government (MOEHRD) (KRF-2005-213-D00043). Jae C. Choe was funded by the Ewha Womans University Research Grant of 2006. The Smithsonian Tropical Research Institute provided space and logistical support. NR 24 TC 26 Z9 26 U1 0 U2 13 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 9 PY 2007 VL 2 IS 5 AR e422 DI 10.1371/journal.pone.0000422 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA V10DX UT WOS:000207445800004 PM 17487270 ER PT J AU Squyres, SW Aharonson, O Clark, BC Cohen, BA Crumpler, L de Souza, PA Farrand, WH Gellert, R Grant, J Grotzinger, JP Haldemann, AFC Johnson, JR Klingelhofer, G Lewis, KW Li, R McCoy, T McEwen, AS McSween, HY Ming, DW Moore, JM Morris, RV Parker, TJ Rice, JW Ruff, S Schmidt, M Schroder, C Soderblom, LA Yen, A AF Squyres, S. W. Aharonson, O. Clark, B. C. Cohen, B. A. Crumpler, L. de Souza, P. A. Farrand, W. H. Gellert, R. Grant, J. Grotzinger, J. P. Haldemann, A. F. C. Johnson, J. R. Klingelhoefer, G. Lewis, K. W. Li, R. McCoy, T. McEwen, A. S. McSween, H. Y. Ming, D. W. Moore, J. M. Morris, R. V. Parker, T. J. Rice, J. W., Jr. Ruff, S. Schmidt, M. Schroeder, C. Soderblom, L. A. Yen, A. TI Pyroclastic activity at home plate in Gusev Crater, Mars SO SCIENCE LA English DT Article ID SPIRIT AB Home Plate is a layered plateau in Gusev crater on Mars. It is composed of clastic rocks of moderately altered alkali basalt composition, enriched in some highly volatile elements. A coarse-grained lower unit lies under a finer-grained upper unit. Textural observations indicate that the lower strata were emplaced in an explosive event, and geochemical considerations favor an explosive volcanic origin over an impact origin. The lower unit likely represents accumulation of pyroclastic materials, whereas the upper unit may represent eolian reworking of the same pyroclastic materials. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Lockheed Martin Corp, Littleton, CO 80127 USA. Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. Vallourec Res Ctr, F-59260 Aulnoye Aymeries, France. Space Sci Inst, Boulder, CO 80301 USA. Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-6500 Mainz, Germany. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. RP Squyres, SW (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Lewis, Kevin/E-5557-2012; Johnson, Jeffrey/F-3972-2015 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; NR 17 TC 101 Z9 102 U1 0 U2 21 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 4 PY 2007 VL 316 IS 5825 BP 738 EP 742 DI 10.1126/science.1139045 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 163RR UT WOS:000246181400044 PM 17478719 ER PT J AU Engelbrecht, BMJ Comita, LS Condit, R Kursar, TA Tyree, MT Turner, BL Hubbell, SP AF Engelbrecht, Bettina M. J. Comita, Liza S. Condit, Richard Kursar, Thomas A. Tyree, Melvin T. Turner, Benjamin L. Hubbell, Stephen P. TI Drought sensitivity shapes species distribution patterns in tropical forests SO NATURE LA English DT Article ID RAIN-FOREST; FLORISTIC COMPOSITION; HABITAT ASSOCIATIONS; NEOTROPICAL FOREST; CLIMATIC GRADIENT; MOIST FOREST; DIVERSITY; SEEDLINGS; TREES; TOLERANCE AB Although patterns of tree species distributions along environmental gradients have been amply documented in tropical forests(1-7), mechanisms causing these patterns are seldom known. Efforts to evaluate proposed mechanisms have been hampered by a lack of comparative data on species' reactions to relevant axes of environmental variation(1). Here we show that differential drought sensitivity shapes plant distributions in tropical forests at both regional and local scales. Our analyses are based on experimental field assessments of drought sensitivity of 48 species of trees and shrubs, and on their local and regional distributions within a network of 122 inventory sites spanning a rainfall gradient across the Isthmus of Panama. Our results suggest that niche differentiation with respect to soil water availability is a direct determinant of both local- and regional-scale distributions of tropical trees. Changes in soil moisture availability caused by global climate change and forest fragmentation are therefore likely to alter tropical species distributions, community composition and diversity. C1 Smithsonian Trop Res Inst, Balboa 03092, Panama. Univ Kaiserslautern, Dept Plant Ecol & Systemat, D-67663 Kaiserslautern, Germany. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. US Forest Serv, USDA, Burlington, VT 05402 USA. Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2E3, Canada. RP Engelbrecht, BMJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843, Balboa 03092, Panama. EM engelbrb@si.edu RI Turner, Benjamin/E-5940-2011; Engelbrecht, Bettina/E-9914-2012; OI Turner, Benjamin/0000-0002-6585-0722; Comita, Liza/0000-0002-9169-1331 NR 30 TC 379 Z9 400 U1 39 U2 303 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 3 PY 2007 VL 447 IS 7140 BP 80 EP U2 DI 10.1038/nature05747 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 163GY UT WOS:000246149300047 PM 17476266 ER PT J AU Wright, IJ Ackerly, DD Bongers, F Harms, KE Ibarra-Manriquez, G Martinez-Ramos, M Mazer, SJ Muller-Landau, HC Paz, H Pitman, NCA Poorter, L Silman, MR Vriesendorp, CF Webb, CO Westoby, M Wright, SJ AF Wright, Ian J. Ackerly, David D. Bongers, Frans Harms, Kyle E. Ibarra-Manriquez, Guillermo Martinez-Ramos, Miguel Mazer, Susan J. Muller-Landau, Helene C. Paz, Horacio Pitman, Nigel C. A. Poorter, Lourens Silman, Miles R. Vriesendorp, Corine F. Webb, Cam O. Westoby, Mark Wright, S. Joseph TI Relationships among ecologically important dimensions of plant trait variation in seven Neotropical forests SO ANNALS OF BOTANY LA English DT Article; Proceedings Paper CT 90th Annual Meeting of the Ecological-Society-of-America/9th International Congress of Ecology CY AUG, 2005 CL Montreal, CANADA SP Ecol Soc Amer DE fruit size; leaf size; phylogenetically independent contrasts; plant height; plant strategies; seed size; specific leaf area; tropical rainforest ecology; wood density ID LOWLAND RAIN-FOREST; LEAF LIFE-SPAN; SEED SIZE; WOOD DENSITY; FUNCTIONAL CONVERGENCE; LIGHT INTERCEPTION; WATER TRANSPORT; TREE HEIGHT; LOS-TUXTLAS; CANOPY AB Background and Aims When ecologically important plant traits are correlated they may be said to constitute an ecological 'strategy' dimension. Through identifying these dimensions and understanding their inter-relationships we gain insight into why particular trait combinations are favoured over others and into the implications of trait differences among species. Here we investigated relationships among several traits, and thus the strategy dimensions they represented, across 2134 woody species from seven Neotropical forests. Methods Six traits were studied: specific leaf area (SLA), the average size of leaves, seed and fruit, typical maximum plant height, and wood density (WD). Trait relationships were quantified across species at each individual forest as well as across the dataset as a whole. 'Phylogenetic' analyses were used to test for correlations among evolutionary trait-divergences and to ascertain whether interspecific relationships were biased by strong taxonomic patterning in the traits. Results The interspecific and phylogenetic analyses yielded congruent results. Seed and fruit size were expected, and confirmed, to be tightly related. As expected, plant height was correlated with each of seed and fruit size, albeit weakly. Weak support was found for an expected positive relationship between leaf and fruit size. The prediction that SLA and WD would be negatively correlated was not supported. Otherwise the traits were predicted to be largely unrelated, being representatives of putatively independent strategy dimensions. This was indeed the case, although WD was consistently, negatively related to leaf size. Conclusions The dimensions represented by SLA, seed/fruit size and leaf size were essentially independent and thus conveyed largely independent information about plant strategies. To a lesser extent the same was true for plant height and WD. Our tentative explanation for negative WD-leaf size relationships, now also known from other habitats, is that the traits are indirectly linked via plant hydraulics. C1 Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Univ Wageningen & Res Ctr, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands. Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58190, Michoacan, Mexico. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. Duke Univ, Dept Bot, Durham, NC 27708 USA. Inst Boliviano Invest Forestal, Santa Cruz, Bolivia. Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. Field Museum Nat Hist, Chicago, IL 60605 USA. Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wright, IJ (reprint author), Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. EM iwright@rna.bio.mq.edu.au RI Pitman, Nigel/A-7681-2008; Wright, Ian/G-4979-2012; Ackerly, David/A-1247-2009; Wright, Stuart/M-3311-2013 OI Pitman, Nigel/0000-0002-9211-2880; Wright, Ian/0000-0001-8338-9143; Ackerly, David/0000-0002-1847-7398; Wright, Stuart/0000-0003-4260-5676 NR 80 TC 158 Z9 180 U1 13 U2 97 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD MAY PY 2007 VL 99 IS 5 BP 1003 EP 1015 DI 10.1093/aob/mcl066 PG 13 WC Plant Sciences SC Plant Sciences GA 162WM UT WOS:000246120200021 PM 16595553 ER PT J AU Hartsough, CDB Connor, EF Smith, DR Spicer, GS AF Hartsough, Chester D. B. Connor, Edward F. Smith, David R. Spicer, Greg S. TI Systematics of two feeding morphs of Schizocerella pilicornis (Hymenoptera : Argidae) and recognition of two species SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE phylogenetics; speciation; Schizocerella pilicornis; mitochondrial DNA; phytophagy ID RIBOSOMAL-RNA GENE; PHYLOGENETIC UTILITY; MITOCHONDRIAL-DNA; NORTH-AMERICA; EVOLUTION; SEQUENCE; COMPLEX; DIFFERENTIATION; DROSOPHILA; TAXONOMY AB A number of species of Argidae were proposed in the late 1800s and early 1900s, all of which later were regarded as a single color-variable species, Schizocerella pilicornis (Holmgren). In the mid-1970s, an external-feeding type was reported in the literature, and it also was identified as S. pilicornis, although previously S. pilicornis was only known to feed by leaf mining. Thus, the uniqueness of a species with two distinct feeding types led us to question the taxonomy of S. pilicornis. We use data from the mitochondrial cytochrome oxidase I gene (COI) to show that the two feeding types have a sequence divergence of 5.8%, which exceeds the difference between many insect taxa currently classified as different species. Considering the existing evidence on morphological, behavioral, allozymic, and ecological differences, we here recognize these two feeding types as distinct species: Schizocerella pilicornis (Holmgren) as the leaf-mining species and Schizocerella lineata (Rohwer) as the external-feeding species. We provide a diagnosis for each species, and show that adults of S. pilicornis have a mostly black mesonotum, whereas adults of S. lineata have an orange-red mesonotum. C1 San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. USDA, Systemat Entomol Lab, PSI Agr Res Serv, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Hartsough, CDB (reprint author), San Francisco State Univ, Dept Biol, 1600 Holloway Ave, San Francisco, CA 94132 USA. EM cdh@sfsu.edu NR 48 TC 4 Z9 5 U1 0 U2 1 PU ENTOMOLOGICAL SOCIETY AMERICA PI LANHAM PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAY PY 2007 VL 100 IS 3 BP 375 EP 380 DI 10.1603/0013-8746(2007)100[375:SOTFMO]2.0.CO;2 PG 6 WC Entomology SC Entomology GA 165SD UT WOS:000246324900005 ER PT J AU Saltonstall, K Stevenson, JC AF Saltonstall, Kristin Stevenson, J. Court TI The effect of nutrients on seedling growth of native and introduced Phragmites australis SO AQUATIC BOTANY LA English DT Article DE common reed; competition; invasive species; North America; nutrient enrichment ID COMMON REED; SALT MARSHES; CRYPTIC INVASION; TIDAL WETLANDS; NORTH-AMERICA; EXPANSION; SALINITY; SPARTINA; ESTABLISHMENT; DETERMINANTS AB Differing responses to abiotic stresses and increased nutrient availability may play a role in the invasion and spread of introduced Phragmites australis Cav. (Trin.) ex. Steud. and the decline of native P.a. americanus Saltonstall, P.M. Peterson & Soreng in North America. We present results from an outdoor experiment where native and introduced P. australis seedlings were grown under two nutrient treatments. Both subspecies responded positively to increased nutrients but introduced plants clearly outperformed natives, growing taller, producing more stems, and had three to four times higher biomass. The biomass of introduced R australis growing in low nutrients was similar to that of the native in high nutrients. Aboveground:belowground biomass ratios were nearly 1.25 for both native and introduced plants across treatments and reflect the high investment P. australis seedlings place on shoot production in their first year of growth. Our results also demonstrate that introduced P. australis can have explosive growth over a single growing season, even when established from seed. This implies that management of young, newly established populations may be prudent where introduced P. australis is considered undesirable, irregardless of whether eutrophication is an issue. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Maryland, Horn Point Environm Lab, Ctr Environm Sci, Cambridge, MD 21613 USA. RP Saltonstall, K (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. EM kristin.saltonstall@aya.yale.edu NR 33 TC 42 Z9 46 U1 7 U2 53 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3770 J9 AQUAT BOT JI Aquat. Bot. PD MAY PY 2007 VL 86 IS 4 BP 331 EP 336 DI 10.1016/j.aquabot.2006.12.003 PG 6 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 156JU UT WOS:000245644800005 ER PT J AU Blackman, MJ Bishop, RL AF Blackman, M. J. Bishop, R. L. TI The Smithsonian-NIST partnership: The application of instrumental neutron activation analysis to archaeology SO ARCHAEOMETRY LA English DT Article DE neutron activation analysis; Maya pottery; standards; Smithsonian Institution; NIST ID CERAMICS AB The history and procedures of the Smithsonian-NIST programme in the application of instrumental neutron activation to the study of archaeological materials are reviewed. Statistical processing of the resulting analytical data is a major focus of the programme, with attention called to processes of initial group formation. Specific areas of current research emphasis are presented, which build upon the strength of accumulated databases. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, NMNH,MRC112, Washington, DC 20013 USA. RP Blackman, MJ (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, NMNH,MRC112, POB 37012, Washington, DC 20013 USA. NR 51 TC 14 Z9 14 U1 0 U2 6 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD MAY PY 2007 VL 49 BP 321 EP 341 DI 10.1111/j.1475-4754.2007.00304.x PN 2 PG 21 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA 174BC UT WOS:000246915200011 ER PT J AU Glascock, MD Speakman, RJ Neff, H AF Glascock, M. D. Speakman, R. J. Neff, H. TI Archaeometry at the University of Missouri Research Reactor and the provenance of obsidian artefacts in North America SO ARCHAEOMETRY LA English DT Article DE neutron activation analysis; obsidian; ceramics; chert; great plains; eastern North America ID NEUTRON-ACTIVATION ANALYSIS; CHEMICAL DIFFERENTIATION; ACID-EXTRACTION; CERAMICS; ICP AB Descriptions of the history of the Archaeometry Laboratory at the University of Missouri Research Reactor and the procedures used for instrumental neutron activation analysis of archaeological materials are presented. The laboratory was established in 1988 to support students and faculty from the University of Missouri and other universities who were interested in archaeological research involving compositional analysis. The results obtained from the analysis of obsidian sources and artefacts from locations in the continental USA are presented for illustration. C1 Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. Calif State Univ Long Beach, Dept Anthropol, Long Beach, CA 90840 USA. RP Glascock, MD (reprint author), Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. OI Glascock, Michael D./0000-0003-0686-7556; Speakman, Robert/0000-0003-2063-154X NR 44 TC 27 Z9 27 U1 0 U2 6 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD MAY PY 2007 VL 49 BP 343 EP 357 DI 10.1111/j.1475-4754.2007.00305.x PN 2 PG 15 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA 174BC UT WOS:000246915200012 ER PT J AU Gramajo, LV Whitney, BA Kenyon, SJ Gomez, M Merrill, KM AF Gramajo, Luciana V. Whitney, Barbara A. Kenyon, Scott J. Gomez, Mercedes Merrill, K. M. TI High spatial resolution near-infrared images of Taurus protostars SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; stars : formation; stars : imaging ID YOUNG STELLAR OBJECTS; AURIGA MOLECULAR CLOUD; CLASS-I PROTOSTARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; OPHIUCHI DARK CLOUD; HARO ENERGY-SOURCES; PROTOSTELLAR ENVELOPES; SUBMILLIMETER CONTINUUM; SIZE DISTRIBUTION; STAR-FORMATION AB We analyze near-infrared K- and L-band images of six embedded Class I objects in the Taurus-Auriga molecular cloud. Three of these sources were observed in both bands and three were observed only at L. The L- and K-band images were obtained with the Cryogenic Optical Bench at the KPNO 4 m telescope in the diffraction-limited mode. With the high spatial resolution L-band data, we identify IRAS 04239+2436 as a close pair with a projected separation of 0.29 ''. We use a radiative transfer code to model the images and derive physical and geometrical parameters for each source. Because the projected positions of the six analyzed sources on the cloud coincide with the densest zones in the complex (AV similar to 10-30 mag), we use two models for the optical properties of dust grains in the envelopes: a diffuse ISM model and a grain model with ratio of total to selective extinction RV 4: 3 corresponding to the measured R values in the densest regions of the Taurus molecular cloud. Although the two grain models have different opacities, we can match the observed images with either model by selecting the appropriate envelope infall rate. Thus we cannot distinguish between the two grain models over this narrow wavelength range (K and L bands). C1 Univ Nacl Cordoba, Astron Observ, RA-5000 Cordoba, Argentina. Space Sci Inst, Boulder, CO 80301 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Gramajo, LV (reprint author), Univ Nacl Cordoba, Astron Observ, RA-5000 Cordoba, Argentina. EM luciana@oac.uncor.edu; bwhitney@spacescience.org; skenyon@cfa.harvard.edu; mercedes@oac.uncor.edu; merrill@noao.edu OI Kenyon, Scott/0000-0003-0214-609X NR 91 TC 6 Z9 6 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 2007 VL 133 IS 5 BP 1911 EP 1926 DI 10.1086/512608 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 165XY UT WOS:000246342200007 ER PT J AU Matthews, LD Reid, MJ AF Matthews, Lynn D. Reid, Mark J. TI Very Large Array observations of HI in the circumstellar envelopes of asymptotic giant branch stars SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; radio continuum : stars; radio lines : stars; stars : AGB and post-AGB; stars : atmospheres ID CIRCUMNEBULAR NEUTRAL HYDROGEN; RADIO-CONTINUUM EMISSION; SMALL-SCALE STRUCTURE; IRAS SURVEY DATA; R-AQUARII JET; PLANETARY-NEBULAE; EVOLVED STARS; ATOMIC-HYDROGEN; VLA OBSERVATIONS; ALPHA-ORIONIS AB We have used the Very Large Array to search for neutral atomic hydrogen (H Iota) in the circumstellar envelopes of five asymptotic giant branch stars. We have detected H Iota 21 cm emission coincident in both position and velocity with the S-type semiregular variable star RS Cnc. The emission comprises a compact, slightly elongated feature centered on the star with a mean diameter of similar to 82 '' (1.5 x 10(17) cm), plus an additional filament extending similar to 6 ' to the northwest. If this filament is associated with RS Cnc, it would imply that a portion of its mass loss is highly asymmetric. We estimate MH Iota approximate to 1.5 x 10(-3) M-circle dot and a mass-loss rate. M approximate to 1.7 x 10(-7) M-circle dot yr(-1). Toward three other stars (IRC+10216, EPAqr, R Cas) we have detected arcminute-scale H Iota emission features at velocities consistent with the circumstellar envelopes, but spatially offset from the stellar positions. Toward R Cas, the emission is weak but peaks at the stellar systemic velocity and overlaps with the location of its circumstellar dust shell and thus is probably related to the star. In the case of IRC+10216, we were unable to confirm the detection of H Iota in absorption against the cosmic background previously reported by Le Bertre & Gerard. However, we detect arcs of emission at projected distances of r similar to 14 '-18 ' (similar to 2 x 10(18) cm) to the northwest of the star. The large separation of the emission from the star is plausible, given its advanced evolutionary status, although it is unclear if the asymmetric distribution and complex velocity structure are consistent with a circumstellar origin. For EPAqr, the detected H Iota emission comprises multiple clumps redward of the systemic velocity, but we are unable to determine unambiguously whether the emission arises from the circumstellar envelope or from interstellar clouds along the line of sight. Regardless of the adopted distance for the H Iota clumps, their inferred H Iota masses are at least an order of magnitude smaller than their individual gravitational binding masses. We did not detect any H Iota emission from our fifth target, R Aqr ( a symbiotic binary), but measured a 1.4 GHz continuum flux density of 18.8 +/- 0.7 mJy. R Aqr is a previously known radio source, and the 1.4 GHz emission likely arises primarily from free-free emission from an ionized circumbinary envelope. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matthews, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 89 TC 27 Z9 27 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 2007 VL 133 IS 5 BP 2291 EP 2309 DI 10.1086/512613 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 165XY UT WOS:000246342200040 ER PT J AU Pillai, T Wyrowski, F Hatchell, J Gibb, AG Thompson, MA AF Pillai, T. Wyrowski, F. Hatchell, J. Gibb, A. G. Thompson, M. A. TI Probing the initial conditions of high mass star formation - I. Deuteration and depletion in high mass pre/protocluster clumps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; astrobiology; molecular data; methods : observational; ISM : clouds; radio lines : ISM ID INFRARED-DARK CLOUDS; HOT MOLECULAR CORES; PROTOSTELLAR CORES; DEUTERIUM FRACTIONATION; INTERSTELLAR-MEDIUM; CO DEPLETION; PHYSICAL-PROPERTIES; ABUNDANCE RATIO; DENSE CORES; AMMONIA AB Aims. UltraCompact HII regions are signposts of high-mass star formation. Since high-mass star formation occurs in clusters, one expects to find even earlier phases of massive star formation in the vicinity of UltraCompact HII regions. Here, we study the amount of deuteration and depletion toward pre/protocluster clumps found in a wide-field ( 10 x 10 arcmin) census of clouds in 32 massive star-forming regions that are known to harbour UCHII regions. Methods. We determine the column density of NH(3), NH(2)D, CO, H(13)CN, and HC(15)N lines. We used the (J, K) = (1, 1) and (2, 2) inversion transitions of NH(3) to constrain the gas temperatures. Results. We find that 65% of the observed sources have strong NH(2)D emission and more than 50% of the sources exhibit a high degree of deuteration, (0.1 <= NH(2)D/ NH(3) <= 0.7), 0.7 being the highest observed deuteration of NH(3) reported to date. Our search for NHD(2) in two sources did not result in a detection. The enhancement in deuteration coincides with moderate CO depletion onto dust grains. There is no evidence of a correlation between the two processes, though an underlying correlation cannot be ruled out as the depletion factor is very likely to be only a lower limit. Based on simultaneously observed H(13)CN and HC(15)N ( J = 1 - 0) lines, we derive a high abundance ratio of H(13)CN to HC(15)N, which might indicate anomalous ratios of C and N isotopes relative to those derived toward the local ISM. Conclusions. We find CO depletion and high deuteration towards cold cores in massive star forming regions. Therefore, these are good candidates for sources at the early phases of massive star formation. While our sensitive upper limits on NHD(2) do not prove the predictions of the gas-phase and grain chemistry models wrong, an enhancement of approximate to 10(4) over the cosmic D/H ratio from NH(2)D warrants explanation. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. RP Pillai, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tpillai@cfa.harvard.edu NR 60 TC 49 Z9 49 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 467 IS 1 BP 207 EP + DI 10.1051/0004-6361:20065682 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166YU UT WOS:000246417900023 ER PT J AU Cernicharo, J Guelin, M Agundez, M Kawaguchi, K McCarthy, M Thaddeus, P AF Cernicharo, J. Guelin, M. Agundez, M. Kawaguchi, K. McCarthy, M. Thaddeus, P. TI Astronomical detection of C4H-, the second interstellar anion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : individual : IRC+10216; stars : carbon; radio lines : stars; astrochemistry; line : identification; stars : AGB and post-AGB ID NEGATIVE-IONS; CIRCUMSTELLAR ENVELOPES; MOLECULAR-IONS; LINE SURVEY; IRC+10216; CHEMISTRY; CLOUDS; PHOTOCHEMISTRY; ATTACHMENT; RADICALS AB Aims. Following the recent detection of C6H- in the laboratory and in space we have succeeded in studying the microwave spectrum of C4H-. We report here the first detection in space of this negative ion. Methods. We have observed in the envelope of the carbon star IRC + 10216 five lines corresponding to the J = 9- 8, 11-10, 12-11, 14-13 and 15-14 rotational transitions of C4H-. The C4H- lines have a cusped shape, denoting that this ion is formed in the outer part of the envelope, like its neutral counterpart C4H. Results. The abundance of C4H- in IRC+ 10216 is 1/6 of the abundance of C6H- and 1/4200 of that of C4H. Conclusions. The detection of C4H-, after that of C6H-, confirms the theoretical prediction that C-chain anions are abundant in interstellar clouds and yields a first measurement of the electron radiative attachment rates. C1 CSIC, Inst Estructura Mat, Dept Mol & Infrared Astrophys, E-28006 Madrid, Spain. IRAM, F-38400 St Martin Dheres, France. Okayama Univ, Fac Sci, Dept Chem, Okayama 7008530, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cernicharo, J (reprint author), CSIC, Inst Estructura Mat, Dept Mol & Infrared Astrophys, Serrano 121, E-28006 Madrid, Spain. EM cerni@damir.iem.csic.es; guelin@iram.fr RI Kawaguchi, Kentarou/B-1758-2011; Agundez, Marcelino/I-5369-2012; OI Kawaguchi, Kentarou/0000-0003-1067-1839; Agundez, Marcelino/0000-0003-3248-3564; McCarthy, Michael/0000-0001-9142-0008 NR 23 TC 141 Z9 141 U1 2 U2 12 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 467 IS 2 BP L37 EP L40 DI 10.1051/0004-6361:20077415 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 167BF UT WOS:000246424900003 ER PT J AU Kraus, S Balega, YY Berger, JP Hofmann, KH Millan-Gabet, R Monnier, JD Ohnaka, K Pedretti, E Preibisch, T Schertl, D Schloerb, FP Traub, WA Weigelt, G AF Kraus, S. Balega, Y. Y. Berger, J.-P. Hofmann, K.-H. Millan-Gabet, R. Monnier, J. D. Ohnaka, K. Pedretti, E. Preibisch, Th. Schertl, D. Schloerb, F. P. Traub, W. A. Weigelt, G. TI Visual/infrared interferometry of Orion Trapezium stars: preliminary dynamical orbit and aperture synthesis imaging of the theta(1) Orionis C system SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : pre-main sequence; stars : fundamental parameters; stars : binaries : close; techniques : interferometric; stars : individual : theta(1) Orionis C, theta(1) Orionis D ID GALACTIC-O-STARS; NEBULA CLUSTER; SPECKLE-MASKING; MAIN-SEQUENCE; STELLAR PARAMETERS; RADIAL-VELOCITY; MAGNETIC-FIELD; MASSIVE STARS; BEAM COMBINER; BINARY STARS AB Context. Located in the Orion Trapezium cluster,theta(1)OriC is one of the youngest and nearest high-mass stars (O5-O7) known. Besides its unique properties as a magnetic rotator, the system is also known to be a close binary. Aims. By tracing its orbital motion, we aim to determine the orbit and dynamical mass of the system, yielding a characterization of the individual components and, ultimately, also new constraints for stellar evolution models in the high-mass regime. Furthermore, a dynamical parallax can be derived from the orbit, providing an independent estimate for the distance of the Trapezium cluster. Methods. Using new multi-epoch visual and near-infrared bispectrum speckle interferometric observations obtained at the BTA 6 m telescope, and IOTA near-infrared long- baseline interferometry, we traced the orbital motion of the theta(1)OriC components over the interval 1997.8 to 2005.9, covering a significant arc of the orbit. Besides fitting the relative position and the flux ratio, we applied aperture synthesis techniques to our IOTA data to reconstruct a model-independent image of the theta(1)OriC binary system. Results. The orbital solutions suggest a highly eccentricity (e approximate to 0.91) and short-period (P approximate to 10.9 yrs) orbit. As the current astrometric data only allows rather weak constraints on the total dynamical mass, we present the two best-fit orbits. Of these two, the one implying a system mass of 48 M-circle dot and a distance of 434 pc to the Trapezium cluster can be favored. When also taking the measured flux ratio and the derived location in the HR-diagram into account, we find good agreement for all observables, assuming a spectral type of O5.5 for theta(1)Ori C1 (M = 34.0 M-circle dot, T-eff = 39 900 K) and O9.5 for C2 (M = 15.5 M-circle dot, T-eff = 31 900 K). Using IOTA, we also obtained first interferometric observations on.1Ori D, finding some evidence for a resolved structure, maybe by a faint, close companion. Conclusions. We find indications that the companion C2 is massive itself, which makes it likely that its contribution to the intense UV radiation field of the Trapezium cluster is non-negligible. Furthermore, the high eccentricity of the preliminary orbit solution predicts a very small physical separation during periastron passage (similar to 1.5 AU, next passage around 2007.5), suggesting strong wind-wind interaction between the two O stars. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Russian Acad Sci, Special Astrophys Observ, Karachai Cherkesia 357147, Russia. Univ Grenoble 1, Lab Astrophys Grenoble, UMR 5571, CNRS, F-38041 Grenoble, France. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48104 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02183 USA. RP Kraus, S (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM skraus@mpifr-bonn.mpg.de NR 63 TC 66 Z9 68 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 466 IS 2 BP 649 EP 659 DI 10.1051/0004-6361:20066965 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YW UT WOS:000245686800026 ER PT J AU Gillon, M Pont, F Moutou, C Santos, NC Bouchy, F Hartman, JD Mayor, M Melo, C Queloz, D Udry, S Magain, P AF Gillon, M. Pont, F. Moutou, C. Santos, N. C. Bouchy, F. Hartman, J. D. Mayor, M. Melo, C. Queloz, D. Udry, S. Magain, P. TI The transiting planet OGLE-TR-132b revisited with new spectroscopy and deconvolution photometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars : individual : OGLE-TR-132; techniques : photometric; techniques : image processing; methods : data analysis ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; DOPPLER FOLLOW-UP; IMAGE SUBTRACTION; ACCURATE RADIUS; CANDIDATES; STARS; FIELD; MASS AB OGLE-TR-132b transits a very metal-rich F dwarf about 2000 pc from the Sun, in the Galactic disc towards Carina. It orbits very close to its host star (a = 0.03 AU) and has an equilibrium temperature of nearly 2000 K. Using rapid-cadence transit photometry from the FORS2 camera on the VLT and SUSI2 on the NTT, and high-resolution spectroscopy with UVES on the VLT, we refine the shape of the transit light curve and the parameters of the system. In particular, we improve the planetary radius estimate, R = 1.18 +/- 0.07 R-J and provide very precise ephemeris, T-tr = 2 453 142.59123 +/- 0.0003 BJD and P = 1.689868 +/- 0.000003 days. The obtained planetary mass is 1.14 +/- 0.12 M-J. Our results give a slightly smaller and lighter star, and bigger planet, than previous values. As the VLT/FORS2 light curve obtained in this analysis with the deconvolution photometry algorithm DECPHOT shows a transit depth in disagreement with the one obtained by a previous study using the same data, we analyze them with two other reduction methods (aperture and image subtraction). The light curves obtained with the three methods are in good agreement, though deconvolution-based photometry is significantly more precise. It appears from these results that the smaller transit depth obtained in the previous study was due to a normalisation problem inherent to the reduction procedure used. C1 Observ Geneva, CH-1290 Sauverny, Switzerland. Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. Traverse Siphon, LAM, F-13376 Marseille, France. Univ Lisbon, Ctr Astron & Astrofis, Observ Astron Lisboa, P-1349018 Lisbon, Portugal. Ctr Geofis Evora, P-7002554 Evora, Portugal. Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, Santiago 19, Chile. RP Gillon, M (reprint author), Observ Geneva, 51 Chemin Maillettes, CH-1290 Sauverny, Switzerland. EM michael.gillon@obs.unige.ch RI Santos, Nuno/E-9957-2011; Melo, Claudio/O-2797-2013; OI Santos, Nuno/0000-0003-4422-2919; Hartman, Joel/0000-0001-8732-6166 NR 27 TC 32 Z9 32 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 466 IS 2 BP 743 EP 748 DI 10.1051/0004-6361:20066367 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YW UT WOS:000245686800039 ER PT J AU Stauber, P Benz, AO Jorgensen, JK van Dishoeck, EF Doty, SD van der Tak, FFS AF Staeuber, P. Benz, A. O. Jorgensen, J. K. van Dishoeck, E. F. Doty, S. D. van der Tak, F. F. S. TI Tracing high energy radiation with molecular lines near deeply embedded protostars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; stars : low-mass, brown dwarfs; ISM : molecules; X-rays : ISM ID YOUNG STELLAR OBJECTS; X-RAY-EMISSION; MASS PROTOSTELLAR ENVELOPES; PHOTON-DOMINATED REGIONS; STAR-FORMING REGIONS; GAS-PHASE H2O; CHEMICAL-STRUCTURE; INTERSTELLAR SO+; IRAS 16293-2422; IC-63 NEBULA AB Aims. The aim is to probe high energy radiation emitted by deeply embedded protostars. Methods. Submillimeter lines of CN, NO, CO+ and SO+, and upper limits on SH+ and N2O are observed with the James Clerk Maxwell Telescope in two high-mass and up to nine low-mass young stellar objects and compared with chemical models. Results. Constant fractional abundances derived from radiative transfer modeling of the line strengths are x( CN) approximate to a few x 10(-11) - 10(-8), x(NO) approximate to 10(-9) - 10(-8) and x(CO+) approximate to 10(-12) - 10(-10). SO+ has abundances of a few x 10(-11) in the high-mass objects and upper limits of approximate to 10(-12) - 10(-11) in the low-mass sources. All abundances are up to 1 - 2 orders of magnitude higher if the molecular emission is assumed to originate mainly from the inner region ( less than or similar to 1000 AU) of the envelope. For high-mass sources, the CN, SO+ and CO+ abundances and abundance ratios are best explained by an enhanced far-ultraviolet (FUV) field impacting gas at temperatures of a few hundred K. The observed column densities require that this region of enhanced FUV has scales comparable to the observing beam, such as in a geometry in which the enhanced FUV irradiates outflow walls. For low-mass sources, the required temperatures within the FUV models of T greater than or similar to 300 K are much higher than found in models, so that an X-ray enhanced region close to the protostar ( r less than or similar to 500 AU) is more plausible. Gas-phase chemical models produce more NO than observed, suggesting an additional reduction mechanism not included in current models. Conclusions. The observed CN, CO+ and SO+ abundances can be explained with either enhanced X-rays or FUV fields from the central source. High-mass sources likely have low opacity regions that allow the FUV photons to reach large distances from the central source. X-rays are suggested to be more effective than FUV fields in the low-mass sources. The observed abundances imply X-ray fluxes for the Class 0 objects of L-X approximate to 10(29) - 10(31) erg s(-1), comparable to those observed from low-mass Class I protostars. Spatially resolved data are needed to clearly distinguish the effects of FUV and X-rays for individual species. C1 ETH, Inst Astron, CH-8092 Zurich, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. SRON, Natl Inst Space Res, NL-9747 AD Groningen, Netherlands. RP Stauber, P (reprint author), ETH, Inst Astron, CH-8092 Zurich, Switzerland. EM pascalst@astro.phys.ethz.ch NR 59 TC 20 Z9 20 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 466 IS 3 BP 977 EP U147 DI 10.1051/0004-6361:20065762 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 161IF UT WOS:000246007400019 ER PT J AU Beuther, H Walsh, AJ Thorwirth, S Zhang, Q Hunter, TR Megeath, ST Menten, KM AF Beuther, H. Walsh, A. J. Thorwirth, S. Zhang, Q. Hunter, T. R. Megeath, S. T. Menten, K. M. TI Hot ammonia in NGC 6334I & I(N) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; stars : early-type; stars : formation; ISM : individual objects : NGC 6334I and I( N); line : profiles; masers ID H-II REGIONS; NGC 6334 I; STAR-FORMATION; METHANOL MASERS; EMISSION; OUTFLOW; NH3; OH; CONTINUUM; COMPLEX AB Aims. The massive twin cores NGC 6334I and I(N) are in different evolutionary stages and hence ideal targets to study evolutionary variations within the same larger-scale environment. Here, we study the warm, compact gas components. Methods. We imaged the two regions with the Australia Telescope Compact Array ( ATCA) at high angular resolution in the NH3(3, 3) to ( 6, 6) inversion lines. Results. Compact emission is detected toward both regions in all observed inversion lines with energy levels up to 407 K above ground. This is particularly surprising for NGC 6334I( N) since it lacks bright infrared emission and is considered a massive cold core at an early evolutionary stage. High optical depth and multiply-peaked line profiles complicate rotation temperature estimates, and we can only conclude that gas components with temperatures > 100 K are present in both regions. Toward NGC 6334I, we confirm previous reports of NH3(3, 3) maser emission toward the outflow bow-shocks. Furthermore, we report the first detection of an NH3(6, 6) maser toward the central region of NGC 6334I. This maser is centered on the second millimeter (mm) peak and elongated along the outflow axis, indicating that this mm continuum core harbors the driving source of the molecular outflow. Toward the main mm peak in NGC 6334I( N), we detect a double-horn line profile in the NH3(6, 6) transition. The current data do not allow us to differentiate whether this double-horn profile is produced by multiple gas components along the line of sight, or whether it may trace a potential underlying massive accretion disk. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. James Cook Univ N Queensland, Townsville, Qld 4811, Australia. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. RP Beuther, H (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM beuther@mpia.de; Andrew.Walsh@jcu.edu.au; sthorwirth@mpifr-bonn.mpg.de; zhang@cfa.harvard.edu; thunter@nrao.edu; megeath@astro1.panet.utoledo.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; Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 39 TC 31 Z9 31 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 466 IS 3 BP 989 EP 998 DI 10.1051/0004-6361:20066799 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 161IF UT WOS:000246007400020 ER PT J AU Beuther, H Leurini, S Schilke, P Wyrowski, F Menten, KM Zhang, Q AF Beuther, H. Leurini, S. Schilke, P. Wyrowski, F. Menten, K. M. Zhang, Q. TI Interferometric multi-wavelength (sub) millimeter continuum study of the young high-mass protocluster IRAS 05358+3543 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; stars : early-type; stars : individual : IRAS 05358+3543; ISM : dust, extinction; ISM : jets and outflows ID STAR-FORMING REGIONS; ORION NEBULA CLUSTER; DUST CONTINUUM; PROTOSTELLAR CANDIDATES; METHANOL MASERS; CIRCUMSTELLAR ENVIRONMENTS; PHYSICAL PARAMETERS; SOUTHERN-HEMISPHERE; MOLECULAR OUTFLOWS; EMISSION AB Aims. We study the small-scale structure of massive star-forming regions through interferometric observations in several ( sub) mm wavelength bands. These observations resolve multiple sources, yield mass and column density estimates, and give information about the density profiles as well as the dust and temperature properties. Methods. We observed the young massive star-forming region IRAS 05358+3543 at high spatial resolution in the continuum emission at 3.1 and 1.2mm with the Plateau de Bure Interferometer, and at 875 and 438 mu m with the Submillimeter Array. The observations are accompanied by VLA 3.6 cm archival continuum data. Results. We resolve at least four continuum sub-sources that are likely of protostellar nature. Two of them are potentially part of a proto-binary system with a projected separation of 1700 AU. Additional ( sub) mm continuum peaks are not necessarily harboring protostars but maybe caused by the multiple molecular outflows. The spectral energy distributions ( SEDs) of the sub-sources show several features. The main power house mm1, which is associated with CH3OH maser emission, a hypercompact HII region and a mid-infrared source, exhibits a typical SED with a free-free emission component at cm and long mm wavelengths and a cold dust component in the ( sub) mm part of the spectrum ( spectral index between 1.2mm and 438 mu m m alpha similar to 3.6). The free-free emission corresponds to a Lyman continuum flux of an embedded 13 M-circle dot B1 star. The coldest source of the region, mm3, has alpha similar to 3.7 between 1.2 mm and 875 mu m, but has lower than expected fluxes in the shorter wavelength 438 mu m band. This turnover of the Planck-function sets an upper limit on the dust temperature of mm3 of approximately 20 K. The uv-data analysis of the density structure of individual sub-cores reveals distributions with power-law indices between 1.5 and 2. This resembles the density distributions of the larger-scale cluster-forming clump as well as those from typical low-mass cores. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Max Planck Inst Radioastron, D-53121 Bonn, Germany. European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beuther, H (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM beuther@mpia.de; sleurini@eso.org; p.schilke@mpifr-bonn.mpg.de; k.m.menten@mpifr-bonn.mpg.de; qzhang@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 60 TC 46 Z9 47 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 466 IS 3 BP 1065 EP 1076 DI 10.1051/0004-6361:20066742 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 161IF UT WOS:000246007400029 ER PT J AU Carpano, S Pollock, AMT Prestwich, A Crowther, P Wilms, J Yungelson, L Ehle, M AF Carpano, S. Pollock, A. M. T. Prestwich, A. Crowther, P. Wilms, J. Yungelson, L. Ehle, M. TI A 33 hour period for the Wolf-Rayet/black hole X-ray binary candidate NGC 300 X-1 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : individuals : NGC 300 X-1; X-rays : binaries; stars : Wolf-Rayet ID SPACED DATA; BLACK-HOLE; CYGNUS X-3; IC-10 X-1; STARS; GALAXY; TELESCOPE; EMISSION; CHANDRA AB Context. NGC 300 X-1 is the second extragalactic candidate, after IC 10 X-1, in the rare class of Wolf-Rayet/compact object X-ray binary systems exemplified in the Galaxy by Cyg X-3. From a theoretical point of view, accretion onto a black hole in a detached system is possible for large orbital periods only if the mass of the relativistic object is high or the velocity of the accreted wind is low. Aims. We analysed a 2 week SWIFT XRT light curve of NGC 300 X-1 and searched for periodicities. Methods. Period searches were made using Lomb-Scargle periodogram analysis. We evaluated the confidence level using Monte Carlo simulations. Results. A period of 32.8 +/- 0.4 h (3 sigma error) was found for NGC 300 X-1 with a confidence level > 99%. Furthermore, we confirm the high irregular variability during the high flux level, as already observed in the XMM-Newton observations of the source. A folded XMM-Newton light curve is shown, with a profile that is in agreement with SWIFT. The mean absorbed X-ray luminosity in the SWIFT observations was 1.5 x 10(38) erg s(-1), close to the value derived from the XMM-Newton data. Conclusions. While Cyg X-3 has a short period of 4.8 h, the period of NGC 300 X-1 is very close to that of IC 10 X-1 (34.8 +/- 0.9 h). These are likely orbital periods. Possibility of formation of accretion disk for such high orbital periods strongly depends on the terminal velocity of the Wolf-Rayet star wind and black-hole mass. While low masses are possible for wind velocities <= 1000 km s(-1), these increase to several tens of solar masses for velocities > 1600 km s(-1) and no accretion disk may form for terminal velocities larger than 1900 km s(-1). C1 ESA, ESAC, XMN Newton Sci Operat Ctr, Madrid 28080, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. FAU Erlangen Nurnberg, Dr Remeis Observ, Inst Astron, D-96049 Bamberg, Germany. Russian Acad Sci, Inst Astron, Moscow 119017, Russia. RP Carpano, S (reprint author), ESA, ESAC, XMN Newton Sci Operat Ctr, POB 50727, Madrid 28080, Spain. EM scarpano@sciops.esa.int RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Crowther, Paul/0000-0001-6000-6920 NR 25 TC 24 Z9 24 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2007 VL 466 IS 2 BP L17 EP L20 DI 10.1051/0004-6361:20077363 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YW UT WOS:000245686800005 ER PT J AU Poindexter, S Morgan, N Kochanek, CS Falco, EE AF Poindexter, Shawn Morgan, Nicholas Kochanek, Christopher S. Falco, Emilio E. TI Mid-IR observations and a revised time delay for the gravitational lens system quasar He 1104-1805 SO ASTROPHYSICAL JOURNAL LA English DT Article ID SPACE-TELESCOPE; HE 1104-1805; GALAXIES; SUBSTRUCTURE; DUST AB The mid-IR flux ratios F(A)/F(B) = 2.84 +/- 0.06 of the two images of the gravitationally lensed quasar HE 1104- 1805 show no wavelength dependence to within 3% across 3.6-8.0 mu m, show no time dependence over 6 months, and agree with the broad emission-line flux ratios. This indicates that the mid-IR emission likely comes from scales large enough to be little affected by microlensing and that there is little differential extinction between the images. We measure a revised time delay between these two images of 152.2(-3.0)(+2.8) (1 sigma) days from R- and V-band data covering the years 1997-2006. This time delay indicates that the lens has an approximately flat rotation curve over scales of 1-2R(e). We also observed uncorrelated variations of similar to 0.05 mag yr(-1), which we attribute to microlensing of the optical emission from the accretion disk. The optical colors have also changed significantly in the sense that image A is now redder than image B, rather than bluer, as it was in 1993. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Poindexter, S (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. EM sdp@astronomy.ohio-state.edu; nmorgan@astronomy.ohio-state.edu; ckochanek@astronomy.ohio-state.edu NR 30 TC 33 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2007 VL 660 IS 1 BP 146 EP 151 DI 10.1086/512773 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162SB UT WOS:000246108700009 ER PT J AU Croston, JH Kraft, RP Hardcastle, MJ AF Croston, J. H. Kraft, R. P. Hardcastle, M. J. TI Shock heating in the nearby radio galaxy NGC 3801 SO ASTROPHYSICAL JOURNAL LA English DT Article ID XMM-NEWTON OBSERVATIONS; CCD SURFACE PHOTOMETRY; X-RAY; ELLIPTIC GALAXIES; CENTAURUS-A; FR-I; DYNAMICAL MODELS; H-I; CHANDRA; JET AB We report the Chandra detection of shock-heated shells of hot gas surrounding the radio lobes of the nearby (D-L similar to 53 Mpc) low-power radio galaxy NGC 3801. The shells have temperatures of 1 and 0.7 keV, compared to an ISM temperature of 0.23 keV. The estimated expansion speed of the shells is similar to 850 km s(-1), corresponding to a Mach number of similar to 4. This is the second X-ray detection of strong shocks produced by a low-power radio galaxy, and allows us to measure directly the contribution of shock heating to the radio galaxy's total energetic input to the ISM. We show that the gas properties of the shells and surrounding ISM are consistent with the Rankine-Hugoniot shock jump conditions. We estimate the energy stored in the hot gas shells (thermal + kinetic energy) to be 1.7 x 10(56) ergs, which is equivalent to the thermal energy of the ISM within similar to 11 kpc of the galaxy center, and a factor of similar to 25 larger than the inferred P dV work required to inflate the lobe cavities, indicating that energy transfer from the AGN to its environment is dominated by shock heating during this stage of radio-source evolution. Our results provide direct evidence that shock heating in the early supersonic phase of FR I radio-source expansion can have important long-term effects on the properties of the host galaxy ISM. Finally, we discuss the merger history of NGC 3801, the fueling of its AGN and the role of this type of system in feedback models. C1 Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Croston, JH (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 30 TC 42 Z9 42 U1 0 U2 6 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 2007 VL 660 IS 1 BP 191 EP 199 DI 10.1086/513500 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162SB UT WOS:000246108700012 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ AF Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. Kurtz, Michael J. TI Hypervelocity stars. II. The bound population SO ASTROPHYSICAL JOURNAL LA English DT Article ID HORIZONTAL-BRANCH STARS; DIGITAL SKY SURVEY; GALACTIC HALO PROJECT; FAINT BLUE STARS; BLACK-HOLE; HOT STARS; O-STAR; SDSS J090745.0+024507; RADIAL-VELOCITIES; DATA RELEASE AB Hypervelocity stars (HVSs) are stars ejected completely out of the Milky Way by three-body interactions with the massive black hole in the Galactic center. We describe 643 new spectroscopic observations from our targeted survey for HVSs. We find a significant ( 3.5 sigma) excess of B-type stars with large velocities +275 km s(-1) < v(rf) < 450 km s(-1) and distances d > 10 kpc that are most plausibly explained as a new class of HVSs: stars ejected from the Galactic center on bound orbits. If a Galactic center ejection origin is correct, the distribution of HVSs on the sky should be anisotropic for a survey complete to a fixed limiting apparent magnitude. The unbound HVSs in our survey have a marginally anisotropic distribution on the sky, consistent with the Galactic center ejection picture. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 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 65 TC 55 Z9 56 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 MAY 1 PY 2007 VL 660 IS 1 BP 311 EP 318 DI 10.1086/513595 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162SB UT WOS:000246108700023 ER PT J AU Strohmayer, TE Mushotzky, RF Winter, L Soria, R Uttley, P Cropper, M AF Strohmayer, Tod E. Mushotzky, Richard F. Winter, Lisa Soria, Roberto Uttley, Phil Cropper, Mark TI Quasi-periodic variability in NGC 5408 X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article ID X-RAY SOURCE; MASS BLACK-HOLES; XMM-NEWTON OBSERVATIONS; MICROQUASAR GRO J1655-40; XTE J1550-564; ACCRETION DISKS; NEARBY GALAXIES; M82 X-1; OSCILLATIONS; FREQUENCY AB We report the discovery with XMM-Newton of quasi-periodic variability in the 0.2-10 keV X-ray flux from the ULX NGC 5408 X-1. The average power spectrum of all EPIC-pn data reveals a strong 20 mHz QPO with an average amplitude (rms) of 9% and a coherence Q equivalent to nu(0)/sigma approximate to 6. In a 33 ks time interval when the 20 mHz QPO is strongest we also find evidence for a second QPO peak at 15 mHz, the first indication of a close pair of QPOs in a ULX source. The frequency ratio of this QPO pair is inconsistent with 3: 2 at the 3 sigma level but is consistent with a 4: 3 ratio. A power-law noise component with slope near 1.5 is also present below 0.1 Hz with evidence for a break to a flatter slope at about 3 mHz. The source shows substantial broadband variability, with a total amplitude (rms) of about 30% in the 0.1-100 mHz frequency band. The power spectrum of hard X-ray photons (> 2 keV) shows a "`classic'' flat-topped continuum breaking to a power law with index 1.5-2. Both the break and 20 mHz QPO are detected in the hard band, and the 20 mHz QPO is essentially at the break. The QPO is both strong and narrow in this band, having an amplitude (rms) of 15%, and Q approximate to 25. Both the timing and spectral properties of NGC 5408 X-1 are strikingly reminiscent of Galactic black holes at high inferred accretion rates, but with its characteristic frequencies (QPO and break frequencies) scaled down by a factor of 10-100. We discuss the implications of these findings for the object's mass. C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Strohmayer, TE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM stroh@milkyway.gsfc.nasa.gov; richard@milkyway.gsfc.nasa.gov; lwinter@astro.umd.edu; rsoria@head.cfa.harvard.edu; msc@mssl.ucl.ac.uk RI Cropper, Mark/C-1574-2008; OI Winter, Lisa/0000-0002-3983-020X NR 54 TC 92 Z9 93 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 1 PY 2007 VL 660 IS 1 BP 580 EP 586 DI 10.1086/512723 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162SB UT WOS:000246108700047 ER PT J AU Nichols, JS DePasquale, J Kellogg, E Anderson, CS Sokoloski, J AF Nichols, J. S. DePasquale, J. Kellogg, E. Anderson, C. S. Sokoloski, J. TI Discovery of rapid hard X-ray variability and new jet activity in the symbiotic binary R aquarii SO ASTROPHYSICAL JOURNAL LA English DT Article ID CH-CYGNI; CATACLYSMIC VARIABLES; WHITE-DWARF; EX-HYDRAE; INTERMEDIATE POLAR; ASCA OBSERVATIONS; RADIO JET; ULTRAVIOLET; CAMELOPARDALIS; EMISSION AB Two Chandra observations of the R Aqr symbiotic binary system taken 3.3 yr apart show dramatic changes in the X-ray morphology and spectral characteristics in the inner 500 AU of this system. The morphology of the soft X-ray emission has evolved from a nearly circular region centered on the binary system to an hourglass shape that indicates the formation of a new southwest jet. Synchrotron radiation from the new jet in contemporaneous VLA radio spectra implies the physical conditions in the early stages of jet development are different from those in the more extended outer thermal jets known to exist for decades in this system. The central binary source has two X-ray spectral components in each of the two epochs, a soft component and a highly absorbed hard component characterized by T similar to 10(8) K if fit with a thermal plasma model. The spectrum hardened considerably between 2000.7 and 2004.0, primarily due to increased flux above 5 keV, suggesting a change in the accretion activity of the white dwarf on a timescale of a few years or less. Point-source Fe K emission is detected at the position of the central binary system in both observations. While the earlier observation shows evidence of only a single emission peak near Fe K alpha at 6.4 keV, the later observation shows a more complex emission structure between 6 and 7 keV. Finally, we have discovered a modulation in the hard X-ray flux with a period of 1734 s at a 95% confidence level in the 2004 observation only. The modulation potentially arises from standing shocks in an accretion column, and we have explored the possibility that the white dwarf in R Aqr is analogous to the magnetic white dwarfs in Intermediate Polars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nichols, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jnichols@cfa.harvard.edu NR 52 TC 20 Z9 20 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 1 PY 2007 VL 660 IS 1 BP 651 EP 661 DI 10.1086/512138 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162SB UT WOS:000246108700053 ER PT J AU Stassun, KG van den Berg, M Feigelson, E AF Stassun, Keivan G. van den Berg, M. Feigelson, Eric TI A simultaneous optical and X-ray variability study of the orion nebula cluster. II. A common origin in magnetic activity SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Orion Nebula Cluster); stars : flare; stars : magnetic fields; stars : pre-main-sequence; stars : spots; X-rays : stars ID CLASSICAL T-TAURI; MAIN-SEQUENCE STARS; ULTRADEEP PROJECT; STELLAR ROTATION; CORONAL ACTIVITY; FLANKING FIELDS; EMISSION; ACCRETION; PARAMETERS; DISKS AB We present a statistical analysis of simultaneous optical and X-ray light curves, spanning 600 ks, for 814 pre- main-sequence (PMS) stars in the Orion Nebula Cluster. The aim of this study is to establish the relationship, if any, between the sites of optical and X-ray variability and thereby to elucidate the origins of X-ray production in PMS stars. In a previous paper, we showed that optical and X-ray variability in PMS stars are very rarely time-correlated. Here, using time-averaged variability indicators to examine the joint occurrences of optical and X-ray variability, we confirm that the two forms of variability are not directly causally related. However, a strong and highly statistically significant correlation is found between optical variability and X-ray luminosity. As this correlation is found to be independent of accretion activity, we argue that X-ray production in PMS stars must instead be intimately connected with the presence and strength of optically variable, magnetically active surface regions (i.e., spots) on these stars. Moreover, because X-ray variability and optical variability are rarely time-correlated, we conclude that the sites of X-ray production are not exclusively cospatial with these regions. We argue that solar-analog coronae, heated by topologically complex fields, can explain these findings. C1 Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Stassun, KG (reprint author), Vanderbilt Univ, Dept Phys & Astron, 221 Kirkland Hall, Nashville, TN 37235 USA. EM keivan.stassun@vanderbilt.edu NR 34 TC 21 Z9 21 U1 1 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 MAY 1 PY 2007 VL 660 IS 1 BP 704 EP 711 DI 10.1086/513138 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162SB UT WOS:000246108700058 ER PT J AU Minniti, D Fernandez, JM Diaz, RF Udalski, A Pietrzynski, G Gieren, W Rojo, P Ruiz, MT Zoccali, M AF Minniti, Dante Fernandez, Jose Miguel Diaz, Rodrigo F. Udalski, Andrzej Pietrzynski, Grzegorz Gieren, Wolfgang Rojo, Patricio Ruiz, Maria Teresa Zoccali, Manuela TI Millimagnitude photometry for transiting extrasolar planetary candidates. III. accurate radius and period for OGLE-TR-111-B SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : individual (OGLE-TR-111) ID GIANT PLANETS; IMAGE SUBTRACTION; N2K CONSORTIUM; HOT SATURN; STARS; EXOPLANET AB We present accurate V-band photometry for a planetary transit of OGLE-TR-111 acquired with VIMOS at the ESO Very Large Telescope. The measurement of this transit allows us to refine the planetary radius, obtaining R-p 1.01 +/- 0.06 R-J. Given the mass of M-p 0.53 M-J previously measured from radial velocities, we confirm that the density is p(p) = 0.6 +/- 0.2 g cm(-3). We also revise the ephemeris for OGLE-TR-111-b, obtaining an accurate orbital period P = 4.014484 +/- 0.000014 days and predicting that the next observable transits would occur around December 2006, and after that only in mid-2008. Even though this period is different from previously published values, we cannot yet rule out a constant period. C1 Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Buenos Aires, Inst Astron & Fis Espacio, CONICET, Buenos Aires, DF, Argentina. Univ Warsaw Observ, PL-00748 Warsaw, Poland. Univ Concepcion, Dept Phys, Concepcion, Chile. Univ Chile, Dept Astron, Santiago, Chile. RP Minniti, D (reprint author), Pontificia Univ Catolica Chile, Dept Astron, Alameda 340, Santiago 22, Chile. EM dante@astro.puc.cl; jfernand@astro.puc.cl; rodrigo@iafe.uba.ar; udalski@astrouw.edu.pl; pietrzyn@hubble.cfm.udec.cl; wgieren@astro-udec.cl; mtruiz@das.uchile.cl; mzoccali@astro.puc.cl RI Diaz, Rodrigo/H-1487-2011; Rojo, Patricio/K-6732-2012; Rojo, Patricio/I-5765-2016; Ruiz, Maria Teresa/I-5770-2016; OI Rojo, Patricio/0000-0002-1607-6443; Ruiz, Maria Teresa/0000-0002-6799-1537; Diaz, Rodrigo/0000-0001-9289-5160 NR 31 TC 20 Z9 20 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2007 VL 660 IS 1 BP 858 EP 862 DI 10.1086/512722 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162SB UT WOS:000246108700072 ER PT J AU Davis, M Guhathakurta, P Konidaris, NP Newman, JA Ashby, MLN Biggs, AD Barmby, P Bundy, K Chapman, SC Coil, AL Conselice, CJ Cooper, MC Croton, DJ Eisenhardt, PRM Ellis, RS Faber, SM Fang, T Fazio, GG Georgakakis, A Gerke, BF Goss, WM Gwyn, S Harker, J Hopkins, AM Huang, JS Ivison, RJ Kassin, SA Kirby, EN Koekemoer, AM Koo, DC Laird, ES Le Floc'h, E Lin, L Lotz, JM Marshall, PJ Martin, DC Metevier, AJ Moustakas, LA Nandra, K Noeske, KG Papovich, C Phillips, AC Rich, RM Rieke, GH Rigopoulou, D Salim, S Schiminovich, D Simard, L Smail, I Small, TA Weiner, BJ Willmer, CNA Willner, SP Wilson, G Wright, EL Yan, R AF Davis, M. Guhathakurta, P. Konidaris, N. P. Newman, J. A. Ashby, M. L. N. Biggs, A. D. Barmby, P. Bundy, K. Chapman, S. C. Coil, A. L. Conselice, C. J. Cooper, M. C. Croton, D. J. Eisenhardt, P. R. M. Ellis, R. S. Faber, S. M. Fang, T. Fazio, G. G. Georgakakis, A. Gerke, B. F. Goss, W. M. Gwyn, S. Harker, J. Hopkins, A. M. Huang, J.-S. Ivison, R. J. Kassin, S. A. Kirby, E. N. Koekemoer, A. M. Koo, D. C. Laird, E. S. Le Floc'h, E. Lin, L. Lotz, J. M. Marshall, P. J. Martin, D. C. Metevier, A. J. Moustakas, L. A. Nandra, K. Noeske, K. G. Papovich, C. Phillips, A. C. Rich, R. M. Rieke, G. H. Rigopoulou, D. Salim, S. Schiminovich, D. Simard, L. Smail, I. Small, T. A. Weiner, B. J. Willmer, C. N. A. Willner, S. P. Wilson, G. Wright, E. L. Yan, R. TI The All-Wavelength Extended Groth Strip International Survey (AEGIS) data sets SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : photometry; infrared : galaxies; radio continuum : galaxies; surveys; ultraviolet : galaxies; X-rays : galaxies ID MULTIBAND IMAGING PHOTOMETER; FRANCE-HAWAII-TELESCOPE; ACTIVE GALACTIC NUCLEI; POINT-SOURCE CATALOGS; DEEP2 REDSHIFT SURVEY; STAR-FORMATION RATE; SPACE-TELESCOPE; SOURCE EXTRACTION; GALAXY EVOLUTION; WESTPHAL STRIP AB In this the first of a series of Letters, we present a panchromatic data set in the Extended Groth Strip region of the sky. Our survey, the All-Wavelength Extended Groth Strip International Survey (AEGIS), aims to study the physical properties and evolutionary processes of galaxies at. It includes the following deep, wide-field imaging data sets: z similar to 1 Chandra/ACIS X-ray, GALEX ultraviolet, CFHT/MegaCam Legacy Survey optical, CFHT/CFH12K optical, Hubble Space Telescope/ACS optical and NICMOS near-infrared, Palomar/WIRC near-infrared, Spitzer/IRAC mid-infrared, Spitzer/MIPS far-infrared, and VLA radio continuum. In addition, this region of the sky has been targeted for extensive spectroscopy using the Deep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck II 10 m telescope. Our survey is compared to other large multiwavelength surveys in terms of depth and sky coverage. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. Lawrence Berkeley Natl Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Royal Observ, United Kingdom Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NG9 2RD, England. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ London Imperial Coll Sci Technol & Med, London SW7 2BZ, England. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Columbia Univ, Dept Astron, New York, NY 10027 USA. Assoc Canadian Univ Res Astron, Herzberg Inst Astrophys, Natl Res Council, Victoria, BC V9E 2E7, Canada. Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Davis, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM mdavis@berkeley.edu RI Conselice, Christopher/B-4348-2013; Georgakakis, Antonis/K-4457-2013; Smail, Ian/M-5161-2013; Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011; OI Georgakakis, Antonis/0000-0002-3514-2442; Koekemoer, Anton/0000-0002-6610-2048; Smail, Ian/0000-0003-3037-257X; Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313; Conselice, Christopher/0000-0003-1949-7638; Weiner, Benjamin/0000-0001-6065-7483; Kirby, Evan/0000-0001-6196-5162; Moustakas, Leonidas/0000-0003-3030-2360 NR 60 TC 268 Z9 271 U1 3 U2 17 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 1 PY 2007 VL 660 IS 1 BP L1 EP L6 DI 10.1086/517931 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700001 ER PT J AU Gerke, BF Newman, JA Lotz, J Yan, RB Barmby, P Coil, AL Conselice, CJ Ivison, RJ Lin, LW Koo, DC Nandra, K Salim, S Small, T Weiner, BJ Cooper, MC Davis, M Faber, SM Guhathakurta, P AF Gerke, Brian F. Newman, Jeffrey A. Lotz, Jennifer Yan, Renbin Barmby, P. Coil, Alison L. Conselice, Christopher J. Ivison, R. J. Lin, Lihwai Koo, David C. Nandra, Kirpal Salim, Samir Small, Todd Weiner, Benjamin J. Cooper, Michael C. Davis, Marc Faber, S. M. Guhathakurta, Puragra TI The DEEP2 Galaxy Redshift Survey: AEGIS observations of a dual AGN at z=0.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei ID ACTIVE GALACTIC NUCLEI; BINARY BLACK-HOLE; EMISSION; QUASAR; KINEMATICS; SEYFERT; STELLAR; MERGERS; SYSTEM AB We present evidence of a dual active galactic nucleus (AGN) within an early-type galaxy at in the z = 0.709 extended Groth strip. The galaxy lies on the red sequence, with absolute magnitude M-B = -21.0 (AB, with h = 0.7) and rest-frame color U - B = 1.38. Its optical spectrum shows strong, double-peaked [O III] emission lines and weak H beta emission, with Seyfert-like line ratios. The two narrow peaks are separated by 630 km s(-1) in velocity and arise from two distinct regions, spatially resolved in the DEIMOS spectrum, with a projected physical separation of 1.2 kpc. HST ACS imaging shows an early-type (E/S0) galaxy with hints of disturbed structure, consistent with the remnant of a dissipationless merger. Multiwavelength photometric information from the AEGIS consortium confirms the identification of a dust-obscured AGN in an early-type galaxy, with detections in X-ray, optical, infrared, and radio wave bands. These data are most readily explained as a single galaxy harboring two AGNs-the first such system to be observed in an otherwise typical early-type galaxy. C1 Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NR9 2RD, England. Royal Observ, United Kingdom Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. Univ London Imperial Coll Sci & Technol, Astrophys Grp, London SW7 2BZ, England. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. CALTECH, Pasadena, CA 91125 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Gerke, BF (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM bgerke@berkeley.edu RI Conselice, Christopher/B-4348-2013; Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011; OI Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313; Conselice, Christopher/0000-0003-1949-7638; Weiner, Benjamin/0000-0001-6065-7483 NR 35 TC 40 Z9 40 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2007 VL 660 IS 1 BP L23 EP L26 DI 10.1086/517968 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700006 ER PT J AU Huang, JS Rigopoulou, D Papovich, C Ashby, MLN Willner, SP Ivison, R Laird, ES Webb, T Wilson, G Barmby, P Chapman, S Conselice, C McLeod, B Shu, CG Smith, HA Le Floc'h, E Egami, E Willmer, CAN Fazio, GG AF Huang, J.-S. Rigopoulou, D. Papovich, C. Ashby, M. L. N. Willner, S. P. Ivison, R. Laird, E. S. Webb, T. Wilson, G. Barmby, P. Chapman, S. Conselice, C. McLeod, B. Shu, C. G. Smith, H. A. Le Floc'h, E. Egami, E. Willmer, C. A. N. Fazio, G. G. TI AEGIS: Infrared spectroscopy of an infrared-luminous Lyman break galaxy at z=3.01 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : high-redshift; galaxies : starburst; infrared : galaxies ID SPITZER-SPACE-TELESCOPE; STAR-FORMATION; SUBMILLIMETER GALAXIES; ANTENNAE GALAXIES; SCUBA GALAXIES; REDSHIFT; SPECTROGRAPH; POPULATION; EMISSION; FEATURES AB We report the detection of rest-frame 6.2 and 7.7 mu m emission features arising from polycyclic aromatic hydrocarbons (PAHs) in the Spitzer IRS spectrum of an infrared-luminous Lyman break galaxy at. This z = 3.01 is currently the highest redshift galaxy where these PAH emission features have been detected. The total IR luminosity inferred from the MIPS 24 mu m and radio flux density is 2 x 10(13) L-circle dot, which qualifies this object as a so-called hyperluminous infrared galaxy (HyLIRG). However, unlike local HyLIRGs, which are generally associated with QSO/AGNs and have weak or absent PAH emission features, this HyLIRG has very strong 6.2 and 7.7 mu m PAH emission. We argue that intense star formation dominates the IR emission of this source, although we cannot rule out the presence of a deeply obscured AGN. This LBG appears to be a distorted system in the HST ACS F606W and F814W images, possibly indicating that a significant merger or interaction is driving the large IR luminosity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Nottingham, Dept Astron, Nottingham NG7 2RD, England. Shanghai Normal Univ, Joint Astrophys Ctr, Shanghai 200234, Peoples R China. Chinese Acad Sci, Shanghai Astron Observ, Shanghai 2000030, Peoples R China. RP Huang, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Conselice, Christopher/B-4348-2013; Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011; OI Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313; Conselice, Christopher/0000-0003-1949-7638 NR 29 TC 12 Z9 12 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2007 VL 660 IS 1 BP L69 EP L72 DI 10.1086/508567 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700017 ER PT J AU Ivison, RJ Chapman, SC Faber, SM Smail, I Biggs, AD Conselice, CJ Wilson, G Salim, S Huang, JS Willner, SP AF Ivison, R. J. Chapman, S. C. Faber, S. M. Smail, Ian Biggs, A. D. Conselice, C. J. Wilson, G. Salim, S. Huang, J.-S. Willner, S. P. TI AEGIS20: A radio survey of the Extended Groth Strip SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : formation ID LYMAN BREAK GALAXIES; POPULATION; EVOLUTION; GALEX; RED; SPITZER AB We describe AEGIS20-a radio survey of the Extended Groth Strip (EGS) conducted with the Very Large Array (VLA) at 1.4 GHz. The resulting catalog contains 1123 emitters and is sensitive to ultraluminous (10(12) L-circle dot) starbursts to z <= 1.3, well matched to the redshift range of the DEEP2 spectroscopic survey in this region. We use stacking techniques to explore the microjansky-level emission from a variety of galaxy populations selected via conventional criteria-Lyman break galaxies (LBGs), distant red galaxies (DRGs), UV-selected galaxies, and extremely red objects (EROs)-determining their properties as a function of color, magnitude, and redshift and their extinction-free contributions to the history of star formation. We confirm the familiar pattern that the star formation rate (SFR) density, rho(*), increases by at least a factor of similar to 5 from z = 0 to 1, although we note highly discrepant UV- and radio-based SFR estimates. Our radio-based SFRs become more difficult to interpret at z > 1 where correcting for contamination by radio-loud active galactic nuclei (AGNs) comes at the price of rejecting luminous starbursts. While stacking radio images is a useful technique, accurate radio-based SFRs for z >> 1 galaxies require precise redshifts and extraordinarily high fidelity radio data to identify and remove accretion-related emission. C1 UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ivison, RJ (reprint author), UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. RI Conselice, Christopher/B-4348-2013; Smail, Ian/M-5161-2013; Ivison, R./G-4450-2011; OI Smail, Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313; Conselice, Christopher/0000-0003-1949-7638 NR 26 TC 54 Z9 54 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 MAY 1 PY 2007 VL 660 IS 1 BP L77 EP L80 DI 10.1086/517917 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700019 ER PT J AU Konidaris, NP Guhathakurta, P Bundy, K Coil, AL Conselice, CJ Cooper, MC Eisenhardt, PRM Huang, JS Ivison, RJ Kassin, SA Kirby, EN Lotz, JM Newman, JA Noeske, KG Rich, RM Small, TA Willmer, CNA Willner, SP AF Konidaris, N. P. Guhathakurta, P. Bundy, K. Coil, A. L. Conselice, C. J. Cooper, M. C. Eisenhardt, P. R. M. Huang, J.-S. Ivison, R. J. Kassin, S. A. Kirby, E. N. Lotz, J. M. Newman, J. A. Noeske, K. G. Rich, R. M. Small, T. A. Willmer, C. N. A. Willner, S. P. TI AEGIS: Galaxy spectral energy distributions from the X-ray to radio SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : general; infrared : galaxies; radio continuum : galaxies; ultraviolet : galaxies; X-rays : galaxies ID REDSHIFT SURVEY; SEQUENCE AB The All-Wavelength Extended Groth Strip International Survey (AEGIS) team presents broadband spectral energy distributions (SEDs), from X-ray to radio wavelengths, for 71 galaxies spanning the redshift range 0.55-1.16 (< z >) similar to 0.7). Galaxies with secure redshifts are selected from a small (22 arcmin(2)) subsection of the Keck/AzS DEIMOS Galaxy Redshift Survey in the Extended Groth Strip field that has also been targeted for deep panchromatic imaging by ultraviolet (120-250 nm), optical (360-900 nm), optical/near-infrared (440-1600 nm), near-infrared (1200-2200 nm), mid/far-infrared (3.6-70 mu m), and radio (6-20 cm). A typical galaxy in our sample is M-B = -19.82. The ultraviolet to mid-infrared portion of their SEDs are found to be bracketed by two stellar-only model SEDs: (1) an early burst followed by passive evolution and (2) a constant star formation rate since early times. This suggests that few of these galaxies are undergoing major starbursts. Approximately half the galaxies show a mid-to far-infrared excess relative to the model SEDs, consistent with thermal emission from interstellar dust. Two objects have power-law SEDs, indicating that they are dominated by active galactic nuclei; both are detected in X-rays. SEDs, from the ultraviolet to the infrared, follow expected trends: redder SEDs are associated with red, early-type morphology, and low [O II] emission, and vice versa for blue SEDs. C1 Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NG9 2RD, England. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Royal Observ, Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Lawrence Berkeley Natl Lab, Inst Nucl Particle Astrophys, Berkeley, CA 94720 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. CALTECH, Pasadena, CA 91125 USA. RP Konidaris, NP (reprint author), Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. EM npk@ucolick.org; raja@ucolick.org; kbundy@astro.caltech.edu; acoil@as.arizona.edu; conselice@nottingham.ac.uk; cooper@astron.berkeley.edu; prme@kromos.jpl.nasa.gov; jhuang@cfa.harvard.edu; rji@roe.ac.uk; kassin@ucolick.org; ekirby@ucolick.org; lotz@noao.edu; janewman@lbl.gov; rmr@astro.ucla.edu; tas@astro.caltech.edu; cnaw@as.arizona.edu; swillner@cfa.harvard.edu RI Conselice, Christopher/B-4348-2013; Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Conselice, Christopher/0000-0003-1949-7638; Kirby, Evan/0000-0001-6196-5162 NR 14 TC 5 Z9 5 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 1 PY 2007 VL 660 IS 1 BP L7 EP L10 DI 10.1086/517929 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700002 ER PT J AU Le Floc'h, E Willmer, CNA Noeske, K Konidaris, NP Laird, ES Koo, DC Nandra, K Bundy, K Salim, S Maiolino, R Conselice, CJ Lotz, JM Papovich, C Smith, JD Bai, L Coil, AL Barmby, P Ashby, MLN Huang, JS Blaylock, M Rieke, G Newman, JA Ivison, R Chapman, S Dole, H Egami, E Elbaz, D AF Le Floc'h, E. Willmer, C. N. A. Noeske, K. Konidaris, N. P. Laird, E. S. Koo, D. C. Nandra, K. Bundy, K. Salim, S. Maiolino, R. Conselice, C. J. Lotz, J. M. Papovich, C. Smith, J. D. Bai, L. Coil, A. L. Barmby, P. Ashby, M. L. N. Huang, J.-S. Blaylock, M. Rieke, G. Newman, J. A. Ivison, R. Chapman, S. Dole, H. Egami, E. Elbaz, D. TI Far-infrared characterization of an ultraluminous starburst associated with a massively accreting black hole at z=1.15 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : high-redshift; infrared : galaxies ID ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; DEEP SUBMILLIMETER SURVEY; FRANCE REDSHIFT SURVEY; 14 HOUR FIELD; X-RAY SOURCES; GROTH STRIP; SPECTROGRAPH IRS; HIGH-RESOLUTION; SCUBA GALAXIES AB As part of the All-Wavelength Extended Groth Strip International Survey (AEGIS), we describe the panchromatic characterization of an X-ray-luminous active galactic nucleus (AGN) in a merging galaxy at z = 1.15. This object is detected at infrared (8, 24, 70, and 160 mu m), submillimeter (850 mu m), and radio wavelengths, from which we derive a bolometric luminosity L-bol similar to 9 x 10(12) L-circle dot. We find that the AGN clearly dominates the hot dust emission below 40 mu m but its total energetic power inferred from the hard X-rays is substantially less than the bolometric output of the system. About 50% of the infrared luminosity is indeed produced by a cold dust component that probably originates from enshrouded star formation in the host galaxy. In the context of a coeval growth of stellar bulges and massive black holes, this source might represent a "transition" object, sharing properties with both quasars and luminous starbursts. Study of such composite galaxies will help address how the star formation and disk-accretion phenomena may have regulated each other at high redshift and how this coordination may have participated in the buildup of the relationship observed locally between the masses of black holes and stellar spheroids. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Observ Meudon, Paris, France. Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. Univ London Imperial Coll Sci & Technol, Astrophys Grp, London SW7 2AW, England. CALTECH, Pasadena, CA 91125 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. INAF, I-00044 Frascati, Italy. Univ Nottingham, Sch Phys & Astron, Nottingham NG9 2RD, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lawrence Berkeley Natl Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Royal Observ, Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. Inst Astrophys Spatiale, F-91405 Orsay, France. CEA, Serv Astrophys, F-91191 Gif Sur Yvette, France. RP Le Floc'h, E (reprint author), Univ Hawaii, Honolulu, HI 96822 USA. RI Conselice, Christopher/B-4348-2013; Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011; OI Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313; Conselice, Christopher/0000-0003-1949-7638 NR 48 TC 26 Z9 26 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 1 PY 2007 VL 660 IS 1 BP L65 EP L68 DI 10.1086/517916 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700016 ER PT J AU Lin, LW Koo, DC Weiner, BJ Chiueh, T Coil, AL Lotz, J Conselice, CJ Willner, SP Smith, HA Guhathakurta, P Huang, JS Le Floc'h, E Noeske, KG Willmer, CNA Cooper, MC Phillips, AC AF Lin, Lihwai Koo, David C. Weiner, Benjamin J. Chiueh, Tzihong Coil, Alison L. Lotz, Jennifer Conselice, Christopher J. Willner, S. P. Smith, H. A. Guhathakurta, Puragra Huang, J.-S. Le Floc'h, Emeric Noeske, Kai G. Willmer, Christopher N. A. Cooper, Michael C. Phillips, Andrew C. TI AEGIS: Enhancement of dust-enshrouded star formation in close galaxy pairs and merging galaxies up to z similar to 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : interactions; infrared : galaxies; large-scale structure of universe ID ULTRALUMINOUS INFRARED GALAXIES; REDSHIFT SURVEY; MORPHOLOGICAL CLASSIFICATION; INTERACTING GALAXIES; FORMATION RATES; FIELD GALAXIES; MERGER RATE; EVOLUTION; LUMINOSITY; HISTORY AB Using data from the DEEP2 Galaxy Redshift Survey and HST/ACS imaging in the Extended Groth Strip, we select nearly 100 interacting galaxy systems, including kinematic close pairs and morphologically identified merging galaxies. Spitzer MIPS 24 mu m fluxes of these systems reflect the current dusty star formation activity, and at a fixed stellar mass (M-*) the median infrared luminosity (L-IR) among merging galaxies and close pairs of blue galaxies is twice (1.9 +/- 0.4) that of control pairs drawn from isolated blue galaxies. Enhancement declines with galaxy separation, being strongest in close pairs and mergers and weaker in wide pairs compared to the control sample. At (z) over bar similar to 0.9, 7.1% +/- 4.3% of massive interacting galaxies (M-* > 2 x 10(10) M-circle dot) are found to be ULIRGs, compared to 2.6% +/- 0.7% in the control sample. The large spread of L-IR/M-* among interacting galaxies suggests that this enhancement may depend on the merger stage as well as other as yet unidentified factors (e.g., galaxy structure, mass ratio, orbital characteristics, presence of AGN or bar). The contribution of interacting systems to the total IR luminosity density is moderate (less than or similar to 36%). C1 Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. Univ Calif Santa Cruz, Lick Observ, UCO, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Lin, LW (reprint author), Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. EM d90222005@ntu.edu.tw RI Conselice, Christopher/B-4348-2013; OI CHIUEH, TZI-HONG/0000-0003-2654-8763; Weiner, Benjamin/0000-0001-6065-7483 NR 37 TC 70 Z9 70 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 1 PY 2007 VL 660 IS 1 BP L51 EP L54 DI 10.1086/517919 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700013 ER PT J AU Noeske, KG Weiner, BJ Faber, SM Papovich, C Koo, DC Somerville, RS Bundy, K Conselice, CJ Newman, JA Schiminovich, D Le Floc'h, E Coil, AL Rieke, GH Lotz, JM Primack, JR Barmby, P Cooper, MC Davis, M Ellis, RS Fazio, GG Guhathakurta, P Huang, J Kassin, SA Martin, DC Phillips, AC Rich, RM Small, TA Willmer, CNA Wilson, G AF Noeske, K. G. Weiner, B. J. Faber, S. M. Papovich, C. Koo, D. C. Somerville, R. S. Bundy, K. Conselice, C. J. Newman, J. A. Schiminovich, D. Le Floc'h, E. Coil, A. L. Rieke, G. H. Lotz, J. M. Primack, J. R. Barmby, P. Cooper, M. C. Davis, M. Ellis, R. S. Fazio, G. G. Guhathakurta, P. Huang, J. Kassin, S. A. Martin, D. C. Phillips, A. C. Rich, R. M. Small, T. A. Willmer, C. N. A. Wilson, G. TI Star formation in AEGIS field galaxies since z=1.1: The dominance of gradually declining star formation, and the main sequence of star-forming galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : high-redshift; galaxies : starburst ID DEEP-FIELD; FORMATION HISTORIES; FORMATION RATES; HIGH-REDSHIFT; STELLAR MASS; SPITZER VIEW; EVOLUTION; UNIVERSE; Z-SIMILAR-TO-1; SIMULATIONS AB We analyze star formation (SF) as a function of stellar mass (M-*) and redshift z in the All-Wavelength Extended M * Groth Strip International Survey. For 2905 field galaxies, complete to 10(10)(10(10.8)) M-circle dot at z < 0.7( 1), spectroscopic redshifts out to z = 1.1, we compile SF rates (SFRs) from emission lines, GALEX, and Spitzer MIPS 24 mu m photometry, optical-NIR M-* measurements, and HST morphologies. Galaxies with reliable signs of SF form a distinct "main sequence" (MS), with a limited range of SFRs at a given M-* and z (1 sigma less than or similar to +/- 0.3 dex), and log (SFR) approximately proportional to log M-*. The range of log (SFR) remains constant to z > 1, while the MS as a whole moves to higher SFR as z increases. The range of the SFR along the MS constrains the amplitude of episodic variations of SF and the effect of mergers on the SFR. Typical galaxies spend similar to 67%( 95%) of their lifetime since z = 1 within a factor of less than or similar to 2(4) of their average SFR at a given M-* and z. The dominant mode of the evolution z similar to 1 is apparently a gradual decline of the average SFR in most individual galaxies, not a decreasing frequency of starburst episodes, or a decreasing factor by which SFRs are enhanced in starbursts. LIRGs at z similar to 1 seem to mostly reflect the high SFR typical for massive galaxies at that epoch. The smooth MS may reflect that the same set of few physical processes governs SF prior to additional quenching processes. A gradual process like gas exhaustion may play a dominant role. C1 Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CALTECH, Pasadena, CA 91125 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NG9 2RD, England. Lawrence Berkeley Natl Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Noeske, KG (reprint author), Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. RI Conselice, Christopher/B-4348-2013; Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Conselice, Christopher/0000-0003-1949-7638; Weiner, Benjamin/0000-0001-6065-7483 NR 40 TC 725 Z9 727 U1 1 U2 12 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 2007 VL 660 IS 1 BP L43 EP L46 DI 10.1086/517926 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700011 ER PT J AU Pierce, CM Lotz, JM Laird, ES Lin, L Nandra, K Primack, JR Faber, SM Barmby, P Park, SQ Willner, SP Gwyn, S Koo, DC Coil, AL Cooper, MC Georgakakis, A Koekemoer, AM Noeske, KG Weiner, BJ Willmer, CNA AF Pierce, C. M. Lotz, J. M. Laird, E. S. Lin, L. Nandra, K. Primack, J. R. Faber, S. M. Barmby, P. Park, S. Q. Willner, S. P. Gwyn, S. Koo, D. C. Coil, A. L. Cooper, M. C. Georgakakis, A. Koekemoer, A. M. Noeske, K. G. Weiner, B. J. Willmer, C. N. A. TI Aegis: Host galaxy morphologies of X-ray-selected and infrared-selected active galactic nuclei at 0.2 <= z < 1.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : interactions; galaxies : nuclei; infrared : galaxies; X-rays : galaxies ID EXTENDED GROTH STRIP; DEEP CHANDRA SURVEY; REDSHIFT SURVEY; SPACE-TELESCOPE; BLACK-HOLES; FIELD-SOUTH; EVOLUTION; PAIRS; DISTRIBUTIONS; QUASARS AB We visually and quantitatively determine the host galaxy morphologies of 94 intermediate-redshift (0.2 <= z < 2) active galactic nuclei (AGNs), selected using Chandra X-ray data and Spitzer mid-infrared data in the Extended Groth Strip. Using recently developed morphology measures, the second-order moment of the brightest 20% of a galaxy's flux (M(20)) and the Gini coefficient, we find that X-ray-selected AGNs mostly reside in E/S0/Sa galaxies (53(-10)(+11)%), while IR-selected AGNs show no clear preference for host morphology. X-ray-selected AGN hosts are members of close pairs more often than the field population by a factor of, but most 3.3 +/- 1.4 of these pair members appear to be undisturbed early-type galaxies and do not tend to show direct evidence of gravitational perturbations or interactions. Thus, the activation mechanism for AGN activity remains unknown, even for pair members. C1 Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AW, England. Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Pierce, CM (reprint author), Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. EM cpierce@physics.ucsc.edu; lotz@noao.edu; eslaird@ucolick.org; lihwai@ucolick.org; k.nandra@imperial.ac.uk; joel@scipp.ucsc.edu; faber@ucolick.org; pbarmby@cfa.harvard.edu; spark@cfa.harvard.edu; willner@cfa.harvard.edu; gwyn@beluga.phys.uvic.ca; koo@ucolick.org; acoil@as.arizona.edu; cooper@astro.berkeley.edu; a.georgakakis@imperial.ac.uk; koekemoe@stsci.edu; kai@ucolick.org; bjw@ucolick.org; cnaw@as.arizona.edu RI Georgakakis, Antonis/K-4457-2013; Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 27 TC 76 Z9 76 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2007 VL 660 IS 1 BP L19 EP L22 DI 10.1086/517922 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700005 ER PT J AU Symeonidis, M Rigopoulou, D Huang, JS Davis, M Ashby, MLN Barmby, P Egami, E Fazio, GG Le Floc'h, E Rieke, G Willner, SP Wilson, G AF Symeonidis, M. Rigopoulou, D. Huang, J.-S. Davis, M. Ashby, M. L. N. Barmby, P. Egami, E. Fazio, G. G. Le Floc'h, E. Rieke, G. Willner, S. P. Wilson, G. TI AEGIS: Infrared spectral energy distributions of MIPS 70 mu m-selected sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : fundamental parameters; galaxies : high-redshift; infrared : galaxies ID SPITZER-SPACE-TELESCOPE; LOCKMAN HOLE; GALAXIES; EMISSION; RADIO AB We present 0.5-160 mu m spectral energy distributions (SEDs) of galaxies, detected at 70 mu m with the Multiband Imaging Photometer for Spitzer (MIPS), using broadband imaging data from Spitzer and ground-based telescopes. Spectroscopic redshifts, in the range 0.2 <= z <= 1.5, have been measured as part of the Deep Extragalactic Evolutionary Probe 2 (DEEP2) project. On the basis of the SEDs, we explore the nature and physical properties of the sources. Using the optical spectra, we derive H beta and [O II]-based star formation rates (SFRs) that are 10-100 times lower than SFR estimates based on IR and radio. The median offset in SFR between optical and IR is reduced by a factor of similar to 3 when we apply a typical extinction correction. We investigate mid-to far-infrared correlations for low-redshift (>0.5) and high-redshift (0.5 < z < 1.2) bins. Using this unique "far-infrared"-selected sample, we derive an empirical mid-to far-infrared relationship that can be used to estimate the infrared energy budget of galaxies in the high-redshift universe. Our sample can be used as a template to translate far-infrared luminosities into bolometric luminosities for high-redshift objects. C1 Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Symeonidis, M (reprint author), Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 24 TC 7 Z9 7 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 MAY 1 PY 2007 VL 660 IS 1 BP L73 EP L76 DI 10.1086/517928 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700018 ER PT J AU Wilson, G Huang, JS Fazio, GG Yan, R Koekemoer, AM Salim, S Faber, SM Lotz, J Willmer, CNA Davis, M Coil, AL Newman, JA Conselice, CJ Papovich, C Ashby, MLN Barmby, P Willner, SP Ivison, R Miyazaki, S Rigopoulou, D AF Wilson, G. Huang, J.-S. Fazio, G. G. Yan, R. Koekemoer, A. M. Salim, S. Faber, S. M. Lotz, J. Willmer, C. N. A. Davis, M. Coil, A. L. Newman, J. A. Conselice, C. J. Papovich, C. Ashby, M. L. N. Barmby, P. Willner, S. P. Ivison, R. Miyazaki, S. Rigopoulou, D. TI AEGIS: A panchromatic study of IRAC-selected extremely red objects with confirmed spectroscopic redshifts SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : high-redshift; galaxies : starburst; infrared : galaxies ID SPITZER-SPACE-TELESCOPE; LYMAN BREAK GALAXIES; ARRAY CAMERA IRAC; MIDINFRARED PROPERTIES; LOCKMAN HOLE; GROTH STRIP; POPULATION; NUCLEI AB We study 87 extremely red objects (EROs), selected both to have color redder than and to R - [3.6] = 4.0 have confirmed spectroscopic redshifts. Together, these two constraints result in this sample populating a fairly narrow redshift range at. The key new ingredient included here is deep Spitzer Space Telescope 0.76 < z < 1.42 Infrared Array Camera (IRAC) data. Based on color, we demonstrate that it is possible to classify [3.6] - [8.0] EROs as early-type galaxies, dusty starburst galaxies, or active galactic nuclei (AGNs; power-law types). We present ultraviolet-to-mid-infrared spectral energy distributions (SEDs) and Advanced Camera for Surveys (ACS) images, both of which support our simple IRAC color classification. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Lawrence Berkeley Natl Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94700 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. Royal Observ, Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. RP Wilson, G (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM gillian@ipac.caltech.edu RI Conselice, Christopher/B-4348-2013; Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011; OI Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313; Conselice, Christopher/0000-0003-1949-7638; Koekemoer, Anton/0000-0002-6610-2048 NR 29 TC 15 Z9 16 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2007 VL 660 IS 1 BP L59 EP L63 DI 10.1086/517923 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162TP UT WOS:000246112700015 ER PT J AU Smith, AR Wcislo, WT O'Donnell, S AF Smith, Adam R. Wcislo, William T. O'Donnell, Sean TI Survival and productivity benefits to social nesting in the sweat bee Megalopta genalis (Hymenoptera : Halictidae) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE per capita productivity; social flexibility; assured fitness returns; ecological constraints; Halictidae; augochlorini ID PRIMITIVELY EUSOCIAL BEE; ALLODAPINE BEE; RUBICUNDUS HYMENOPTERA; ECUADORIA HYMENOPTERA; SEX ALLOCATION; HOVER WASPS; COLONY SIZE; PAPER WASP; EVOLUTION; BEHAVIOR AB Facultatively solitary and eusocial species allow for direct tests of the benefits of group living. We used the facultatively social sweat bee Megalopta genalis to test several benefits of group living. We surveyed natural nests modified for observation in the field weekly for 5 weeks in 2003. First, we demonstrate that social and solitary nesting are alternative behaviors, rather than different points on one developmental trajectory. Next, we show that solitary nests suffered significantly higher rates of nest failure than did social nests. Nest failure apparently resulted from solitary foundress mortality and subsequent brood orphanage. Social nests had significantly higher productivity, measured as new brood cells provisioned during the study, than did solitary nests. After accounting for nest failures, per capita productivity did not change with group size. Our results support key predictions of Assured Fitness Return models, suggesting such indirect fitness benefits favor eusocial nesting in M. genalis. We compared field collections of natural nests to our observation nest data to show that without accounting for nest failures, M. genalis appear to suffer a per capita productivity decrease with increasing group size. Calculating per capita productivity from collected nests without accounting for the differential probabilities of survival across group sizes leads to an overestimate of solitary nest productivity. C1 Smithsonian Trop Res Inst, Miami, FL 34002 USA. Univ Washington, Dept Psychol, Anim Behav Area, Seattle, WA 98195 USA. RP Smith, AR (reprint author), Smithsonian Trop Res Inst, Unit 0948,APO,AA, Miami, FL 34002 USA. EM smithad@si.edu NR 59 TC 37 Z9 37 U1 2 U2 16 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 MAY PY 2007 VL 61 IS 7 BP 1111 EP 1120 DI 10.1007/s00265-006-0344-4 PG 10 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 154PM UT WOS:000245519700014 ER PT J AU Wright, SJ Stoner, KE Beckman, N Corlett, RT Dirzo, R Muller-Landau, HC Nunez-Iturri, G Peres, CA Wang, BC AF Wright, S. Joseph Stoner, Kathryn E. Beckman, Noelle Corlett, Richard T. Dirzo, Rodolfo Muller-Landau, Helene C. Nunez-Iturri, Gabriela Peres, Carlos A. Wang, Benjamin C. TI The plight of large animals in tropical forests and the consequences for plant regeneration SO BIOTROPICA LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and-Conservation CY 2005 CL Uberlandia, BRAZIL SP Canadian Assoc Phys Anthropol DE bushmeat; hunting; mammals; poaching; plant diversity; seed dispersal; seed predation; seed survival; seedling survival AB We introduce a special section that addresses the bushmeat or wild meat crisis, its direct impact on game species, and its indirect impact on plants in tropical forests. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Nacl Autonoma Mexico, Ctr Invest Ecosist, Morelia 58189, Michoacan, Mexico. Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. Univ Hong Kong, Dept Ecol & Biodivers, Hong Kong, Hong Kong, Peoples R China. Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. Univ Illinois, Dept Biol Sci, Chicago, IL 60607 USA. Univ E Anglia, Sch Environm Sci, Ctr Ecol Evolut & Conservat, Norwich NR4 7TJ, Norfolk, England. Univ Calif Los Angeles, Dept Ecol & Evolut Biol, Los Angeles, CA 90095 USA. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM wrightj@si.edu RI Beckman, Noelle/E-5554-2011; Corlett, Richard/G-1251-2011; Peres, Carlos/B-1276-2013; Wright, Stuart/M-3311-2013; Stoner, Kathryn/E-1510-2015; OI Beckman, Noelle/0000-0001-5822-0610; Peres, Carlos/0000-0002-1588-8765; Wright, Stuart/0000-0003-4260-5676; Stoner, Kathryn/0000-0002-9964-1697; Corlett, Richard/0000-0002-2508-9465 NR 14 TC 93 Z9 96 U1 7 U2 41 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2007 VL 39 IS 3 BP 289 EP 291 DI 10.1111/j.1744-7429.2007.00293.x PG 3 WC Ecology SC Environmental Sciences & Ecology GA 160KM UT WOS:000245939300001 ER PT J AU Wright, SJ Hernandez, A Condit, R AF Wright, S. Joseph Hernandez, Andres Condit, Richard TI The bushmeat harvest alters seedling banks by favoring lianas, large seeds, and seeds dispersed by bats, birds, and wind SO BIOTROPICA LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and-Conservation CY 2005 CL Uberlandia, BRAZIL SP Canadian Assoc Phys Anthropol DE anthropogenic disturbance; Barro Colorado Island; poachers; seed dispersal; tropical forest ID TROPICAL FORESTS; TREES; FRAGMENTATION; RECRUITMENT; COMMUNITY; DIVERSITY; SURVIVAL; POACHERS; TRAITS; PANAMA AB We evaluated predictions that hunters favor lianas, large seeds, and seeds dispersed by bats, small birds, and mechanical means for seedling banks in central Panama. We censused 3201 trees in 20 1-ha plots and 38,250 seedlings in the central 64 m(2) of each plot. We found significant differences in the species composition of the seedling bank between nine protected sites in the Barro Colorado Nature Monument and 11 hunted sites in the contiguous Parque Nacional Soberania. Lianas, species with large seeds, and species with seeds dispersed by bats, small birds, and mechanical means were all overrepresented at hunted sites. The latter two findings could also be evaluated relative to the species composition of reproductively mature adults for canopy trees. The tree species present in the seedling bank had significantly heavier seeds than the tree species present as adults at hunted sites but not at protected sites. The representation of seed dispersal modes among the species present in the seedling bank did not reflect pre-existing differences in the local species composition of adults. We hypothesize that hunting large seed predators favors large seeds by reducing predation and increasing survival. We also hypothesize that the harvest of large birds and mammals that disperse many seeds favors other species whose seeds are dispersed by bats, small birds, and mechanical means. This process also favors lianas because the seeds of disproportionate numbers of liana species are dispersed by wind. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 36 TC 109 Z9 113 U1 4 U2 37 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2007 VL 39 IS 3 BP 363 EP 371 DI 10.1111/j.1744-7429.2007.00289.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 160KM UT WOS:000245939300009 ER PT J AU Stoner, KE Vulinec, K Wright, SJ Peres, CA AF Stoner, Kathryn E. Vulinec, Kevina Wright, S. Joseph Peres, Carlos A. TI Hunting and plant community dynamics in tropical forests: A synthesis and future directions SO BIOTROPICA LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and-Conservation CY 2005 CL Uberlandia, BRAZIL SP Canadian Assoc Phys Anthropol DE bushmeat; management plans; plant community structure; seed dispersal; seed predation ID DUNG BEETLE COMMUNITIES; SEED DISPERSAL; COSTA-RICA; WILDLIFE CONSERVATION; AMAZONIAN FORESTS; RAIN-FOREST; SURVIVAL; FRAGMENTATION; PRIMATE; MAMMALS AB This synthesis builds on the preceding articles of this Special Section and has three goals. We first review the nascent literature that addresses indirect effects of hunting for tropical forest plant communities. Next, we highlight the potential indirect effects of hunting for other groups of organisms. Our final goal is to consider what could be done to ameliorate the demographic threats to harvest-sensitive game species caused by unsustainable hunting. Three conclusions are possible at this time concerning the impact of hunting for tropical forest plant communities: (1) Hunting tends to reduce seed movement for animal-dispersed species with very large diaspores; (2) Hunting reduces seed predation by granivorous vertebrates for species with large seeds; and (3) Hunting alters the species composition of the seedling and sapling layers. The cascading effects of hunting are already known to affect bruchid beetles and dung beetles and are likely to affect other, nongame taxa. To ameliorate these problems, several lines of research should be further explored to facilitate the development of game management plans including: (1) alternative use of sources of animal protein; (2) income supplementation for local people from sources other than wild meat; (3) outreach and extension activities for communities; (4) recognition and facilitation of the shifting of attitudes towards hunting; (5) implementation of community-based wildlife management programs in regulated-use areas such as extractive reserves; and (6) landscape-scale conservation planning that maximizes the source-sink dynamics of harvested and unharvested game populations and enforces game regulations in strictly protected areas. C1 Univ Nacl Autonoma Mexico, Ctr Invest Ecosist, Morelia 58189, Michoacan, Mexico. Delaware State Univ, Dept Agr & Nat Resources, Dover, DE 19901 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ E Anglia, Sch Environm Sci, Ctr Ecol Evolut & Conservat, Norwich NR4 7TJ, Norfolk, England. RP Stoner, KE (reprint author), Univ Nacl Autonoma Mexico, Ctr Invest Ecosist, Apartado Postal 27-3, Morelia 58189, Michoacan, Mexico. EM kstoner@oikos.unam.mx RI Peres, Carlos/B-1276-2013; Gardner, Toby/B-7516-2008; Wright, Stuart/M-3311-2013; Stoner, Kathryn/E-1510-2015 OI Peres, Carlos/0000-0002-1588-8765; Wright, Stuart/0000-0003-4260-5676; Stoner, Kathryn/0000-0002-9964-1697 NR 65 TC 77 Z9 84 U1 7 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD MAY PY 2007 VL 39 IS 3 BP 385 EP 392 DI 10.1111/j.1744-7429.2007.00291.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 160KM UT WOS:000245939300011 ER PT J AU Avalos, G Mulkey, SS Kitajima, K Wright, SJ AF Avalos, Gerardo Mulkey, Stephen S. Kitajima, Kaoru Wright, S. Joseph TI Colonization strategies of two liana species in a tropical dry forest canopy SO BIOTROPICA LA English DT Article DE Bonamia trichantha; Combretum fruticosum; light acclimation; Panama ID RAIN-FOREST; LEAF AGE; PHOTOSYNTHETIC CAPACITY; CARBON GAIN; TREES; ACCLIMATION; DYNAMICS; DECLINE; GROWTH; PANAMA AB Lianas impose intense resource competition for light in the upper forest canopy by displaying dense foliage on top of tree crowns. Using repeated access with a construction crane, we studied the patterns of canopy colonization of the lianas Combretum fruticosum and Bonamia trichantha in a Neotropical dry forest in Panama. Combretum fruticosum flushed leaves just before the rainy season, and its standing leaf area quickly reached a peak in the early rainy season (May-June). In contrast, B. trichantha built up foliage area continuously throughout the rainy season and reached a peak in the late rainy season (November). Both species displayed the majority of leaves in full sun on the canopy surface, but C. fruticosum displayed a greater proportion of leaves (26%) in more shaded microsites than B. trichantha (12%). Self-shading within patches of liana leaves within the uppermost 40-50 cm of the canopy reduced light levels measured with photodiodes placed directly on leaves to 4-9 percent of light levels received by sun leaves. Many leaves of C. fruticosum acclimated to shade within a month following the strongly synchronized leaf flushing and persisted in deep shade. In contrast, B. trichantha produced short-lived leaves opportunistically in the sunniest locations. Species differences in degree of shade acclimation were also evident in terms of structural (leaf mass per area, and leaf toughness) and physiological characters (nitrogen content, leaf life span, and light compensation point). Contrasting leaf phenologies reflect differences in light exploitation and canopy colonization strategies of these two liana species. C1 Sch Field Studies, Ctr Sustainable Dev Studies, Salem, MA 01970 USA. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Avalos, G (reprint author), Sch Field Studies, Ctr Sustainable Dev Studies, 10 Fed St, Salem, MA 01970 USA. EM avalos@fieldstudies.org RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 35 TC 14 Z9 16 U1 1 U2 7 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2007 VL 39 IS 3 BP 393 EP 399 DI 10.1111/j.1744-7429.2007.00265.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 160KM UT WOS:000245939300012 ER PT J AU Dietz, M Kalko, EKV AF Dietz, M. Kalko, E. K. V. TI Reproduction affects flight activity in female and male Daubenton's bats, Myotis daubentoni SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID FORAGING BEHAVIOR; EPTESICUS-FUSCUS; FEEDING ECOLOGY; INSECTIVOROUS BAT; BODY-TEMPERATURE; GLEANING BAT; DAILY TORPOR; HABITAT USE; BROWN BAT; CHIROPTERA AB Nearly all mammals in the temperate zone breed in spring and summer when climatic conditions are favourable and food is abundant. Similar to other mammals, food requirements of female bats are particularly high during pregnancy and lactation and of males during spermatogenesis. Seasonal changes in energy demand and reproductive condition should therefore result in different foraging activity within and between sexes. This assumption was tested on 16 adult females and 13 adult males of the Palaearctic Daubenton's bat, Myotis daubentoni (Kuhl, 1817), that were radio-tracked during pregnancy, lactation, and post-lactation periods. Pregnant females, as hypothesized, flew significantly longer (mean: 358.9 min; 70% of the night length) than males (mean: 228.5 min; 42.4% of the night length) during spring. In contrast, nightly flight time of lactating females decreased and was significantly less than that of pregnant females, but was similar to that of males during the same period. The longest flight times of males were registered during late summer when spermatogenetic activity is high. However, there were distinct differences in the use of foraging areas between female and male Daubenton's bats. Female bats used small, individual foraging areas during pregnancy and lactation. The pattern was reversed in females after the young had been weaned and in males after they entered spermatogenesis. Overall, the results confirmed Our proposition that flight activity reflects the higher energy demand and nutrition requirements in the different reproductive periods. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Kalko, EKV (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM Elisabeth.Kalko@uni-ulm.de NR 64 TC 20 Z9 21 U1 0 U2 11 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD MAY PY 2007 VL 85 IS 5 BP 653 EP 664 DI 10.1139/Z07-045 PG 12 WC Zoology SC Zoology GA 192SP UT WOS:000248223600008 ER PT J AU Ordonez, C Troeng, S Meylan, A Meylan, P Ruiz, A AF Ordonez, Cristina Troeng, Sebastian Meylan, Anne Meylan, Peter Ruiz, Argelis TI Chiriqui Beach, Panama, the most important leatherback nesting beach in Central America SO CHELONIAN CONSERVATION AND BIOLOGY LA English DT Article AB Chiriqui Beach, in the Comarca Ngobe-Bugle on the Caribbean coast of Panama, is the most important nesting beach for leatherback turtles (Dermochelys coriacea) in Caribbean Central America. Beach surveys during the 2003 and 2004 nesting seasons documented 3077 leatherback nests in one season and a minimum of 234 individual leatherbacks. Monitoring of nest fate revealed that predation by dogs represents the greatest human-related survival threat to leatherbacks at Chiriqui Beach, although the killing of leatherbacks from the same nesting population on beaches near the Panama-Costa Rica border also is of concern. C1 Caribbean Conservat Corp, San Pedro, Costa Rica. Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. Eckerd Coll, St Petersburg, FL 33711 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Ordonez, C (reprint author), Caribbean Conservat Corp, Apdo Postal 246-2050, San Pedro, Costa Rica. EM cristinao@cccturtle.org; s.troeng@conservation.org; anne.meylan@lnyfwc.com; meylanpa@eckerd.edu NR 8 TC 13 Z9 15 U1 1 U2 2 PU CHELONIAN RESEARCH FOUNDATION PI LUNENBURG PA 168 GOODRICH ST., LUNENBURG, MA USA SN 1071-8443 J9 CHELONIAN CONSERV BI JI Chelonian Conserv. Biol. PD MAY PY 2007 VL 6 IS 1 BP 122 EP 126 DI 10.2744/1071-8443(2007)6[122:CBPTMI]2.0.CO;2 PG 5 WC Zoology SC Zoology GA 177OI UT WOS:000247162000015 ER PT J AU Stover, DB Day, FP Butnor, JR Drake, BG AF Stover, Daniel B. Day, Frank P. Butnor, John R. Drake, Bert G. TI Effect of elevated Co-2 on coarse-root biomass in Florida scrub detected by ground-penetrating radar SO ECOLOGY LA English DT Article DE carbon dioxide; coarse-root biomass; ground-penetrating radar; roots; scrub oak ID ATMOSPHERIC CO2; FINE ROOTS; CARBON-DIOXIDE; OAK ECOSYSTEM; SYSTEMS; RESPONSES; FOREST; FIELD; SOIL AB Growth and distribution of coarse roots in time and space represent a gap in our understanding of belowground ecology. Large roots may play a critical role in carbon sequestration belowground. Using ground-penetrating radar (GPR), we quantified coarseroot biomass from an open-top chamber experiment in a scrub-oak ecosystem at Kennedy Space Center, Florida, USA. GPR propagates electromagnetic waves directly into the soil and reflects a portion of the energy when a buried object is contacted. In our study, we utilized a 1500 MHz antenna to establish correlations between GPR signals and root biomass. A significant relationship was found between GPR signal reflectance and biomass (R-2 = 0.68). This correlation was applied to multiple GPR scans taken from each open-top chamber (elevated and ambient C0(2)). Our results showed that plots receiving elevated C02 had significantly (P = 0.049) greater coarse-root biomass compared to ambient plots, suggesting that coarse roots may play a large role in carbon sequestration in scrub-Oak ecosystems. This nondestructive method holds much promise for rapid and repeatable quantification of coarse roots, which are currently the most elusive aspect of long-term belowground studies. C1 Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. US Forest Serv, So Res Stn, Res Triangle Pk, NC 27709 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Stover, DB (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. EM dstover@odu.edu RI Butnor, John/P-9738-2016 NR 46 TC 59 Z9 63 U1 1 U2 17 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 MAY PY 2007 VL 88 IS 5 BP 1328 EP 1334 DI 10.1890/06-0989 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 166HN UT WOS:000246369900027 PM 17536418 ER PT J AU Thompson, FC AF Thompson, F. Christian TI Microdon falcatus Williston (Diptera : Syrphidae): A redescription, with lectotype designation and new synonyms SO ENTOMOLOGICAL NEWS LA English DT Article DE Microdon falcatus; Diptera; Syrphidae; redescrition; lectotype; synonyms; Neotropics AB Microdon falcatus Williston 1887 (Diptera: Syrphidae) is redescribed. A lectotype is designated for the name and three new synonyms are proposed (Microdon aquilinus Giglio-Tos 1892, Microdon hondanaria Hull 1940, and Microdon mellogutta Hull 1943). C1 USDA, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20560 USA. RP Thompson, FC (reprint author), USDA, Systemat Entomol Lab, Smithsonian Inst, NHB-168, Washington, DC 20560 USA. EM chris.thompson@ars.usda.gov NR 17 TC 3 Z9 3 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0013-872X EI 2162-3236 J9 ENTOMOL NEWS JI Entomol. News PD MAY-JUN PY 2007 VL 118 IS 3 BP 283 EP 291 DI 10.3157/0013-872X(2007)118[283:MFWDSA]2.0.CO;2 PG 9 WC Entomology SC Entomology GA 196SS UT WOS:000248502900010 ER PT J AU Sheppard, PR Speakman, RJ Ridenour, G Witten, ML AF Sheppard, Paul R. Speakman, Robert J. Ridenour, Gary Witten, Mark L. TI Temporal variability of tungsten and cobalt in Fallon, Nevada SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article DE childhood leukemia; cobalt; dendrochemistry; Fallon; Nevada; tungsten ID CHILDHOOD LEUKEMIA CLUSTER; MILITARY AVIATION FACILITIES; TREE-RINGS; ELEVATED TUNGSTEN; CARBIDE; POWDER; WATER; TOXICITY; METALS; ALLOY AB BACKGROUND: Since 1997, Fallon, Nevada, has experienced a duster of childhood leukemia that has been declared '' one of the most unique clusters of childhood cancer ever reported.'' Multiple environmental studies have shown airborne tungsten and cobalt to be elevated within Fallon, but the question remains: Have these metals changed through time in correspondence with the onset of the leukemia cluster? METHODS: We used dendrochemistry, the study of element concentrations through time in tree rings, in Fallon to assess temporal variability of airborne tungsten and cobalt since the late 1980s. The techniques used in Fallon were also tested in a different town (Sweet Home, OR) that has airborne tungsten from a known source. RESULTS: The Sweet Home test case confirms the accuracy of dendrochemistry for showing temporal variability of environmental tungsten. Given that dendrochemistry works for tungsten, tree-ring chemistry shows that tungsten increased in Fallon relative to nearby comparison towns beginning by the mid-1990s, slightly before the onset of the cluster, and cobalt has been high throughout the last similar to 15 years. Other metals do not show trends through time in Fallon. DISCUSSION: Results in Fallon suggest a temporal correspondence between the onset of excessive childhood leukemia and elevated levels of tungsten and cobalt. Although environmental data alone cannot directly link childhood leukemia with exposure to metals, research by others has shown that combined exposure to tungsten and cobalt can be carcinogenic to humans. CONCLUSION: Continued biomedical research is warranted to directly test for linkage between childhood leukemia and tungsten and cobalt. C1 Univ Arizona, Lab Tree Ring Res, Tucson, AZ 85721 USA. Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. Internal Med, Fallon, NV USA. Univ Arizona, Dept Pediat, Tucson, AZ USA. RP Sheppard, PR (reprint author), Univ Arizona, Lab Tree Ring Res, 105 W Stadium, Tucson, AZ 85721 USA. EM sheppard@ltrr.arizona.edu OI Speakman, Robert/0000-0003-2063-154X NR 45 TC 29 Z9 29 U1 0 U2 15 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD MAY PY 2007 VL 115 IS 5 BP 715 EP 719 DI 10.1289/ehp.9451 PG 5 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 163KZ UT WOS:000246159900030 PM 17520058 ER PT J AU Wagner, CG AF Wagner, Cynthia G. TI Designing for the "Other 90 Percent" SO FUTURIST LA English DT Article C1 Smithsonian Inst, Cooper Hewitt Natl Design Museum, New York, NY 10028 USA. RP Wagner, CG (reprint author), Smithsonian Inst, Cooper Hewitt Natl Design Museum, 2 E 91st St, New York, NY 10028 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WORLD FUTURE SOCIETY PI BETHESDA PA 7910 WOODMONT AVE, SUITE 450, BETHESDA, MD 20814 USA SN 0016-3317 J9 FUTURIST JI Futurist PD MAY-JUN PY 2007 VL 41 IS 3 BP 34 EP 35 PG 2 WC Social Issues SC Social Issues GA 158AC UT WOS:000245762100019 ER PT J AU DiMichele, WA Falcon-Lang, HJ Nelson, WJ Brick, SD Ames, PR AF DiMichele, William A. Falcon-Lang, Howard J. Nelson, W. John Brick, Scott D. Ames, Philip R. TI Ecological gradients within a Pennsylvanian mire forest SO GEOLOGY LA English DT Article DE pennsylvanian; coal geology; peat mire; coal balls; spatial; heterogeneity; ecological gradients ID PLANT-COMMUNITIES; CONSTRAINTS AB Pennsylvanian coals represent remains of the earliest peat-forming rain forests, but there is no current consensus on forest ecology. Localized studies of fossil forests suggest intermixture of taxa (heterogeneity), while, in contrast, coal ball and palynological analyses imply the existence of pronounced ecological gradients. Here, we report the discovery of a spectacular fossil forest preserved over 1000 ha on top of the Pennsylvanian (Desmoinesian) Herrin (No. 6) Coal of Illinois, United States. The forest was abruptly drowned when fault movement dropped a segment of coastal mire below sea level. In the largest study of its kind to date, forest composition is statistically analyzed within a well-constrained paleogeographic context. Findings resolve apparent conflicts in models of Pennsylvanian mire ecology by confirming the existence of forest heterogeneity at the local scale, while additionally demonstrating the emergence of ecological gradients at landscape scale. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. Illinois State Geol Survey, Champaign, IL 61820 USA. Black Beauty Coal Co, Evansville, IN 47715 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM dimichel@si.edu RI Falcon-Lang, Howard/D-8465-2011; DiMichele, William/K-4301-2012 NR 15 TC 48 Z9 49 U1 3 U2 12 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD MAY PY 2007 VL 35 IS 5 BP 415 EP 418 DI 10.1130/G23472A.1 PG 4 WC Geology SC Geology GA 221UX UT WOS:000250253900008 ER PT J AU Farmer, AJ Goldreich, P AF Farmer, Alison J. Goldreich, Peter TI How much oxygen is too much? Constraining Saturn's ring atmosphere SO ICARUS LA English DT Article DE ionospheres; Saturn, rings; Saturn, magnetosphere ID WATER ICE; IONOSPHERE; DYNAMICS; SYSTEM; MODEL AB The discovery of a molecular oxygen atmosphere around Saturn's rings has important implications for the electrodynamics of the ring system. Its existence was inferred from the Cassini in situ detection of molecular oxygen ions above the rings during Saturn Orbit Insertion in 2004. Molecular oxygen is difficult to observe remotely, and theoretical estimates have yielded only a lower limit (Nu greater than or similar to 10(13) cm(-2)) to the O-2 column density. Comparison with observations has previously concerned matching ion densities at spacecraft altitudes far larger than the scale height of the neutral atmosphere. This is further complicated by charged particle propagation effects in Saturn's offset magnetic field. In this study we adopt a complementary approach, by focusing on bulk atmospheric properties and using additional aspects of the Cassini observations to place an upper limit on the column density. We develop a simple analytic model of the molecular atmosphere and its photo-ionization and dissociation products, with N-n a free parameter. Heating of the neutrals by viscous stir-ring, cooling by collisions with the rings, and torquing by collisions with pickup ions are all included in the model. We limit the neutral scale height to h less than or similar to 3000 km using the INMS neutral density nondetection over the A ring. A first upper limit to the neutral column is derived by using our model to reassess O-2 production and loss rates. Two further limits are then obtained from Cassini observations: corotation of the observed ions with the planet implies that the height-integrated conductivity of the ring atmosphere is less than that of Saturn's ionosphere; and the nondetection of fluorescent atomic oxygen over the rings constrains the molecular column from which it is produced via photo-dissociation. These latter limits are independent of production and loss rates and are only weakly dependent on temperature. From the three independent methods described, we obtain similar limits: Nn less than or similar to 2 x 10(15) cm(-2). The mean free path for collisions between neutrals thus cannot be very much smaller than the scale height. (c) 2007 Elsevier Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. Inst Adv Study, Princeton, NJ 08540 USA. RP Farmer, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS-51,60 Garden St, Cambridge, MA 02138 USA. EM afarmer@cfa.harvard.edu NR 22 TC 5 Z9 5 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 2007 VL 188 IS 1 BP 108 EP 119 DI 10.1016/j.icarus.2006.11.013 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160WA UT WOS:000245971900007 ER PT J AU Baldwin, CC Leis, JM AF Baldwin, Carole C. Leis, Jeffrey M. TI Rainfordia opercularis, a liopropomin serranid (Teleostei : Serranidae : Epinephelinae): corroborative evidence from settlement-stage larvae SO ICHTHYOLOGICAL RESEARCH LA English DT Article DE Rainfordia opercularis; settlement-stage larvae; relationships; epinephelinae; liopropomini ID FISHES AB Rainfordia opercularis was described in 1923 from a single specimen taken in Edgecumbe Bay, Queensland, Australia. The species is rare in museum collections, and the larvae have not been described. In 1999, two settlement-stage larvae (20-21 mm in standard length) were collected in light traps set off Lizard Island, Great Barrier Reef, Queensland. The smaller of the two has one thin, flexible, extremely elongate dorsal-fin spine encased in a pigmented sheath. The larger specimen lacks an elongate dorsal-fin spine and exhibits caudal-fin pigment characteristic of adults. A combination of features in one or both of the settlement-stage larvae support the placement of Rainfordia in the epinepheline-serranid tribe Liopropomini: presence of an elongate, filamentous dorsal-fin spine serially associated with the first dorsal-fin pterygiophore; presence of a spine on the inner preopercular ridge; presence of dense pigment on the frontals; absence of an elongate spine at the angle of the preopercle; and absence of supraorbital spination. C1 Smithsonian Inst, Div Fishes, MRC 159, Natl Museum Nat Hist, Washington, DC 20013 USA. Australian Museum, Sydney, NSW 2010, Australia. RP Baldwin, CC (reprint author), Smithsonian Inst, Div Fishes, MRC 159, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM baldwinc@si.edu RI Leis, Jeffrey/E-7502-2012; OI Leis, Jeffrey/0000-0003-0603-3447 NR 14 TC 1 Z9 1 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 PY 2007 VL 54 IS 2 BP 193 EP 197 DI 10.1007/s10228-006-0390-y PG 5 WC Zoology SC Zoology GA 181SQ UT WOS:000247456800008 ER PT J AU Hunt, DR Bullen, L AF Hunt, D. R. Bullen, L. TI The frequency of os acromiale in the Robert J. Terry collection SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE non-metric traits; acromial process; stress-induced trauma; population-specific features ID IMPINGEMENT; ANATOMY C1 Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. RP Hunt, DR (reprint author), Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, MRC 112,POB 37012, Washington, DC 20013 USA. EM huntd@si.edu NR 26 TC 7 Z9 8 U1 0 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 MAY-JUN PY 2007 VL 17 IS 3 BP 309 EP 317 DI 10.1002/oa.877 PG 9 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 180UU UT WOS:000247392400007 ER PT J AU Rompre, G Robinson, WD Desrochers, A Angehr, G AF Rompre, Ghislain Robinson, W. Douglas Desrochers, Andre Angehr, George TI Environmental correlates of avian diversity in lowland Panama rain forests SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE avian diversity; biogeographical history; distribution patterns; environmental correlates; habitat heterogeneity; neotropical rain forest; Panama Canal corridor; path analysis; plant species richness; species sensitivity ID BIRD SPECIES RICHNESS; TROPICAL FOREST; PATH-ANALYSIS; HABITAT FRAGMENTATION; VEGETATION STRUCTURE; PLANT DIVERSITY; GLOBAL PATTERNS; REGIONAL-SCALE; LAND-USE; GRADIENT AB Aim The composition of communities is known to be influenced by biogeographical history, but also by local environmental conditions. Yet few studies have evaluated the relative importance of the direct and indirect effects of multiple factors on species diversity in rich Neotropical forests. Our study aims to assess drivers of change in local bird species richness in lowland tropical rain forests. Location Thirty-two physiographic subregions along the corridor of the Panama Canal, Panama. Methods We mapped the distributions of all forest-dwelling bird species and quantified the environmental characteristics of all subregions, including mean annual rainfall, topographic complexity, elevational variability, forest age and forest area. Plant species richness, believed to be correlated with structural complexity, was estimated by interpolation through kriging for subregions where data were unavailable. Results The study region has a strong rainfall gradient across a short distance (65 km), which is also accompanied by steep gradients in plant and bird species diversity. Path analysis showed that precipitation strongly affected plant species diversity, which in turn affected avian diversity. Forest age and topography affected bird diversity independently of plant diversity. Forest area and its proportion occurring in the largest two fragments of each subregion (habitat configuration) were also positive correlates of bird species richness. Main conclusions Our results suggest that plant species richness, known to be influenced in part by biogeographical history and geology, also affects bird species assemblages locally. We provide support for the hypothesis that bird species richness increases with structural complexity of the habitat. Our analysis of the distributions of the region's most disturbance-sensitive bird species showed that subregions with more rainfall, more complex topography and older forests harboured not only richer communities but also more sensitive species; while subregions with the opposite characteristics usually lacked large fractions of the regional forest bird community and hosted only common, widely distributed species. Results also emphasize the importance of preserving forest diversity from habitat loss and fragmentation, and confirm that larger, continuous forest tracts are necessary to maintain the rich avian diversity in the region. C1 Univ Laval, Fac Foresterie & Geomat, Ctr Etud Foret, Quebec City, PQ G1K 7P4, Canada. Oregon State Univ, Dept Fisheries & Wildlife, Oak Creek Lab Biol, Corvallis, OR 97331 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Rompre, G (reprint author), Univ Laval, Fac Foresterie & Geomat, Ctr Etud Foret, Quebec City, PQ G1K 7P4, Canada. EM ghislain.rompre.1@ulaval.ca RI Rohlf, F/A-8710-2008; Desrochers, Andre/B-6248-2008 OI Desrochers, Andre/0000-0002-5676-964X NR 94 TC 24 Z9 26 U1 0 U2 34 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD MAY PY 2007 VL 34 IS 5 BP 802 EP 815 DI 10.1111/j.1365-2699.2006.01657.x PG 14 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 157BN UT WOS:000245693700007 ER PT J AU Suarez-Morales, E Iliffe, TM AF Suarez-Morales, Eduardo Iliffe, Thomas M. TI A new genus of Ridgewayiidae (Copepoda : Calanoida) from a karstic cave of the western Caribbean SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article ID BIOGEOGRAPHY; BAHAMAS; GENERA AB The calanoid copepod family Ridgewayiidae, containing demersal and cave-dwelling forms, has representatives worldwide. bill Most have been known from the Northwestern Tropical Atlantic. Eight valid genera were hitherto known, most of them were described recently (Ridgewayia Thompson and Scott. Exumella Fosshagen, Brattstromia Fosshagen and Hille, Placocalamus Ohtsuka, Fosshagen and Soh, Exumellina Fosshagen and Iliffe, Normancava Fosshagen and Iliffe, Robpalmeria Fosshagen and Iliffe, Slargatia Fosshagen and Iliffe). Biological collections in cave environments ill all island off the Caribbean coastline of Honduras, Central America, showed the presence of ridgewayiid copepods. These specimens Were found to belong to an undescribed genus of the family. The new genus Hondurella is distinguished from the other eight known ridgewayiid genera by a combination of characters that include a simple rostillill with 110 filaments, maxilliped with modified setae, first leg with a modified exopod and a reduced endopodal armature, and most importantly. a female fifth leg with a slightly modified exopod and a l-segmented endopod, plus a reduced right exopod of the male fifth leg, and the presence of spines oil the middle segments of the male right antennule. As all other ridgewayiids, the new genus retains several plesiomorphic characters. thus confirming the primitive profile of this family. The distribution of Ridgewayiidae in the Caribbean region remains largely unknown, bill it is suggested that distributional patterns and a relatively high degree of endemism are related to the geological Origin and dynamics of the area. Aside the modified maxillipedal setae, mouthparts in the new genus, are normally developed; this, together with our observations of the gut contents, suggest that this ridgewayiid is more a particle-feeder than a carnivorous form. C1 ECOSUR, Chetmal 77000, Qunitana Roo, Mexico. Texas A&M Univ, Dept Marine Biol, Natl Museum Nat Hist, Smithsonian Inst, Galveston, TX 77553 USA. RP Suarez-Morales, E (reprint author), ECOSUR, AP 424, Chetmal 77000, Qunitana Roo, Mexico. EM esuarez@ecosur-qroo.mx NR 17 TC 6 Z9 6 U1 0 U2 1 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD MAY PY 2007 VL 27 IS 2 BP 339 EP 350 DI 10.1651/S-2720.1 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 164LG UT WOS:000246234600018 ER PT J AU Comita, LS Condit, R Hubbell, SP AF Comita, Liza S. Condit, Richard Hubbell, Stephen P. TI Developmental changes in habitat associations of tropical trees SO JOURNAL OF ECOLOGY LA English DT Article DE dispersal limitation; edaphic specialization; environmental heterogeneity; habitat preference; regeneration niche; tropical tree seedlings ID NEOTROPICAL RAIN-FOREST; SPATIAL-PATTERNS; LIFE-HISTORY; SPECIES DISTRIBUTIONS; TOPOGRAPHIC POSITION; SEEDLING MORTALITY; DIVERSITY; RECRUITMENT; NICHE; LIGHT AB 1 Recent studies have documented local-scale associations between tree species and topographic and edaphic habitat types in forests worldwide. To determine whether such associations form at early life stages, we compared species' positive associations with five habitat types (high plateau, low plateau, slope, streamside, and swamp) at two life stages for 80 tree and shrub species in a Panamanian lowland forest. 2 Nineteen significant, positive habitat associations were detected at the small tree stage (seedlings and saplings >= 20 cm tall and < 1 cm d.b.h.), and 18 at the large tree stage (individuals >= 1 cm d.b.h.), according to results of torus-translation randomization tests. The majority of species did not show consistent associations at the two stages. Of the 30 species significantly associated with a habitat, only five were associated with the same habitat at both stages. Overall, more species were associated with the wetter slope habitat at the large tree stage compared with the small tree stage. 3 For a subset of species, we examined the relationship between observed habitat associations and seed dispersal and seedling establishment patterns by using species-specific seed dispersal kernels to predict seed rain into each habitat. 4 Two-thirds of species associated with a habitat at the large tree stage had higher predicted seed densities in the associated habitat relative to other habitat types, indicating that limited seed dispersal acts to reinforce habitat associations for most species. In contrast, only one-third of the species associated with a habitat at the large tree stage showed evidence of higher seedling establishment rates in the associated habitat compared with other habitats, and an equal number of species appeared to have lower rates of establishment in the habitat that large trees of the species were associated with. 5 Overall, our results indicate that habitat associations of large trees typically do not form at early life stages. Rather, many species appear to exhibit different ecological habitat preferences across life stages. Future studies of species' habitat associations should therefore include multiple life stages in order to detect developmental shifts in ecological preferences. C1 Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. RP Comita, LS (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, 100 Ecol Bldg,1987 Upper Buford Circle St, St Paul, MN 55108 USA. EM comit001@umn.edu OI Comita, Liza/0000-0002-9169-1331 NR 63 TC 94 Z9 110 U1 1 U2 29 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD MAY PY 2007 VL 95 IS 3 BP 482 EP 492 DI 10.1111/j.1365-2745.2007.01229.x PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 157BO UT WOS:000245693800009 ER PT J AU Brown, RP Ubelaker, DH Schanfield, MS AF Brown, Robert P. Ubelaker, Douglas H. Schanfield, Moses S. TI Evaluation of Purkait's triangle method for determining sexual dimorphism SO JOURNAL OF FORENSIC SCIENCES LA English DT Article; Proceedings Paper CT 58th Annual Meeting of the American-Academy-of-Forensic-Sciences CY FEB, 2006 CL Seattle, WA SP Amer Acad Forens Sci DE forensic science; forensic anthropology; sex determination; femur ID FEMUR; WHITES; BLACKS AB The identification of sex from the skeleton is an important demographic assessment in medicolegal investigations. Rama Purkait developed a method for estimating sex using measurements from a triangle defined by three points on the proximal end of the femur using skeletal material from Bhopal, India. This method was tested with measurements on 200 Indo-European and African American adult femora from the Terry collection using discriminant function analysis to determine if Purkait's method was valuable for determining sex in Americans. A side-by-side analysis was conducted of Purkait's "triangle method" and the maximum diameter of the femoral head to determine their relative value in assessing sexual dimorphism. In the study sample a single variable from Purkait's method provided 85.5% prediction accuracy, similar to 87% for the head diameter. Combining threshold values for a single variable from Purkait's method and the femoral head diameter raised the predictability to greater than 90% for both sexes. C1 Smithsonian Inst, Dept Anthropol, NMNH, MRC 112, Washington, DC 20560 USA. USA, Criminal Invest Command, Ft Lewis, WA 98433 USA. George Washington Univ, Dept Forens Sci, Washington, DC 20052 USA. RP Brown, RP (reprint author), 22nd Mil Police Battal CID,POB 331009, Ft Lewis, WA 98433 USA. EM Robert.paul.brown@us.army.mil NR 8 TC 7 Z9 7 U1 1 U2 4 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD MAY PY 2007 VL 52 IS 3 BP 553 EP 556 DI 10.1111/j.1556-4029.2007.2007.00423.x PG 4 WC Medicine, Legal SC Legal Medicine GA 160LN UT WOS:000245942300006 PM 17456081 ER PT J AU Hill, EM Ponte, RM Davis, JL AF Hill, Emma M. Ponte, Rui M. Davis, James L. TI Dynamic and regression modeling of ocean variability in the tide-gauge record at seasonal and longer periods SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID MEAN SEA-LEVEL; SPACED DATA; RISE; MASS; VOLUME; CYCLE AB [1] Comparison of monthly mean tide-gauge time series to corresponding model time series based on a static inverted barometer (IB) for pressure-driven fluctuations and a ocean general circulation model ( OM) reveals that the combined model successfully reproduces seasonal and interannual changes in relative sea level at many stations. Removal of the OM and IB from the tide-gauge record produces residual time series with a mean global variance reduction of 53%. The OM is mis-scaled for certain regions, and 68% of the residual time series contain a significant seasonal variability after removal of the OM and IB from the tide-gauge data. Including OM admittance parameters and seasonal coefficients in a regression model for each station, with IB also removed, produces residual time series with mean global variance reduction of 71%. Examination of the regional improvement in variance caused by scaling the OM, including seasonal terms, or both, indicates weakness in the model at predicting sea-level variation for constricted ocean regions. The model is particularly effective at reproducing sea-level variation for stations in North America, Europe, and Japan. The RMS residual for many stations in these areas is 25 - 35 mm. The production of "cleaner'' tide-gauge time series, with oceanographic variability removed, is important for future analysis of nonsecular and regionally differing sea-level variations. Understanding the ocean model's strengths and weaknesses will allow for future improvements of the model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Atmospher & Environm Res Inc, Lexington, MA 02421 USA. RP Hill, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM ehill@cfa.harvard.edu; ponte@aer.com; jdavis@cfa.harvard.edu RI Hill, Emma/B-7037-2011; Davis, James/D-8766-2013; OI Hill, Emma/0000-0003-0231-5818; Davis, James/0000-0003-3057-477X; Ponte, Rui/0000-0001-7206-6461 NR 36 TC 8 Z9 8 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD MAY 1 PY 2007 VL 112 IS C5 AR C05007 DI 10.1029/2006JC003745 PG 14 WC Oceanography SC Oceanography GA 165LQ UT WOS:000246307400004 ER PT J AU Collard, M Wood, B AF Collard, Mark Wood, Bernard TI Hominin homoiology: An assessment of the impact of phenotypic plasticity on phylogenetic analyses of humans and their fossil relatives SO JOURNAL OF HUMAN EVOLUTION LA English DT Review DE hominin; phylogeny; homoplasy; homoiology; hominoid; variance ID MONKEY TRIBE PAPIONINI; INVIVO BONE STRAIN; TRAIT LIST BIAS; HUMAN-EVOLUTION; MACACA-FASCICULARIS; CLADISTIC-ANALYSIS; GALAGO CRASSICAUDATUS; PRIMATE PHYLOGENETICS; CONTINUOUS CHARACTERS; DENTAL MORPHOLOGY AB Homoiologies are phylogenetically misleading morphological similarities that are due to nongenetic factors. It has been claimed that homoiologies are common in the hominin skull, especially in regions affected by masticatory strain, and that their prevalence is one reason why reconstructing hominin phylogenetic relationships is difficult. To evaluate this "homoiology hypothesis," we performed analyses on a group of extant primates for which a robust molecular phylogeny is available-the hominoids. We compiled a data set from measurements that developmental considerations and experimental evidence suggest differ in their likelihood of exhibiting masticatory-strain-induced phenotypic plasticity. We then used the coefficient of variation and t-tests to evaluate the phenotypic plasticity of the measurements. We predicted that, if the hypothesis is correct, the measurements of skeletal features that do not remodel and therefore are unaffected by phenotypic plasticity should be less variable than the measurements of skeletal features that remodel and are subject to low-to-moderate strains, and that the latter should be less variable than the measurements of skeletal features that remodel and are subject to moderate-to-high strains. Subsequently, we performed phylogenetic analyses on character state data derived from the measurements and compared the resulting phylogenetic hypotheses to the consensus molecular phylogeny for the hominoids. We predicted that, if the hypothesis is correct, agreement between the phylogenies should be best for the non-phenotypically-plastic characters, intermediate for the low-to-moderate-strain characters, and worst for the moderate-to-high-strain characters. The results of the coefficient of variation/t-test analyses were consistent with the predictions of the hypothesis to the extent that the moderate-to-high-strain measurements exhibited significantly more variability than the non-phenotypically-plastic and low-to-moderate-strain measurements. In contrast, the results of the phylogenetic analyses were not those predicted. The phylogeny derived from the moderate-to-high-strain characters matched the molecular phylogeny better than those obtained using the non-phenotypically-plastic and low-to-moderate-strain characters. Thus, our study supports the suggestion that mechanical loading results in phenotypic plasticity in the hominin skull, but it does not support the notion that homoiologies have a significant negative impact on hominin phylogenetics. (c) 2007 Elsevier Ltd. All rights reserved. C1 Univ British Columbia, Lab Biol Anthropol, Dept Anthropol, Vancouver, BC V6T 1Z1, Canada. UCL, AHRC Ctr Evolut Cultural Divers, Archaeol Inst, London WC1H 0PY, England. George Washington Univ, CASHP, Dept Anthropol, Washington, DC 20052 USA. Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC USA. RP Collard, M (reprint author), Univ British Columbia, Lab Biol Anthropol, Dept Anthropol, 6303 NW Marine Dr, Vancouver, BC V6T 1Z1, Canada. EM mark.collard@ubc.ca; bernardawood@gmail.com FU Wellcome Trust NR 142 TC 27 Z9 27 U1 3 U2 20 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAY PY 2007 VL 52 IS 5 BP 573 EP 584 DI 10.1016/j.jhevol.2006.11.018 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 176AL UT WOS:000247055000009 PM 17412395 ER PT J AU Fukami, H Chen, CA Chiou, CY Knowlton, N AF Fukami, Hironobu Chen, Chaolun Allen Chiou, Chi-Yung Knowlton, Nancy TI Novel group I introns encoding a putative homing endonuclease in the mitochondrial cox1 gene of scleractinian corals SO JOURNAL OF MOLECULAR EVOLUTION LA English DT Article DE scleractinia; corals; mitochondria; group I intron; homing endonuclease; cox1 ID SPECIES COMPLEX CNIDARIA; ANEMONE METRIDIUM-SENILE; DNA-SEQUENCES; SARCOPHYTON-GLAUCUM; HORIZONTAL TRANSFER; ACROPORA-TENUIS; RIBOSOMAL-RNA; EVOLUTION; GENOME; ORDER AB Analyses of mitochondrial sequences revealed the existence of a group I intron in the cytochrome oxidase subunit 1 (cox1) gene in 13 of 41 genera (20 out of 73 species) of corals conventionally assigned to the suborder Faviina. With one exception, phylogenies of the coral cox1 gene and its intron were concordant, suggesting at most two insertions and many subsequent losses. The coral introns were inferred to encode a putative homing endonuclease with a LAGLI-DADG motif as reported for the cox1 group I intron in the sea anemone Metridium senile. However, the coral and sea anemone cox1 group I introns differed in several aspects, such as the intron insertion site and sequence length. The coral cox1 introns most closely resemble the mitochondrial cox1 group I introns of a sponge species, which also has the same insertion site. The coral introns are also more similar to the introns of several fungal species than to that of the sea anemone (although the insertion site differs in the fungi). This suggests either a horizontal transfer between a sponge and a coral or independent transfers from a similar fungal donor (perhaps one with an identical insertion site that has not yet been discovered). The common occurrence of this intron in corals strengthens the evidence for an elevated abundance of group I introns in the mitochondria of anthozoans. C1 Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. Acad Sinica, Res Ctr Biodivers, Taipei 115, Taiwan. Smithsonian Trop Res Inst, Balboa, Panama. Kyoto Univ, Field Sci Educ & Res Ctr, Seto Marine Biol Lab, Wakayama 6492211, Japan. RP Fukami, H (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. EM hfukami@kais.kyoto-u.ac.jp NR 50 TC 35 Z9 35 U1 0 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0022-2844 J9 J MOL EVOL JI J. Mol. Evol. PD MAY PY 2007 VL 64 IS 5 BP 591 EP 600 DI 10.1007/s00239-006-0279-4 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 165NC UT WOS:000246311200010 PM 17437148 ER PT J AU Ram, RS Gordon, I Hirao, T Yu, S Bernath, PF Pinchemel, B AF Ram, R. S. Gordon, I. Hirao, T. Yu, S. Bernath, P. F. Pinchemel, B. TI Fourier transform emission spectroscopy of the C-3 Delta-X-3 Phi, D-3 Delta-X-3 Phi, G(3)Phi-X-3 Phi and G(3)Phi-C-3 Delta systems of CoCl SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE fourier transform spectroscopy; transition metal halides; metal chlorides ID ROTATIONAL SPECTRUM; COF; COBALT; REGION; IRON AB The emission spectrum of CoCl has been recorded in the 2000-23 000 cm(-1) region at high resolution. CoCl was made in a carbon tube furnace by heating cobalt metal to a temperature of about 2300 degrees C as well as in a DC discharge source and the spectra were observed using a Fourier transform spectrometer. The bands observed in the 2000-13000 cm(-1) interval have been classified into four transitions: 3 3(1)_X3(D 3q)_C3 C-3 Delta-X-3 Phi (2500-3600 cm(-1)), D-3 Delta-X-3 Phi (9300-10 030 cm(-1)), G(3)Phi-X-3 Phi (8500-13000 cm(-1)) and G(3)Phi-C-3 Delta (7400-7900 cm(-1)) analogous to the near infrared transitions of CoF reported previously [R.S. Ram, P.F. Bernath, S.P. Davis, J. Chem. Phys. 104 (1996) 6949.]. A rotational analysis of a number of vibrational bands of these transitions has been obtained and spectroscopic constants extracted for the low-lying electronic states of CoCl. It is found that the energy levels of CoCl correlate very well with those of CoF and CoH. (c) 2007 Elsevier Inc. All rights reserved. C1 Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. Univ Sci & Tech Lille Flandres Artois, Ctr Etud & Rech Lasers & Applicat, Lab PhLAM, F-59655 Villeneuve Dascq, France. RP Ram, RS (reprint author), Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. EM rram@u.arizona.edu RI Bernath, Peter/B-6567-2012; Yu, Shanshan/D-8733-2016 OI Bernath, Peter/0000-0002-1255-396X; NR 26 TC 4 Z9 4 U1 0 U2 7 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 MAY PY 2007 VL 243 IS 1 BP 69 EP 77 DI 10.1016/j.jms.2007.03.007 PG 9 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 183YV UT WOS:000247609200008 ER PT J AU Hershler, R Liu, HP Sada, DW AF Hershler, Robert Liu, Hsiu-Ping Sada, Donald W. TI Origin and diversification of the soldier meadow springsnails (Hydrobiidae : Pyrgulopsis), a species flock in the northwestern Great Basin, United States SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID AMERICAN NYMPHOPHILINE GASTROPODS; MITOCHONDRIAL-DNA SEQUENCES; EVOLUTIONARY GENETICS; RIVER-BASIN; NEVADA; POPULATION; CALIFORNIA; HISTORY; RANGE; SYSTEMATICS AB The large, western North American hydrobiid gastropod genus Pyrgulopsis (commonly known as springsnails) includes a series of locally endemic faunas that are thought to be species flocks. Although these assemblages are of interest from the evolutionary, biogeographic and conservation perspectives, their monophyly and phylogenetic relationships have yet to be rigorously evaluated. Here we present a molecular phylogeny (based on mitochondrial sequence data) of a putative flock of four thermal spring-dwelling springsnails that is distributed in many sites in Soldier Meadow and a single locality in Bog Hot Valley (northwestern Nevada). Our analyses support monophyly of this assemblage ('Soldier Meadow clade') and a close relationship with other regional species and suggest that the invasion of thermal habitats by these springsnails occurred independently of other such radiations within the genus. The divergence of the Soldier Meadow clade relative to its sister group is substantial (6.7910.36% for COI, 10.35-15.88% for NDI), suggesting a split in the early Pliocene, based on the application of a COI clock for Pyrgulopsis. The splits within the Soldier Meadow clade into three main subunits also appear to be old events, based on their 5.78-8.54% COI divergence relative to each other. These findings are consistent with a long history of springsnail evolution in Soldier Meadow, which is intriguing given that this basin was flooded by Lake Lahontan during periods of the early and middle Pleistocene. We suggest that progenitors of the contemporary fauna survived in high elevation springs that may have been present in the basin during these pluvial periods and subsequently colonized contemporary habitats following the termination of the extreme Lake Lahontan highstands. We speculate that the broadly disjunct population (of P. militaris) in Bog Hot Valley, which is consistently nested within the Soldier Meadow clade in our phylogenetic analyses, is either a vicariant relict of a spring zone that may have once extended between these two areas; or was founded by a past `jump' dispersal event from Soldier Meadow. Phylogeographic structure of springsnail populations in Soldier Meadow bears the strong stamp of geologically recent, allopatric diversification, perhaps reflecting the short time that basin floor habitats have been occupied. We describe a new species (P. varneri) for a series of recently discovered populations that are monophyletic, substantially divergent and morphologically distinctive. Additional studies will be necessary to confidently assess the taxonomic status of morphologically distinctive P. limaria and P. umbilicata, which are shown herein to be little divergent genetically; and a recently discovered minute springsnail that is morphologically divergent yet closely similar genetically to P. notidicola. C1 Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. Univ Nevada, Desert Res Inst, Div Hydrol Sci, Reno, NV 89512 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-205,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu NR 66 TC 10 Z9 10 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 EI 1464-3766 J9 J MOLLUS STUD JI J. Molluscan Stud. PD MAY PY 2007 VL 73 BP 167 EP 183 DI 10.1093/mollus/eym/014 PN 2 PG 17 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 207QW UT WOS:000249267200007 ER PT J AU Goodyear, FH AF Goodyear, Frank H., III TI The blue and gray in black and white: A history of Civil War photography. SO JOURNAL OF SOUTHERN HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Goodyear, FH (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 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 2007 VL 73 IS 2 BP 472 EP 473 PG 2 WC History SC History GA 161XT UT WOS:000246051100044 ER PT J AU Zotz, G AF Zotz, Gerhard TI The population structure of the vascular epiphytes in a lowland forest in Panama correlates with species abundance SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Bromeliaceae; Orchidaceae; population dynamics; rarity; San Lorenzo crane site; size class structure; tropical forests ID PALM SOCRATEA-EXORRHIZA; TROPICAL FORESTS; LONG-TERM; VEGETATION; GROWTH; DIVERSITY; DYNAMICS; RATES; SIZE; RARE AB The long-term dynamics of epiphyte communities are little studied although such baseline data are urgently needed, in particular in the context of global change. Census data of a vascular epiphyte community from 0.4 ha Of undisturbed lowland forest in Panama were used to infer future changes in community composition by deducing population growth from the current size class structure of populations. The study includes 11 387 individuals out of 45 species. ranging in abundance from 16 to 1 568 individuals. There was a significant negative correlation between the size of a population and the steepness of the size distribution, indicating that more common species are likely to increase in abundance in the future, while rarer species apparently depend on immigration from other populations to allow local persistence. C1 Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 28 TC 3 Z9 8 U1 1 U2 8 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 2007 VL 23 BP 337 EP 342 DI 10.1017/S026646740700404X PN 3 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 174IK UT WOS:000246935400009 ER PT J AU Arnold, AE Engelbrecht, BMJ AF Arnold, A. Elizabeth Engelbrecht, Bettina M. J. TI Fungal endophytes nearly double minimum leaf conductance in seedlings of a neotropical tree species SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE cocoa; endophytes; minimum leaf conductance; Panama; Theobronia cacao; water relations ID CUTICULAR WATER PERMEABILITY; DROUGHT; LEAVES; IMPACT C1 Univ Arizona, Dept Plant Sci, Div Plant Pathol & Microbiol, Tucson, AZ 85721 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Kaiserslautern, D-67663 Kaiserslautern, Germany. Tech Univ Kaiserslautern, Dept Plant Ecol & Syst, D-67663 Kaiserslautern, Germany. RP Arnold, AE (reprint author), Univ Arizona, Dept Plant Sci, Div Plant Pathol & Microbiol, Tucson, AZ 85721 USA. EM arnold@ag.arizona.edu RI Engelbrecht, Bettina/E-9914-2012 NR 31 TC 34 Z9 38 U1 2 U2 28 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 2007 VL 23 BP 369 EP 372 DI 10.1017/S0266467407004038 PN 3 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 174IK UT WOS:000246935400013 ER PT J AU Matzke, AT AF Matzke, Andreas T. TI An almost complete juvenile specimen of the cheloniid turtle Ctenochelys stenoporus (Hay, 1905) from the Upper Cretaceous Niobrara Formation of Kansas, USA SO PALAEONTOLOGY LA English DT Article DE Testudines; Cheloniidae; Ctenochelys; braincase; Upper Cretaceous; Niobrara Formation; Kansas ID SEA-TURTLE; TESTUDINES AB A new, unusually well-preserved juvenile specimen of Ctenochelys stenoporus from the Niobrara Formation is described. The skull has come apart at its sutures and all bones of the braincase and ear region are preserved three-dimensionally. This allows a detailed reconstruction of the important brain structures of a basal juvenile cheloniid turtle. It is compared with adult Ctenochelys specimens, and the major ontogenetic changes in the skull and postcranial skeleton are described. Furthermore, the specimen is compared with other fossil and extant cheloniids with well-known braincases and the differences between basal and advanced cheloniids turtles are specified. C1 Natl Museum Nat Hist, MRC NHB, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA. RP Matzke, AT (reprint author), Inst Geowissensch, Keplerstr 17, D-72076 Tubingen, Germany. EM matzke@uni-tuebingen.de NR 38 TC 4 Z9 4 U1 1 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0031-0239 J9 PALAEONTOLOGY JI Paleontology PD MAY PY 2007 VL 50 BP 669 EP 691 DI 10.1111/j.1475-4983.2007.00650.x PN 3 PG 23 WC Paleontology SC Paleontology GA 169XB UT WOS:000246624300010 ER PT J AU Christ, KV Sadeghpour, HR AF Christ, K. V. Sadeghpour, H. R. TI Energy dispersion in graphene and carbon nanotubes and molecular encapsulation in nanotubes SO PHYSICAL REVIEW B LA English DT Article ID GRAPHITE; PSEUDOPOTENTIALS; STATES AB Density-functional calculations of electronic and vibrational dispersion energies for pristine graphite monolayer (graphene) and single-walled carbon nanotubes (SWCNTs) are presented. Optimized parameters for nonlocal norm-preserving pseudopotentials which replace the potential field due to core electrons are given. Comparison with observations, where available, is made. The effect of encapsulation of carbon nanotubes with an alkali-halide matrix is numerically investigated. The electronic band structure of encapsulated SWCNT is noticeably modified, as is its charge density, and hence its optical properties. C1 Univ Wisconsin, Dept Mech Engn, Madison, WI 53706 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Christ, KV (reprint author), Univ Wisconsin, Dept Mech Engn, Madison, WI 53706 USA. EM hsadeghpour@cfa.harvard.edu NR 38 TC 13 Z9 13 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD MAY PY 2007 VL 75 IS 19 AR 195418 DI 10.1103/PhysRevB.75.195418 PG 7 WC Physics, Condensed Matter SC Physics GA 173RS UT WOS:000246890800143 ER PT J AU Markevitch, M Vikhlinin, A AF Markevitch, Maxim Vikhlinin, Alexey TI Shocks and cold fronts in galaxy clusters SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS LA English DT Review DE Galaxies : clusters : general-X-rays; Galaxies : clusters-hydrodynamics ID XMM-NEWTON OBSERVATION; LARGE-SCALE STRUCTURE; X-RAY SPECTROSCOPY; FAST MODE SHOCKS; DARK-MATTER; CHANDRA OBSERVATION; THERMAL CONDUCTION; MAGNETIC-FIELD; RADIO HALOS; PERSEUS CLUSTER AB The currently operating X-ray imaging observatories provide us with an exquisitely detailed view of the Megaparsec-scale plasma atmospheres in nearby galaxy clusters. At z < 0.05, the Chandra's 1 '' angular resolution corresponds to linear resolution of less than a kiloparsec, which is smaller than some interesting linear scales in the intracluster plasma. This enables us to study the previously unseen hydrodynamic phenomena in clusters: classic bow shocks driven by the infalling subclusters, and the unanticipated "cold fronts," or sharp contact discontinuities between regions of gas with different entropies. The ubiquitous cold fronts are found in mergers as well as around the central density peaks in "relaxed" clusters. They are caused by motion of cool, dense gas clouds in the ambient higher-entropy gas. These clouds are either remnants of the infalling subclusters, or the displaced gas from the cluster's own cool cores. Both shock fronts and cold fronts provide novel tools to study the intracluster plasma on microscopic and cluster-wide scales, where the dark matter gravity, thermal pressure, magnetic fields, and ultrarelativistic particles are at play. In particular, these discontinuities provide the only way to measure the gas bulk velocities in the plane of the sky. The observed temperature jumps at cold fronts require that thermal conduction across the fronts is strongly suppressed. Furthermore, the width of the density jump in the best-studied cold front is smaller than the Coulomb mean free path for the plasma particles. These findings show that transport processes in the intracluster plasma can easily be suppressed. Cold fronts also appear less prone to hydrodynamic instabilities than expected, hinting at the formation of a parallel magnetic field layer via magnetic draping. This may make it difficult to mix different gas phases during a merger. A sharp electron temperature jump across the best-studied shock front has shown that the electron-proton equilibration timescale is much shorter than the collisional timescale; a faster mechanism has to be present. To our knowledge, this test is the first of its kind for any astrophysical plasma. We attempt a systematic review of these and other results obtained so far (experimental and numerical), and mention some avenues for further studies. (c) 2007 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow Space Res Inst, Moscow 117997, Russia. RP Markevitch, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM maxim@head.cfa.harvard.edu NR 172 TC 314 Z9 314 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-1573 J9 PHYS REP JI Phys. Rep.-Rev. Sec. Phys. Lett. PD MAY PY 2007 VL 443 IS 1 BP 1 EP 53 DI 10.1016/j.physrep.2007.01.001 PG 53 WC Physics, Multidisciplinary SC Physics GA 173ID UT WOS:000246865800001 ER PT J AU Marino, L Connor, RC Fordyce, RE Herman, LM Hof, PR Lefebvre, L Lusseau, D McCowan, B Nimchinsky, EA Pack, AA Rendell, L Reidenberg, JS Reiss, D Uhen, MD Van der Gucht, E Whitehead, H AF Marino, Lori Connor, Richard C. Fordyce, R. Ewan Herman, Louis M. Hof, Patrick R. Lefebvre, Louis Lusseau, David McCowan, Brenda Nimchinsky, Esther A. Pack, Adam A. Rendell, Luke Reidenberg, Joy S. Reiss, Diana Uhen, Mark D. Van der Gucht, Estel Whitehead, Hal TI Cetaceans have complex brains for complex cognition SO PLOS BIOLOGY LA English DT Article ID BOTTLE-NOSED DOLPHINS; RESIDENT KILLER WHALES; ODONTOCETI TOOTHED WHALES; TURSIOPS-TRUNCATUS; CULTURAL TRANSMISSION; SELF-RECOGNITION; CEREBRAL-CORTEX; VOCAL MIMICRY; WHITE-MATTER; ORCINUS-ORCA C1 Emory Univ, Neurosci & Behav Biol Program, Atlanta, GA 30322 USA. Univ Massachusetts, Dept Biol, Dartmouth, MA USA. Univ Otago, Dept Geol, Dunedin, New Zealand. Univ Hawaii Manoa, Dept Psychol, Honolulu, HI 96822 USA. Mt Sinai Sch Med, Dept Neurosci, New York, NY 10029 USA. McGill Univ, Dept Biol, Quebec City, PQ H3A 2T5, Canada. Dalhousie Univ, Dept Biol, Halifax, NS B3H 3J5, Canada. Univ Calif Davis, Sch Vet Med, Davis, CA 95616 USA. Rutgers State Univ, Ctr Mol & Behav Neurosci, Newark, NJ 07102 USA. Dolphin Inst, Honolulu, HI USA. Univ St Andrews, Dept Biol, St Andrews KY16 9AJ, Fife, Scotland. Mt Sinai Sch Med, Dept Anat & Funct Morphol, New York, NY 10029 USA. CUNY Hunter Coll, Dept Psychol, New York, NY 10021 USA. New York Aquarium Wildlife Conservat Soc, Bronx, NY USA. Smithsonian Institut, Dept Paleobiol, Washington, DC USA. Mt Sinai Sch Med, Dept Neurosci, New York, NY USA. RP Marino, L (reprint author), Emory Univ, Neurosci & Behav Biol Program, Atlanta, GA 30322 USA. EM lmarino@emory.edu RI Rendell, Luke/G-2594-2010; Lusseau, David/A-8501-2012; OI Rendell, Luke/0000-0002-1121-9142; Reidenberg, Joy/0000-0002-4180-7156; Fordyce, Ewan/0000-0002-2656-730X; Lusseau, David/0000-0003-1245-3747 NR 90 TC 97 Z9 97 U1 10 U2 122 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1544-9173 J9 PLOS BIOL JI PLoS. Biol. PD MAY PY 2007 VL 5 IS 5 BP 966 EP 972 AR e139 DI 10.1371/journal.pbio.0050139 PG 7 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA 171EC UT WOS:000246716700002 PM 17503965 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI Spacecraft technology: The early years SO SPACE POLICY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, POB 37012, Washington, DC 20013 USA. EM neufeldm@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 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 2007 VL 23 IS 2 BP 131 EP 131 DI 10.1016/j.spacepol.2007.02.005 PG 1 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 176MP UT WOS:000247089700011 ER PT J AU Newell-Fugate, A Kennedy-Stoskopf, S Brown, JL Levine, JF Swanson, WF AF Newell-Fugate, Annie Kennedy-Stoskopf, Suzanne Brown, Janine L. Levine, Jay F. Swanson, William F. TI Seminal and endocrine characteristics of male Pallas' cats (Otocolobus manul) maintained under artificial lighting with simulated natural photoperiods SO ZOO BIOLOGY LA English DT Article DE felids; testosterone; cortisol; leptin; spermatozoa; reproductive seasonality ID CHEETAH ACINONYX-JUBATUS; ADRENOCORTICAL FUNCTION; NONINVASIVE ASSESSMENT; METABOLITE ANALYSIS; MANAGEMENT; FELIDS AB Pallas' cats (Otocolobus manul) have a pronounced reproductive seasonality controlled by photoperiod. Previous studies of reproduction in captive Pallas' cats exposed to natural light showed a breeding season of December April. This study evaluated the impact of artificial lighting timed to simulate natural photoperiods on male reproductive seasonality of four Pallas' cats housed indoors. Semen evaluation, blood collection, and body weight measurements were conducted every 1-2 months from November 2000-June 2001. Fecal samples were collected from each male twice weekly to assess testosterone and corticoid concentrations. Mean values for reproductive traits (sperm attributes, testicular volume) were highest from February-April, the defined breeding season. Fecal testosterone concentrations were highest from mid-January to mid-March. Male Pallas' cats managed indoors under simulated photoperiods experienced a delayed onset of the breeding season by 1-2 months and a decreased length of the breeding season. Over the course of the study, fecal corticoid concentrations did not seem to differ among seasons. Although mating attempts during this study were unsuccessful, subsequent pairings of male and female Pallas' cats in the same research colony during the 2002 and 2003 breeding seasons produced viable offspring. These results suggest that male Pallas' cats, housed indoors under simulated photoperiods, exhibit distinct reproductive cyclic patterns, characterized by a delayed and truncated breeding season. Adrenocortical activity varied among individuals, but did not adversely affect reproductive parameters. Housing Pallas' cats indoors under simulated photoperiods may represent a viable strategy for maintaining breeding success while limiting disease exposure. C1 N Carolina State Univ, Coll Vet Med, Raleigh, NC 27606 USA. Univ Pretoria, Fac Vet Sci, Vet Wildlife Unit, ZA-0002 Pretoria, South Africa. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, Cincinnati, OH USA. RP Kennedy-Stoskopf, S (reprint author), N Carolina State Univ, Coll Vet Med, 4700 Hillsborough St, Raleigh, NC 27606 USA. EM suzanne_stoskopf@ncsu.edu NR 25 TC 5 Z9 5 U1 0 U2 10 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAY-JUN PY 2007 VL 26 IS 3 BP 187 EP 199 DI 10.1002/zoo.20127 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 185EE UT WOS:000247693400003 PM 19360572 ER PT J AU Mah, C AF Mah, Christopher TI Phylogeny of the Zoroasteridae (Zorocallina; Forcipulatida): evolutionary events in deep-sea Asteroidea displaying Palaeozoic features SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE basal diversification; morphology; Neoasteroidea; onshore; offshore; taxonomy; Zoroaster ID NE ATLANTIC-OCEAN; SEASTARS ECHINODERMATA; ANTARCTIC PENINSULA; NORTHEAST PACIFIC; STARS ASTEROIDEA; PALEOCEANOGRAPHY; CLASSIFICATION; CONSUMPTION; SYSTEMATICS; ABUNDANCE AB The Zoroasteridae comprise a small but widespread family of asteroids distributed throughout the deep sea. Although poorly understood, they are often collected in the hundreds, suggesting that they occupy important ecological roles. A phylogenetic analysis including 24 terminal taxa and 70 morphological characters was performed, resulting in a single most-parsimonious tree. The tree separated zoroasterids with open, reticulate skeletons (e.g. Myxoderma) as more basal than those with more heavily armored, imbricate skeletons (e.g. Zoroaster), which were more derived. In addition to agreement with established genera, a new genus is supported by the phylogeny as the sister taxon to Myxoderma. The cladistic analysis was performed in conjunction with a revisionary survey of zoroasterid species, resulting in taxonomic changes to species in nearly every genus. Bathymetric and physiographic shifts were observed between the reticulate and imbricate zoroasterid clades. Zoroasterids possess a single marginal plate series, which occurs in basal sister-group neoasteroids (crown-group asteroids). Phylogenetic results suggest that the morphololgical resemblance between zoroasterids and Palaeozoic taxa, such as Calliasterella, is convergent but a paraphyletic Zoroasteride cannot be rejected and remains consistent with basal crown-group affinities. Although the phylogenetic position of the Eocene Zoroaster aff. fulgens was not strongly supported, its presence within a derived cluster of Zoroaster spp. suggests a relatively recent (i.e. Cenozoic) diversification into the deep sea. Taxonomic revisions, and geographical and bathymetric range extensions are also included. (c) 2007 The Linnean Society of London. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Mah, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20560 USA. EM brisinga@gmail.com RI Mah, Christopher/B-5771-2008 NR 139 TC 16 Z9 18 U1 0 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAY PY 2007 VL 150 IS 1 BP 177 EP 210 DI 10.1111/j.1096-3642.2007.00291.x PG 34 WC Zoology SC Zoology GA 161CY UT WOS:000245993100006 ER PT J AU Anker, A Dworschak, PC AF Anker, Arthur Dworschak, Peter C. TI Jengalpheops rufus gen. nov., sp nov., a new commensal alpheid shrimp from the Philippines (Crustacea : Decapoda) SO ZOOLOGICAL STUDIES LA English DT Article DE Alpheidae; new genus; symbiosis; Callianassidae; Philippines ID SNAPPING SHRIMP; EDWARDSII AUDOUIN; SPECIES CRUSTACEA; CARIDEA; POTAMALPHEOPS; PACIFIC; ATHANAS; AUSTRALIA; MUDFLATS; BURROWS AB Jengalpheops rufus gen. nov., sp. nov., is described on the basis of several specimens collected on intertidal sand and mud flats of Panglao I., the Philippines. The uniformly reddish shrimps inhabit burrow mounds of the large callianas-sid mudshrimp, Glypturus armatus (A. Milne Edwards, 1870). Jengalpheops is defined mainly by the dorsally exposed eyestalks; the absence of orbital teeth; the short triangular rostrum; the unspecialized and feebly enlarged chelipeds, with comb-like rows of setae on the carpus and without snapping mechanism on the fingers; the 3rd maxilliped with styliform lateral plate; and the presence of strap-like epipods on the 1st to 4th pereiopods. The new genus appears to be relatively basal within the family, and is presumably most closely related to Potamalpheops Powell, 1979 and Stenalpheops Miya, 1997. C1 Smithsonian Trop Res Inst, Naos Unit 0948, Miami, FL 34002 USA. Nat Hist Museum, Zool Abt 3, A-1010 Vienna, Austria. RP Anker, A (reprint author), Smithsonian Trop Res Inst, Naos Unit 0948, APO AA, Miami, FL 34002 USA. EM ankera@si.edu; Peter.Dworschak@nhm-wien.ac.at RI Dworschak, Peter/O-4031-2015 OI Dworschak, Peter/0000-0003-4705-6426 NR 47 TC 11 Z9 13 U1 0 U2 2 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1021-5506 EI 1810-522X J9 ZOOL STUD JI Zool. Stud. PD MAY PY 2007 VL 46 IS 3 BP 290 EP 302 PG 13 WC Zoology SC Zoology GA 180IL UT WOS:000247356200004 ER PT J AU Knoll, AH Barnbach, RK Payne, JL Pruss, S Fischer, WW AF Knoll, Andrew H. Barnbach, Richard K. Payne, Jonathan L. Pruss, Sara Fischer, Woodward W. TI Paleophysiology and end-Permian mass extinction SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Review DE Permian; Triassic; mass extinction; physiology; paleontology ID WESTERN UNITED-STATES; TEMPERATURE-DEPENDENT BIOGEOGRAPHY; CENTRAL TRANSANTARCTIC MOUNTAINS; TRIASSIC SUPERANOXIC EVENT; THERMAL TOLERANCE; ATMOSPHERIC CO2; TERRESTRIAL ECOSYSTEMS; ENVIRONMENTAL-STRESS; MARINE INVERTEBRATE; OXYGEN LIMITATION AB Physiological research aimed at understanding current global change provides a basis for evaluating selective survivoyship associated with Permo-Triassic mass extinction. Comparative physiology links paleontological and palcoenvironmental observations, supporting the hypothesis that an end-Permian trigger, most likely Siberian Trap volcanism, touched off a set of physically-l inked perturbations that acted synergistically to disrupt the metabolisms of latest Permian organisms. Global wan-ning, anoxia, and toxic sulfide probably all contributed to end-Permian mass mortality, but hypercapnia (physiological effects of elevated P-CO2) best accounts for the selective survival of marine invertebrates. Paleophysiological perspectives further suggest that persistent or recurring hypercapnia/global warmth also played a principal role in delayed Triassic recovery. More generally, physiology provides an important way of paleobiological knowing in the age of Earth system science. (C) 2007 Elsevier B.V. All rights reserved. C1 Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Knoll, AH (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. EM aknoll@oeb.harvard.edu RI Payne, Jonathan/A-1240-2007; Payne, Jonathan/B-8088-2012 OI Payne, Jonathan/0000-0002-9601-3310; NR 135 TC 307 Z9 331 U1 14 U2 136 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD APR 30 PY 2007 VL 256 IS 3-4 BP 295 EP 313 DI 10.1016/j.epsl.2007.02.018 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 176CU UT WOS:000247061300001 ER PT J AU Labandeira, CC Allen, EG AF Labandeira, Conrad C. Allen, Emily G. TI Minimal insect herbivory for the Lower Permian Coprolite Bone Bed site of north-central Texas, USA, and comparison to other Late Paleozoic floras SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Review DE herbivorous taxa; Pteridospermae; leaves; paleoecology; diet; Parana Basin; Lower Permian; Late Paleozoic; insect herbivory ID PLANT ANIMAL INTERACTIONS; PENNSYLVANIAN TREE FERNS; EARLY HISTORY; WIND DAMAGE; LEAF MINES; ASSOCIATIONS; ARTHROPOD; PATTERNS; ILLINOIS; FORESTS AB An examination of 598 leaves from the Lower Permian (late Sakmarian) Coprolite Bone Bed (CBB) site in north-central Texas, USA, reveals low herbivory levels based on analyses of foliar surface-area removed (0.25%) and frequency of herbivorized leaves (15.6%). These values contrast with a similar study from a somewhat younger (mid-Artinskian) nearby site where analogous values are 2.55% and 31.8%, respectively. As at the younger site, when compared to all other co-occurring plant taxa, CBB pteridosperms were overwhelmingly herbivorized, particularly the peltasperm Autunia cf. conferta and the medullosan Odontopteris cf. fingulata, the latter preserving an exceptionally high herbivory level of 3.31%. These two host-plant taxa accounted for 96.8% of all herbivorized leaves and 96.4% of all leaf surface area removed by insects. For the bulk flora, four subgroups of feeding were documented: margin feeding (70.1% of all occurrences), hole feeding (24.1%), and minor skeletonization (earliest occurrence), and galling. Distinctive gall types, one on the midveinal region of A. cf. conferta and the other on a branchlet of Walchia piniformis (also occurring in the European Early Permian) add to an existing but depauperate insect gall record for the Pennsylvanian and Permian. Emerging evidence indicates that herbivory intensity was spatiotemporally heterogeneous across fluvially-associated landscapes during the Early Permian in both western Euramerica (Texas, USA) and western Gondwana (Parana Basin, Brazil), differing by an order of magnitude within each of these areas. Localities with the highest percentages of bulk leaf surface-area removed by herbivores in both realms ranged from 2.39 to 2.97%. This range approximates about a third of modem surface-area removal values by insect herbivores in both subtropical to tropical floras. (C) 2006 Elsevier B.V. All rights reserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Bryn Mawr Coll, Dept Comp Sci, Bryn Mawr, PA 19010 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM labandec@si.edu NR 155 TC 39 Z9 40 U1 2 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD APR 30 PY 2007 VL 247 IS 3-4 BP 197 EP 219 DI 10.1016/j.palaeo.2006.10.015 PG 23 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 163NS UT WOS:000246167300002 ER PT J AU Kratter, KM Carter, LM Campbell, DB AF Kratter, Kaitlin M. Carter, Lynn M. Campbell, Donald B. TI An expanded view of Lada Terra, Venus: New Arecibo radar observations of Quetzalpetlatl Corona and surrounding flows SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GLOBAL DISTRIBUTION; MAGELLAN; TECTONICS; VOLCANISM; FEATURES AB [ 1] Quetzalpetlatl, a corona approximately 800 km in diameter, lies in Lada Terra centered at 68 degrees S, 357 degrees E. It is characterized by vast, radar-bright lava flows stretching to the southeast for over 1500 km, covering a total area of nearly 600,000 km(2). Magellan SAR images covered most of the Quetzalpetlatl flow field, but 12.6 cm Arecibo radar data from March 2001 gives complete coverage of the region. With these new data, we examine the circular polarization properties of the Quetzalpetlatl flow field for comparison with other flows on Venus as well as terrestrial lava. Our analysis suggests that Quetzalpetlatl Corona is primarily a source for flows with 13-cm-scale roughness properties similar to terrestrial pahoehoe, and which appear to have traveled down a system of channels or tubes until reaching some unresolved topographic boundary. We also identify four new crater candidates. C1 Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Kratter, KM (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM kratter@astro.utoronto.ca RI Carter, Lynn/D-2937-2012 NR 21 TC 5 Z9 6 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD APR 26 PY 2007 VL 112 IS E4 AR E04008 DI 10.1029/2006JE002722 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 163FR UT WOS:000246144700001 ER PT J AU Butt, YM AF Butt, Yousaf M. TI Astrophysics - The answer is blowing in the wind SO NATURE LA English DT Editorial Material ID PARTICLE-ACCELERATION; SUPERBUBBLES; GALAXY; RAYS C1 Quaid I Azam Univ, Natl Ctr Phys, Islamabad, Pakistan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Butt, YM (reprint author), Quaid I Azam Univ, Natl Ctr Phys, Islamabad, Pakistan. EM ybutt@cfa.harvard.edu NR 13 TC 3 Z9 3 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 APR 26 PY 2007 VL 446 IS 7139 BP 986 EP 987 DI 10.1038/446986a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 160NU UT WOS:000245950400025 PM 17460649 ER PT J AU Cairns, SD AF Cairns, Stephen D. TI Studies on western Atlantic Octocorallia (Gorgonacea : Ellisellidae). Part 7: The genera Riisea Duchassaing & Michelotti, 1860 and Nicella Gray, 1870 SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID COELENTERATA AB The eleven western Atlantic species belonging to the two ellisellid genera Riisea and Nicella are described and illustrated. Six new species of Nicella are described, and another distinguished as new but not described. A dichotomous key and a table of comparisons is provided for the eleven western Atlantic species of Nicella. An annotated list of the 19 species of this genus is given. Detailed morphology of the double head sclerites and the type of body wall sclerite were used to distinguish species. Specimens of these genera were common at shelf and upper slope depths throughout the tropical western Atlantic, the deepest record being at 819 m. Specimens from 140 stations were examined as well as the types of all previously described species of western Atlantic Nicella. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA. EM cairnss@si.edu NR 36 TC 4 Z9 4 U1 1 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 25 PY 2007 VL 120 IS 1 BP 1 EP 38 DI 10.2988/0006-324X(2007)120[1:SOWAOG]2.0.CO;2 PG 38 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 163OB UT WOS:000246168300001 ER PT J AU Graves, GR AF Graves, Gary R. TI Diagnoses of hybrid hummingbirds (Aves : Trochilidae). 15. A new intergeneric hybrid (Hylocharis leucotis X Selasphorus platycercus) from the Huachuca Mountains, southeastern Arizona SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID HYBRIDIZATION; GOULD; HELIANGELUS; SYSTEMATICS; MULSANT; ORIGIN AB A hummingbird specimen collected by W. W. Brown in 1917 in the Huachuca Mountains, southeastern Arizona, is a hybrid of Hylocharis leucotis (white-eared hummingbird) X Selasphorus platycercus (broad-tailed hummingbird). Brown's specimen, which exhibits a blended mosaic of plumage characters of the presumed parental species, represents the first known instance of hybridization between species currently placed in Hylocharis and Selasphorus. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu NR 28 TC 5 Z9 5 U1 0 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 25 PY 2007 VL 120 IS 1 BP 99 EP 105 DI 10.2988/0006-324X(2007)120[99:DOHHAT]2.0.CO;2 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 163OB UT WOS:000246168300008 ER PT J AU Graves, GR AF Graves, Gary R. TI Diagnoses of hybrid hummingbirds (Aves : Trochilidae). 16. Characterization of a striking intergeneric hybrid (Lampornis clemencide X Calypte anna) from Ramsey Canyon, Huachuca Mountains, southeastern Arizona SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA Rumanian DT Article ID HELIANGELUS AB A hummingbird specimen from Ramsey Canyon, Huachuca Mountains, southeastern Arizona, represents a hybrid of Lampornis clemenciae (Blue-throated Hummingbird) X Calypte anna (Anna's Hummingbird). The specimen, which constitutes the only verified instance of hybridization between a species in the "mountain gem" group of hummingbirds and a species in the "bee" group, exhibits a blended mosaic of plumage characters of the parental species. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu NR 27 TC 3 Z9 3 U1 2 U2 6 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 25 PY 2007 VL 120 IS 1 BP 106 EP 112 DI 10.2988/0006-324X(2007)120[106:DOHHAT]2.0.CO;2 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 163OB UT WOS:000246168300009 ER PT J AU Hardcastle, MJ Evans, DA Croston, JH AF Hardcastle, M. J. Evans, D. A. Croston, J. H. TI Hot and cold gas accretion and feedback in radio-loud active galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; X-rays : galaxies ID ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLES; XMM-NEWTON OBSERVATIONS; 7C REDSHIFT SURVEY; X-RAY ENVIRONMENT; GALACTIC NUCLEI; ELLIPTIC GALAXIES; CHANDRA OBSERVATION; RELATIVISTIC MODEL; UNIFIED MODELS AB We have recently shown that X-ray observations of the population of 'low-excitation' radio galaxies, which includes most low-power, Fanaroff-Riley class I sources as well as some more powerful Fanaroff-Riley class II objects, are consistent with a model in which the active nuclei of these objects are not radiatively efficient at any waveband. In another recent paper, Allen et al. have shown that Bondi accretion of the hot, X-ray emitting phase of the intergalactic medium (IGM) is sufficient to power the jets of several nearby, low-power radio galaxies at the centres of clusters. In this paper, we combine these ideas and suggest that accretion of the hot phase of the IGM is sufficient to power all low-excitation radio sources, while high-excitation sources are powered by accretion of cold gas that is in general unrelated to the hot IGM. This model explains a number of properties of the radio-loud active galaxy population, and has important implications for the energy input of radio-loud active galactic nuclei into the hot phase of the IGM: the energy supply of powerful high-excitation sources does not have a direct connection to the hot phase. C1 Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hardcastle, MJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM mjh@star.herts.ac.uk RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 68 TC 194 Z9 194 U1 0 U2 4 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 APR 21 PY 2007 VL 376 IS 4 BP 1849 EP 1856 DI 10.1111/j.1365-2966.2007.11572.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156UP UT WOS:000245675700035 ER PT J AU Risaliti, G Elvis, M Fabbiano, G Baldi, A Zezas, A Salvati, M AF Risaliti, G. Elvis, M. Fabbiano, G. Baldi, A. Zezas, A. Salvati, M. TI Occultation measurement of the size of the X-ray-emitting region in the active galactic nucleus of NGC 1365 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual ( NGC 1365) ID BLACK-HOLES; NGC 1365; GALAXIES; SPECTRUM; LINES AB We present an occultation of the central X-ray-emitting region in the Seyfert galaxy NGC 1365. This extreme spectral variation (from Compton-thin to reflection-dominated and back to Compton-thin in 4 days) has been caught in a 10 day Chandra monitoring campaign consisting of six short (15 ks) observations performed every 2 days. We discuss the implications of this occultation within the scenario of a Compton-thick cloud crossing the line of sight of the X-ray source. We estimate a source size R <= 10(14) cm and a distance of the cloud from the source D <= 10(16) cm. This direct measurement confirms the theoretical expectations of an extremely compact X-ray source and shows that the Compton-thick circumnuclear gas is located at a distance from the center on the scale of the broad-line region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAF Osservatorio Arcetri, 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 NR 18 TC 80 Z9 80 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 2007 VL 659 IS 2 BP 111 EP 114 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EV UT WOS:000245775000008 ER PT J AU Lidz, A Zahn, O McQuinn, M Zaldarriaga, M Dutta, S Hernquist, L AF Lidz, Adam Zahn, Oliver McQuinn, Matthew Zaldarriaga, Matias Dutta, Suvendra Hernquist, Lars TI Higher order contributions to the 21 cm power spectrum SO ASTROPHYSICAL JOURNAL LA English DT Article DE theory; intergalactic medium; large-scale structure of universe ID LARGE-SCALE STRUCTURE; LOW-MASS GALAXIES; LY-ALPHA FOREST; HIGH-REDSHIFT; REIONIZATION OBSERVATORIES; HYDROGEN REIONIZATION; CENTIMETER TOMOGRAPHY; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; PERTURBATION-THEORY AB We consider the contribution of third- and fourth-order terms to the 21 cm power spectrum during the epoch of reionization, which arise because the 21 cm brightness temperature involves a product of the hydrogenic neutral fraction and the gas density. The third-order terms vanish for Gaussian random fields and have been previously neglected or ignored. We measure these terms from radiative transfer simulations and estimate them using cosmological perturbation theory. In our simulated models, the higher order terms are significant, and neglecting them leads to inaccurate 21 cm power spectrum estimates. On small scales the higher order terms are produced by gravitational mode coupling. Small-scale structure grows more readily in large-scale overdense regions, but the same regions tend to be ionized and hence do not contribute to the 21 cm signal. This modifies an earlier intuition that the 21 cm power spectrum simply traces the density power spectrum on scales smaller than that of a typical bubble and implies that small-scale measurements contain more information about the ionizing sources than previously believed. On large scales, higher order moments are not directly related to gravity. They are nonzero because overdense regions tend to ionize first and are important in magnitude at late times, due to large fluctuations in the neutral fraction. Finally, we show that second-order Lagrangian perturbation theory approximately reproduces the statistics of the density field from full numerical simulations for all redshifts and scales of interest, including the mode-coupling effects mentioned above. It can, therefore, be used in conjunction with semianalytic models to explore the broad regions of parameter space relevant for future 21 cm surveys. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Heidelberg, Inst Theoret Astrophys, D-69117 Heidelberg, Germany. Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP Lidz, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alidz@cfa.harvard.edu; ozahn@cfa.harvard.edu NR 41 TC 36 Z9 36 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 20 PY 2007 VL 659 IS 2 BP 865 EP 876 DI 10.1086/511670 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700001 ER PT J AU Hopkins, PF Bundy, K Hernquist, L Ellis, RS AF Hopkins, Philip F. Bundy, Kevin Hernquist, Lars Ellis, Richard S. TI Observational evidence for the coevolution of galaxy mergers, quasars, and the blue/red galaxy transition SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; galaxies : active; galaxies : evolution; quasars : general ID DIGITAL-SKY-SURVEY; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; QSO REDSHIFT SURVEY; DARK-MATTER HALOES; ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMATION HISTORY; ORIGINS DEEP SURVEY; LUMINOSITY FUNCTION; RED GALAXIES AB We compile a number of observations to estimate the time-averaged rate of formation or buildup of red sequence galaxies, as a function of mass and redshift. Comparing this with the mass functions of mergers and quasar hosts, and independently comparing their clustering properties as a function of redshift, we find that these populations trace the same mass distribution, with similar evolution, at redshifts 0 < z less than or similar to 1.5. Knowing one of the quasar, merger, or elliptical mass/luminosity functions, it is possible to predict the others. Allowing for greater model dependence, we compare the rate of early-type buildup with the implied merger and quasar triggering rates as a function of mass and redshift and find agreement. Over this redshift range, observed merger fractions can account for the entire bright quasar luminosity function and buildup of the red sequence at all but the highest masses at low redshift (greater than or similar to 10(11) M-circle dot at z less than or similar to 0.3) where "dry'' mergers appear to dominate. This supports a necessary prediction of theories where mergers between gas-rich galaxies produce ellipticals with an associated phase of quasar activity, after which the remnant becomes red. These populations trace a similar characteristic transition mass, possibly reflecting the mass above which the elliptical population is mostly (greater than or similar to 50%) assembled at a given redshift, which increases with redshift over the observed range in a manner consistent with suggestions that cosmic down sizing may apply to red galaxy assembly as well as star formation. These mass distributions as a function of redshift do not uniformly trace the all/red/blue galaxy population, ruling out models in which quasar activity is generically associated with star formation or is long lived in "old'' systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 187 TC 82 Z9 83 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2007 VL 659 IS 2 BP 976 EP 996 DI 10.1086/512091 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700010 ER PT J AU Kraft, RP Birkinshaw, M Hardcastle, MJ Evans, DA Croston, JH Worrall, DM Murray, SS AF Kraft, R. P. Birkinshaw, M. Hardcastle, M. J. Evans, D. A. Croston, J. H. Worrall, D. M. Murray, S. S. TI A radio through X-ray study of the hot spots, active nucleus, and environment of the nearby FR II radio galaxy 3C 33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (3C 33); galaxies : ISM; galaxies : jets; hydrodynamics; X-rays : galaxies : clusters ID MAGNETIC-FIELD STRENGTHS; XMM-NEWTON OBSERVATIONS; PARTICLE-ACCELERATION; CHANDRA OBSERVATIONS; SYNCHROTRON SPECTRA; GALACTIC NUCLEI; COMPLETE SAMPLE; 3C 33; EMISSION; LOBES AB We present results from Chandra ACIS-S, Spitzer, XMM-Newton, HST, and VLA observations of the radio hot spots, extended environment, and nucleus of the nearby (z = 0.0597) FR II radio galaxy 3C 33. This is a relatively low power FR II radio galaxy, so we expect, a priori, to detect a significant X-ray synchrotron component to the emission from the hot spots. We detect X-ray emission coincident with the two knots of polarized optical emission from the southern hot spot (SHS), as well as along the northwest arm of this hot spot. We also detect X-ray emission from two compact regions of the northern hot spot ( NHS), as well as diffuse emission behind the radio peak. The X-ray flux density of the region at the tip of the southern hot spot, the most compact radio feature of the southern lobe, is consistent with the synchrotron self-Compton (SSC) process. The X-ray flux densities of the other three regions of the SHS and the two compact regions of the NHS are an order of magnitude or more above the predictions from either the SSC or inverse Compton scattering of the CMB(IC/CMB) mechanisms, thus strongly disfavoring these scenarios unless they are far from equipartition (B similar to 4-14 times smaller than the equipartition values). We conclude that the X-ray emission is synchrotron emission from multiple populations of ultrarelativistic electrons. There must be complex, unresolved substructure within each region. The detection of X-ray emission from both hot spots combined with the large absorbing column toward the primary power-law component of the nucleus conclusively demonstrate that the jets must lie relatively close to the plane of the sky and that relativistic beaming cannot be important. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, 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 48 TC 25 Z9 26 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 2007 VL 659 IS 2 BP 1008 EP 1021 DI 10.1086/512766 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700012 ER PT J AU Krongold, Y Nicastro, F Elvis, M Brickhouse, N Binette, L Mathur, S Jimenez-Bailon, E AF Krongold, Yair Nicastro, Fabrizio Elvis, Martin Brickhouse, Nancy Binette, Luc Mathur, Smita Jimenez-Bailon, Elena TI The compact, conical, accretion-disk warm absorber of the Seyfert 1 galaxy NGC 4051 and its implications for IGM-galaxy feedback processes SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4051); galaxies : Seyfert ID ACTIVE GALACTIC NUCLEI; REFLECTION GRATING SPECTROMETER; NARROW-LINE REGION; XMM-NEWTON VIEW; X-RAY SPECTRUM; IONIZED-GAS; ELEMENTAL ABUNDANCES; ULTRAVIOLET ABSORBER; ABSORPTION-LINES; PHOTOIONIZED GAS AB Using a 100 ks XMM-Newton exposure of NGC 4051, we show that the time evolution of the ionization state of the X-ray absorbers in response to the rapid and highly variable X-ray continuum constrains all the main physical and geometrical properties of an AGN "warm absorber'' wind. The absorber consists of two different ionization components, with a difference of approximate to 100 in ionization parameter and approximate to 5 in column density. By tracking the response in the opacity of the gas to changes in the ionizing continuum, we were able to constrain the electron density of the system. We find n(e) (5.8-21.0) x 10(6) cm(-3) for the high-ionization absorber and n(e) > 8.1 x 10(7) cm(-3) for the low- ionization absorber. These densities require that the high- and low- ionization absorbing components of NGC 4051 must be compact, at distances 0.5-1.0 lt-days (2200R(S)-4400R(S)) and < 3.5 lt-days (< 15,800R(S)) from the continuum source, respectively. This rules out an origin in the dusty obscuring torus, as the dust sublimation radius is at least an order of magnitude larger (similar to 12 lt-days). An accretion-disk origin for the warm absorber wind is strongly suggested, and an association with the high- ionization, He II emitting, broad emission line region ( radius < 2 lt-days) is possible. The two detected phases are consistent with pressure equilibrium, which suggests that the absorber consists of a two- phase medium. A radial flow in a spherical geometry is unlikely, and a conical wind geometry is preferred. The implied mass outflow rate from this wind can be well constrained and is 2%-5% of the mass accretion rate. If the mass outflow rate scaling with accretion rate is representative of all quasars, our results imply that warm absorbers in powerful quasars are unlikely to produce important evolutionary effects on their larger environment, unless we are observing the winds before they get fully accelerated. Only in such a scenario can AGN winds be important for cosmic feedback. C1 Univ Nacl Autonoma Mexico, Dept Astrofis Extragalact & Cosmol, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Roma, INAF, I-00136 Rome, Italy. Ohio State Univ, Columbus, OH 43210 USA. Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. RP Krongold, Y (reprint author), Univ Nacl Autonoma Mexico, Dept Astrofis Extragalact & Cosmol, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. OI Nicastro, Fabrizio/0000-0002-6896-1364; Brickhouse, Nancy/0000-0002-8704-4473 NR 76 TC 116 Z9 116 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 APR 20 PY 2007 VL 659 IS 2 BP 1022 EP 1039 DI 10.1086/512476 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700013 ER PT J AU Argon, AL Greenhill, LJ Reid, MJ Moran, JM Humphreys, EML AF Argon, A. L. Greenhill, L. J. Reid, M. J. Moran, J. M. Humphreys, E. M. L. TI Toward a new geometric distance to the active galaxy NGC 4258. I. VLBI monitoring of water maser emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4258); galaxies : kinematics and dynamics; galaxies : nuclei; masers; techniques : interferometric ID LARGE-MAGELLANIC-CLOUD; HUBBLE-SPACE-TELESCOPE; CEPHEID DISTANCE; ACCRETION DISK; METALLICITY DEPENDENCE; FUNDAMENTAL PROPERTIES; ECLIPSING BINARIES; GALACTIC NUCLEI; ROTATING-DISK; KEY PROJECT AB We report a 3 yr, 18 epoch, VLBI monitoring study of H2O masers in the subparsec, warped, accretion disk within the NGC 4258 AGN. Our immediate goals are to trace the geometry of the underlying disk, track rotation via measurement of proper motion, and ascertain the radii of masers for which centripetal acceleration may be measured separately. The monitoring includes similar to 4 times as many epochs, similar to 3 times denser sampling, and tighter control over sources of systematic error than earlier VLBI investigations. Coverage of a similar to 2400 km s(-1) bandwidth has also enabled mapping of molecular material similar to 30% closer to the black hole than accomplished previously, which will strengthen geometric and dynamical disk models. Through repeated observation we have also measured for the first time a 5 mu as (1 sigma) thickness of the maser medium. Assuming that this corresponds to the thickness of the accretion disk, hydrostatic equilibrium requires a disk plane temperature of approximate to 600K. Our long-term goal is a geometric distance to NGC 4258 that is accurate to similar to 3%, a similar to 2 times improvement over the current best estimate. A geometric estimate of distance can be compared to distances obtained from analysis of Cepheid light curves, with the intent to recalibrate the extragalactic distance scale with reduced systematic uncertainties. This is the first paper in a series. We present here VLBI observations, data reduction, and temporal and spatial characteristics of the maser emission. Later papers will report estimation of orbital acceleration and proper motion, modeling of disk 3D geometry and dynamics, and estimation of a "maser distance.'' Estimation of a "Cepheid distance'' is presented in a parallel paper series. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Argon, AL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Moran, James/0000-0002-3882-4414 NR 45 TC 40 Z9 40 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 2007 VL 659 IS 2 BP 1040 EP 1062 DI 10.1086/512718 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700014 ER PT J AU Maughan, BJ Jones, C Jones, LR Van Speybroeck, L AF Maughan, B. J. Jones, C. Jones, L. R. Van Speybroeck, L. TI Deep XMM-Newton and Chandra observations of Cl J1226.9+3332: A detailed X-ray mass analysis of a z=0.89 galaxy cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : general; galaxies : clusters : individual (Cl J1226.9+3332); galaxies : high-redshift; intergalactic medium; X-rays : galaxies ID HIGH-REDSHIFT CLUSTER; ROSAT POINTED SURVEY; INTRACLUSTER MEDIUM; DARK ENERGY; COSMOLOGICAL PARAMETERS; TEMPERATURE; EVOLUTION; MERGER; SAMPLE; CONSTRAINTS AB Deep XMM-Newton and Chandra observations of Cl J1226.9+ 3332 at z = 0: 89 have enabled the most detailed X-ray mass analysis of any such high-redshift galaxy cluster. The XMM-Newton temperature profile of the system shows no sign of central cooling, with a hot core and a radially declining profile. A temperature map shows asymmetry with a hot region that appears to be associated with a subclump of galaxies at the cluster redshift but is not visible in the X-ray surface brightness. This is likely to be the result of a merger event in the cluster but does not appear to significantly affect the overall temperature profile. The XMM-Newton temperature profile and combined Chandra and XMM-Newton emissivity profile allowed precise measurements of the global properties of Cl J1226.9+3332. Within an overdensity radius of 500 times the critical density at z = 0.89 (R-500), we find kT 10.4 +/- 0.6 keV, Z = 0.16 +/- 0.05 Z(circle dot), and M = 5.2(-0.8)(+1.0) x 10(14) M-circle dot. We obtain profiles of the metallicity, entropy, cooling time, and gas fraction and find a high concentration parameter for the total density profile of the system. The global properties are compared with the local L-T and M- T relations, and we are able to make the first observational test of the predicted evolution of the Y-X-M-500 relation. We find that departures from these scaling relations are most likely caused by an underestimate of the total mass by similar to 30% in the X-ray hydrostatic mass analysis due to the apparent recent or ongoing merger activity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Maughan, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA. EM bmaughan@cfa.harvard.edu NR 61 TC 33 Z9 33 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 20 PY 2007 VL 659 IS 2 BP 1125 EP 1137 DI 10.1086/512669 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700020 ER PT J AU Wise, MW McNamara, BR Nulsen, PEJ Houck, JC David, LP AF Wise, M. W. McNamara, B. R. Nulsen, P. E. J. Houck, J. C. David, L. P. TI X-ray supercavities in the Hydra A cluster and the outburst history of the central galaxy's active nucleus SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : elliptical and lenticular, cD; intergalactic medium; X-rays : galaxies ID RADIO; GAS; CAVITIES; FEEDBACK; CHANDRA; LOBES; JETS AB A 227 ks Chandra X-ray image of the hot plasma in the Hydra A cluster has revealed an extensive cavity system. The system was created by a continuous outflow or a series of bursts from the nucleus of the central galaxy over the past 200-500 Myr. The cavities have displaced 10% of the plasma within a 300 kpc radius of the central galaxy, creating a swiss-cheese-like topology in the hot gas. The surface brightness decrements are consistent with empty cavities oriented within 40 degrees of the plane of the sky. The outflow has deposited upward of 10(61) ergs into the cluster gas, most of which was propelled beyond the inner similar to 100 kpc cooling region. The supermassive black hole has accreted at a rate of approximately 0.1-0.25 M-circle dot yr(-1) over this time frame, which is a small fraction of the Eddington rate of a similar to 10(9) M-circle dot black hole, but is dramatically larger than the Bondi rate. Given the previous evidence for a circumnuclear disk of cold gas in Hydra A, these results are consistent with the AGN being powered primarily by infalling cold gas. The cavity system is shadowed perfectly by 330 MHz radio emission. Such low-frequency synchrotron emission may be an excellent proxy for X-ray cavities and thus the total energy liberated by the supermassive black hole. C1 MIT, Kavli Inst, Cambridge, MA 02139 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ohio Univ, Inst Astrophys, Athens, OH 45701 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wise, MW (reprint author), MIT, Kavli Inst, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 23 TC 109 Z9 109 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 20 PY 2007 VL 659 IS 2 BP 1153 EP 1158 DI 10.1086/512767 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700022 ER PT J AU Raymond, JC Korreck, KE Sedlacek, QC Blair, WP Ghavamian, P Sankrit, R AF Raymond, J. C. Korreck, K. E. Sedlacek, Q. C. Blair, W. P. Ghavamian, P. Sankrit, R. TI The preshock gas of SN 1006 from Hubble space telescope advanced camera for surveys observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (SN 1006); shock waves; supernova remnants ID BALMER-DOMINATED SHOCKS; HIGH-RESOLUTION SPECTROSCOPY; SUPERNOVA-REMNANT; SN 1006; X-RAY; EMISSION; ACCELERATION; NORTHEAST; SPECTRUM; IMAGERY AB We derive the preshock density and scale length along the line of sight for the collisionless shock from a deep HST image that resolves the H alpha filament in SN 1006 and updated model calculations. The very deep ACS high-resolution image of the Balmer line filament in the northwest quadrant shows that 0: 25 cm(-3) <= n(0) <= 0.4 cm(-3) and that the scale along the line of sight is about 2 x 10(18) cm, while bright features within the filament correspond to ripples with radii of curvature less than 1/10 that size. The derived densities are within the broad range of earlier density estimates, and they agree well with the ionization timescale derived from the Chandra X-ray spectrum of a region just behind the optical filament. This provides a test for widely used models of the X-ray emission from SNR shocks. The scale and amplitude of the ripples are consistent with expectations for a shock propagating through interstellar gas with similar to 20% density fluctuations on parsec scales as expected from studies of interstellar turbulence. One bulge in the filament corresponds to a knot of ejecta overtaking the blast wave, however. The interaction results from the rapid deceleration of the blast wave as it encounters an interstellar cloud. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Baltimore, MD USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 38 TC 32 Z9 32 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 2007 VL 659 IS 2 BP 1257 EP 1264 DI 10.1086/512483 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700030 ER PT J AU Brown, PJ Dessart, L Holland, ST Immler, S Landsman, W Blondin, S Blustin, AJ Breeveld, A Dewangan, GC Gehrels, N Hutchins, RB Kirshner, RP Mason, KO Mazzali, PA Milne, P Modjaz, M Roming, PWA AF Brown, Peter J. Dessart, Luc Holland, Stephen T. Immler, Stefan Landsman, Wayne Blondin, Stephane Blustin, Alexander J. Breeveld, Alice Dewangan, Gulab C. Gehrels, Neil Hutchins, Robert B. Kirshner, Robert P. Mason, Keith O. Mazzali, Paolo A. Milne, Peter Modjaz, Maryam Roming, Peter W. A. TI Early ultraviolet, optical, and X-ray observations of the type IIPSN 2005cs in M51 with Swift SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M51); ultraviolet : general; X-rays : general ID PRELIMINARY SPECTRAL-ANALYSIS; II-P SUPERNOVAE; SN 2005CS; PLANETARY-NEBULAE; STANDARD CANDLES; STAR-FORMATION; DISTANCE; GALAXY; EMISSION; TELESCOPE AB We report early photospheric-phase observations of the Type IIP supernova ( SN) 2005cs obtained by the Swift ultraviolet-optical and X-ray telescopes. Observations started within 2 days of discovery and continued on a regular basis for 3 weeks. During this time the V-band magnitude remained essentially constant, while the UV was initially bright, but steadily faded until below the brightness of an underlying UV-bright H II region. This UV decay is similar to SNe II observed by the International Ultraviolet Explorer. UV grism spectra show the P Cygni absorption of Mg II 2798 8, indicating a photospheric origin of the UV flux. Based on non-LTE model atmosphere calculations with the CMFGEN code, we associate the rapid evolution of the UV flux with the cooling of the ejecta, the peak of the spectral energy distribution ( SED) shifting from similar to 700 angstrom on June 30 to similar to 1200 angstrom on July 5. Furthermore, the corresponding recombination of the ejecta, e. g., the transition from Fe III to Fe II, induces a considerable strengthening of metal line-blanketing at and above the photosphere, blocking more and more effectively this fading UV flux. SN 2005cs was not detected in the X-ray band, and the upper limit to the X-ray luminosity yields a limit to the mass-loss rate of the progenitor of M less than or similar to 1 x 10(-5) yr(-1) (v(w)/10 km s(-1)). Overall, Swift represents a unique opportunity to capture the early and fast evolution of Type II SNe in the UV, providing additional constraints on the reddening, the SED shortward of 4000 angstrom, and the ionization state and temperature of the photon-decoupling regions. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Xray Astrophys Branch, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. UCL, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Brown, PJ (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM pbrown@astro.psu.edu RI Gehrels, Neil/D-2971-2012 NR 57 TC 33 Z9 33 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2007 VL 659 IS 2 BP 1488 EP 1495 DI 10.1086/511968 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700046 ER PT J AU Walker, GAH Croll, B Kuschnig, R Walker, A Rucinski, SM Matthews, JM Guenther, DB Moffat, AFJ Sasselov, D Weiss, WW AF Walker, Gordon A. H. Croll, Bryce Kuschnig, Rainer Walker, Andrew Rucinski, Slavek M. Matthews, Jaymie M. Guenther, David B. Moffat, Anthony F. J. Sasselov, Dimitar Weiss, Werner W. TI The differential rotation of kappa(1) Ceti as observed by MOST SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : individual (kappa(1) Ceti, HD 20630); stars : late-type; stars : oscillations; stars : rotation; stars : spots ID MAIN-SEQUENCE STARS; PHOTOMETRY; TIME; EVOLUTION; MODEL; SUN AB We first reported evidence for differential rotation of kappa(1) Ceti in Paper I. In this paper we demonstrate that the differential rotation pattern closely matches that for the Sun. This result is based on additional MOST observations in 2004 and 2005, as well as those from 2003. Using StarSpotz, a program developed specifically to analyze MOST photometry, we have solved for k, the differential rotation coefficient, and P-eq, the equatorial rotation period using the light curves from all three years. The absolute range in spot latitudes is 10 degrees-75 degrees and k = 0.090(-0.005)(+0.006), less than the solar value but consistent with the younger age of the star; k is also well constrained by the independent spectroscopic estimate of v sin i. We demonstrate independently that the pattern of differential rotation with latitude is indeed solar. Details are given of the parallel tempering formalism used in finding the most robust solution, which gives P-eq = 8.77(-0.04)(+0.03) days, smaller than that usually adopted, implying an age < 750 My. Our values of P-eq and k can explain the range of rotation periods others have found by spots or activity at a variety of latitudes. Historically, Ca II activity seems to occur consistently between latitudes 50 degrees and 60 degrees, which might indicate a permanent magnetic feature. Knowledge of k and P-eq is key to understanding the dynamo mechanism and rotation structure in the convective zone, as well assessing age for solar-type stars. We recently published values of k and P-eq for epsilon Eri based on MOST photometry and expect to analyze MOST light curves for several more spotted, solar-type stars. C1 Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Mont Megant Astron Observ, Notre Dame Des Bois, PQ J0B 2E0, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Walker, GAH (reprint author), 1234 Hewlett Pl, Victoria, BC V8S 4P7, Canada. EM gordonwa@uvic.ca; croll@astro.utoronto.ca; kuschnig@phas.ubc.ca; arwalker@sumusltd.com; rucinski@astro.utoronto.ca; matthews@phas.ubc.ca; guenther@ap.stmarys.ca; moffat@astro.umontreal.ca; sasselov@cfa.harvard.edu; weiss@astro.univie.ac.at NR 33 TC 50 Z9 50 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 2007 VL 659 IS 2 BP 1611 EP 1622 DI 10.1086/511851 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700057 ER PT J AU van Ballegooijen, AA Mackay, DH AF van Ballegooijen, A. A. Mackay, D. H. TI Model for the coupled evolution of subsurface and coronal magnetic fields in solar active regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun : activity; Sun : corona; Sun : magnetic fields ID 3-DIMENSIONAL CONVECTING FLOW; EMERGING FLUX TUBES; LARGE-SCALE CORONA; FILAMENT CHANNELS; HEMISPHERIC PATTERN; DYNAMIC EVOLUTION; DRIVEN EVOLUTION; CURRENT HELICITY; MASS EJECTIONS; TRANSPORT AB According to Babcock's theory of the solar dynamo, bipolar active regions are Omega-shaped loops emerging from a toroidal field located near the base of the convection zone. In this paper, a mean field model for the evolution of a twisted Omega-loop is developed. The model describes the coupled evolution of the magnetic field in the convection zone and the corona after the loop has fully emerged into the solar atmosphere. Such a coupled evolution is required to fully understand what happens to the coronal and subsurface fields as magnetic flux cancels at polarity inversion lines on the photosphere. The jump conditions for the magnetic field at the photosphere are derived from the magnetic stress balance between the convection zone and corona. The model reproduces the observed spreading of active region magnetic flux over the solar surface. At polarity inversion lines, magnetic flux submerges below the photosphere, but the component of magnetic field along the inversion line cannot submerge, because the field in the upper convection zone is nearly radial. Therefore, magnetic shear builds up in the corona above the inversion line, which eventually leads to a loss of equilibrium of the coronal fields and the "lift-off" of a coronal flux rope. Fields that submerge are transported back to the base of the convection zone, leading to the repair of the toroidal flux rope. Following Martens and Zwaan, interactions between bipoles are also considered. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 91 TC 32 Z9 32 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 2007 VL 659 IS 2 BP 1713 EP 1725 DI 10.1086/512849 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700066 ER PT J AU Bensch, F Bergin, EA AF Bensch, F. Bergin, E. A. TI The pure rotational line emission of ortho-water vapor in comets. I. Radiative transfer model (vol 615, pg 531, 2004) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Bensch, F (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. NR 1 TC 1 Z9 1 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 20 PY 2007 VL 659 IS 2 BP 1795 EP 1799 DI 10.1086/512724 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158ES UT WOS:000245774700075 ER PT J AU Hao, H Stanek, KZ Dobrzycki, A Matheson, T Bentz, MC Kuraszkiewicz, J Garnavich, PM Howk, JC Calkins, ML Worthey, G Modjaz, M Serven, J AF Hao, H. Stanek, K. Z. Dobrzycki, A. Matheson, T. Bentz, M. C. Kuraszkiewicz, J. Garnavich, P. M. Howk, J. C. Calkins, M. L. Worthey, G. Modjaz, M. Serven, J. TI Strongly variable z=1.48 FeII and MgII absorption in the spectra of z=4.05 GRB 060206 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; gamma rays : bursts; intergalactic medium ID RAY BURST AFTERGLOWS; LYMAN-ALPHA SYSTEMS; HIGH-REDSHIFT; SIGHT; LINES; ABSORBERS; EVOLUTION; ABUNDANCE; GAS AB We report on the discovery of strongly variable Fe ii and Mg ii absorption lines seen at z = 1.48 in the spectra of the z = 4.05 of the GRB 060206 obtained between 4.13 and 7.63 hr (observer frame) after the burst. In particular, the Fe ii line equivalent width (EW) decayed rapidly from 1.72 +/- 0.25 angstrom to 0.28 +/- 0.21 angstrom only to increase to 0.96 +/- 0.21 angstrom in a later spectrum. The Mg ii doublet shows even more complicated evolution: the weaker line of the doublet drops from 2.05 +/- 0.25 angstrom to 0.92 +/- 0.32 angstrom but then more than doubles to 2.47 +/- 0.41 angstrom in later data. The ratio of the EWs for the Mg ii doublet is also variable, being closer to 1 : 1 (saturated regime) when the lines are stronger and becoming closer to 2 : 1 (unsaturated regime) when the lines are weaker, consistent with expectations based on atomic physics. We have investigated and rejected the possibility of any instrumental or atmospheric effects causing the observed strong variations. Our discovery of clearly variable intervening Fe ii and Mg ii lines immediately indicates that the characteristic size of intervening patches of Mg ii "clouds" is comparable to the GRB beam size, i.e., about 10(16) cm. We discuss various implications of this discovery, including the nature of the Mg ii absorbers, the physics of GRBs, and measurements of chemical abundances from GRB and quasar absorption lines. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. European So Observ, D-85748 Garching, Germany. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. FL Whipple Observ, Amado, AZ 85645 USA. Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. RP Hao, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hhao@cfa.harvard.edu; kstanek@astronomy.ohio-state.edu; adam.dobrzycki@eso.org; matheson@noao.edu; bentz@astronomy.ohio-state.edu; jkuraszkiewicz@cfa.harvard.edu; pgarnavi@nd.edu; jhowk@nd.edu; mcalkins@cfa.harvard.edu; gworthey@wsu.edu; mmodjaz@cfa.harvard.edu; jdogg@wsu.edu RI Howk, Jay/D-2577-2013; OI Howk, J. Christopher/0000-0002-2591-3792 NR 28 TC 28 Z9 28 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 20 PY 2007 VL 659 IS 2 BP L99 EP L102 DI 10.1086/518032 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EV UT WOS:000245775000005 ER PT J AU Kiss, LL Szekely, P Bedding, TR Bakos, GA Lewis, GF AF Kiss, L. L. Szekely, P. Bedding, T. R. Bakos, G. A. Lewis, G. F. TI A wide-field kinematic survey for tidal tails around five globular clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy : halo; galaxy : kinematics and dynamics; galaxy : structure globular; clusters : general ID PHOTOMETRIC STANDARD STARS; CELESTIAL EQUATOR; OMEGA-CENTAURI; PALOMAR-5; EVOLUTION; DISCOVERY; NGC-5466; TIDES AB Using the AAOmega instrument of the Anglo-Australian Telescope, we have obtained medium-resolution near-infrared spectra of 10,500 stars in 2 degrees fields centered on the galactic globular clusters 47 Tuc, NGC 288, M12, M30, and M55. Radial velocities and equivalent widths of the infrared Ca II triplet lines have been determined to constrain cluster membership, which in turn has been used to study the angular extent of the clusters. From the analysis of 140-1000 member stars in each cluster, we do not find extended structures that go beyond the tidal radii. For three cluster we estimate a 1% upper limit of extratidal red giant branch stars. We detect systemic rotation in 47 Tuc and M55. C1 Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kiss, LL (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RI Kiss, Laszlo/A-2539-2008; Lewis, Geraint/F-9069-2015; OI Lewis, Geraint/0000-0003-3081-9319; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661 NR 26 TC 13 Z9 13 U1 1 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 20 PY 2007 VL 659 IS 2 BP L129 EP L132 DI 10.1086/517971 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EV UT WOS:000245775000012 ER PT J AU Lee, JJ Koo, BC Raymond, J Ghavamian, P Pyo, TS Tajitsu, A Hayashi, M AF Lee, Jae-Joon Koo, Bon-Chul Raymond, John Ghavamian, Parviz Pyo, Tae-Soo Tajitsu, Akito Hayashi, Masahiko TI Subaru HDS observations of a Balmer-dominated shock in Tycho's supernova remnant SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G120.1 ~ 1.4, Tycho); line : profiles; shock waves; supernova remnants ID HIGH-RESOLUTION SPECTROSCOPY; COSMIC-RAY ACCELERATION; OPTICAL-EMISSION; CYGNUS LOOP; HIGH-ENERGY; NOVA; RCW-86; CLOUD; WAVE AB We present an Ha spectral observation of a Balmer-dominated shock on the eastern side of Tycho's supernova remnant using the Subaru Telescope. Utilizing the High Dispersion Spectrograph (HDS), we measure the spatial variation of the line profile between preshock and postshock gas. Our observation clearly shows a broadening and centroid shift of the narrow-component postshock H alpha line relative to the H alpha emission from the preshock gas. The observation supports the existence of a thin precursor where gas is heated and accelerated ahead of the shock. Furthermore, the spatial profile of the emission ahead of the Balmer filament shows a gradual gradient in the H alpha intensity and line width ahead of the shock. We propose that this region (similar to 10(16) cm) is likely to be the spatially resolved precursor. The line width increases from similar to 30 up to similar to 45 km s(-1), and its central velocity shows a redshift of similar to 5 km s(-1) across the shock front. The characteristics of the precursor are consistent with a cosmic-ray precursor, although the possibility of a fast neutral precursor is not ruled out. C1 Seoul Natl Univ, Astron Program, Dept Phys & Astron, Seoul 151742, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. RP Lee, JJ (reprint author), Seoul Natl Univ, Astron Program, Dept Phys & Astron, Seoul 151742, South Korea. EM jjlee@astro.snu.ac.kr NR 19 TC 24 Z9 24 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 2007 VL 659 IS 2 BP L133 EP L136 DI 10.1086/517520 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EV UT WOS:000245775000013 ER PT J AU Pohl, MED Piperno, DR Pope, KO Jones, JG AF Pohl, Mary E. D. Piperno, Dolores R. Pope, Kevin O. Jones, John G. TI Microfossil evidence for pre-Columbian maize dispersals in the neotropics from San Andres, Tabasco, Mexico SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE phytoliths; pollen; paleoecology; radiocarbon ID ZEA-MAYS L.; HUMAN DISTURBANCE; COASTAL ECUADOR; TROPICAL FOREST; COB PHYTOLITHS; AMAZON BASIN; AGRICULTURE; PANAMA; EVOLUTION; TEOSINTE AB The history of maize (Zea mays L.) is one of the most debated topics in New World archaeology. Molecular and genetic studies indicate that maize domestication took place in tropical southwest Mexico. Although archaeological evidence for the evolution of maize from its wild ancestor teosinte has yet to be found in that poorly studied region, other research combining paleclecology and archaeology is documenting the nature and timing of maize domestication and dispersals. Here we report a phytolith analysis of sediments from San Andres, Tabasco, that confirms the spread of maize cultivation to the tropical Mexican Gulf Coast > 7,000 years ago (approximate to 7,300 calendar years before present). We review the different methods used in sampling, identifying, and dating fossil maize remains and compare their strengths and weaknesses. Finally, we examine how San Andres amplifies the present evidence for widespread maize dispersals into Central and South America. Multiple data sets from many sites indicate that maize was brought under cultivation and domesticated and had spread rapidly out of its domestication cradle in tropical southwest Mexico by the eighth millennium before the present. C1 Florida State Univ, Dept Anthropol, Tallahassee, FL 32306 USA. Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. Smithsonian Trop Res Inst, Balboa 084303092, Panama. Geo Eco Arc Res, Garrett Pk, MD 20896 USA. Washington State Univ, Dept Anthropol, Pullman, WA 99164 USA. RP Pohl, MED (reprint author), Florida State Univ, Dept Anthropol, Tallahassee, FL 32306 USA. EM mpohl@mailer.fsu.edu NR 63 TC 49 Z9 54 U1 0 U2 8 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 17 PY 2007 VL 104 IS 16 BP 6870 EP 6875 DI 10.1073/pnas.0701425104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 159ME UT WOS:000245869200068 PM 17426147 ER PT J AU Staines, CL AF Staines, C. L. TI A review of the genus Bruchia Weise 1906 (Coleoptera : Chrysomelidae : Cassidinae) SO ZOOTAXA LA English DT Review DE Chrysomelidae; Cassidinae; Bruchia; new species; key AB The species of Bruchia are reviewed. Bruchia armata from Brazil, Colombia and Peru, and B. scapularis from Colombia are described as new. Each species is described and illustrated and a key to the species is provided. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, Washington, DC 20013 USA. RP Staines, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, POB 37012, Washington, DC 20013 USA. EM stainesc@si.edu NR 20 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 16 PY 2007 IS 1449 BP 45 EP 50 PG 6 WC Zoology SC Zoology GA 156VU UT WOS:000245678800003 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI World bank. Atlas of global development: A visual guide to the world's greatest challenges. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 15 PY 2007 VL 132 IS 7 BP 120 EP 120 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 160ID UT WOS:000245933200265 ER PT J AU Faisal, FHM AF Faisal, F. H. M. TI Gauge-invariant intense-field approximations to all orders SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article AB We present a gauge-invariant formulation of the so-called strong-field KFR approximations in the 'velocity' and 'length' gauges and demonstrate their equivalence in all orders. The theory thus overcomes a longstanding discrepancy between the strong-field velocity and the length-gauge approximations for non-perturbative processes in intense laser fields. C1 Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Faisal, FHM (reprint author), Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany. NR 9 TC 24 Z9 25 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, 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 2007 VL 40 IS 7 BP F145 EP F155 DI 10.1088/0953-4075/40/7/F02 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 161JG UT WOS:000246010100002 ER PT J AU Copperwheat, C Cropper, M Soria, R Wu, K AF Copperwheat, Christopher Cropper, Mark Soria, Roberto Wu, Kinwah TI Irradiation models for ULXs and fits to optical data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; X-rays : galaxies; X-rays : stars ID X-RAY SOURCES; MASS BLACK-HOLES; QUASI-PERIODIC OSCILLATIONS; NEARBY SPIRAL GALAXIES; SOURCE NGC-1313 X-2; HOLMBERG-IX X-1; CATACLYSMIC BINARIES; ACCRETION DISK; COUNTERPART; EMISSION AB We have constructed a model which describes the optical emission from ultraluminous X-ray sources (ULXs), and have used it to constrain the parameters of seven ULX systems. Our model assumes a binary nature for ULXs, and accounts for optical emission from an X-ray-irradiated companion star and accretion disc. We apply our model to six different ULX optical counterparts observed with the Hubble Space Telescope, and one observed with the ESO VLT, and determine the mass, radius and age of the donor stars in these systems. In addition, we obtained constraints for the black hole (BH) mass in some cases. We use the mass accretion rate implied by the X-ray luminosity of these sources as an additional constraint on the donor star, by assuming the mass transfer is driven by the stellar nuclear evolution. We find that in general the donors are older and less massive than previously thought, and are consistent with being of spectral type B. We discuss how these results affect our understanding of the evolution and history of ULXs. Where we can constrain the BH masses, we find them to be consistent with stellar mass BHs or intermediate mass BHs of order similar to 100 M(circle dot). We make predictions for future observations of optical/infrared ULX counterparts, calculating binary periods for different BH masses in each of the seven sources. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Copperwheat, C (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM cmc@mssl.ucl.ac.uk RI Cropper, Mark/C-1574-2008 NR 55 TC 26 Z9 26 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 APR 11 PY 2007 VL 376 IS 3 BP 1407 EP 1423 DI 10.1111/j.1365-2966.2007.11551.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 155YN UT WOS:000245614800046 ER PT J AU Kim, M Wilkes, BJ Kim, DW Green, PJ Barkhouse, WA Lee, MG Silverman, JD Tananbaum, HD AF Kim, Minsun Wilkes, Belinda J. Kim, Dong-Woo Green, Paul J. Barkhouse, Wayne A. Lee, Myung Gyoon Silverman, John D. Tananbaum, Harvey D. TI Chandra multiwavelength project X-ray point source number counts and the cosmic X-ray background SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; methods : data analysis; surveys; X-rays : diffuse background; X-rays : general ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; HELLAS2XMM SURVEY; SOURCE CATALOG AB We present the Chandra Multiwavelength Project (ChaMP) X-ray point source number counts and cosmic X-ray background (CXRB) flux densities in multiple energy bands. From the ChaMP X-ray point source catalog, similar to 5500 sources are selected, covering 9.6 deg(2) in sky area. To quantitatively characterize the sensitivity and completeness of the ChaMP sample, we perform extensive simulations. We also include the ChaMP+CDFs ( Chandra Deep Fields) number counts to cover large flux ranges from 2; 10(-17) to 2.4 x 10(-12) (0.5-2 keV) and from 2; 10(-16) to 7: 1; 10(-12) (2-8 keV) ergs cm(-2) s(-1). The ChaMP and the ChaMP+CDFs differential number counts are well fitted with a broken power law. The best-fit faint and bright power indices are 1: 49 +/- 0: 02 and 2: 36 +/- 0: 05 (0.5-2 keV), and 1: 58 +/- 0: 01 and 2.59(-0.05)(+0.06) (2-8 keV), respectively. We detect breaks in the differential number counts that appear at different fluxes in different energy bands. Assuming a single power-law model for a source spectrum, we find that the same population(s) of soft X-ray sources causes the break in the differential number counts for all energy bands. We measure the resolved CXRB flux densities from the ChaMP and the ChaMP+CDFs number counts with and without bright target sources. By adding the known unresolved CXRB to the ChaMP+CDF resolved CXRB, we also estimate total CXRB flux densities. The fractions of the resolved CXRB without target sources are 78% +/- 1% and 81% +/- 2% in the 0.5-2 and 2-8 keV bands, respectively, somewhat lower than but generally consistent with earlier numbers because of their large errors. These fractions increase by similar to 1% when target sources are included. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Max Planck Inst Extraterr Phys, Garching, Germany. RP Kim, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 34 TC 67 Z9 67 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 10 PY 2007 VL 659 IS 1 BP 29 EP 51 DI 10.1086/511630 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300002 ER PT J AU Webb, TMA Tran, KVH Lilly, SJ van der Werf, P AF Webb, T. M. A. Tran, K.-V. H. Lilly, S. J. van der Werf, P. TI Deep submillimeter observations of two Ly alpha-emitting galaxies at z similar to 6.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : formation; galaxies : high redshift; galaxies : starburst; submillimeter ID LYMAN-BREAK GALAXIES; 14 HOUR FIELD; CLERK-MAXWELL-TELESCOPE; SPITZER-SPACE-TELESCOPE; STAR-FORMATION HISTORY; HIGH-REDSHIFT; INFRARED GALAXIES; SPECTROSCOPIC CONFIRMATION; SOURCE IDENTIFICATIONS; FORMATION RATES AB We present deep submillimeter imaging of two spectroscopically confirmed z similar to 6.5 Ly alpha emitters (LAEs) in the Subaru Deep Field. Although we reach the nominal confusion limit at 850 mu m, neither LAE is detected at 850 or 450 mu m; thus, we conclude that the LAEs do not contain large dust masses (< 2.3; 10(8) and < 5.7; 10(8) M-circle dot). The limit on their average L-FIR/L-UV ratios (less than or similar to 35) is substantially lower than seen for most submillimeter-selected galaxies at z similar to 3 and is within the range of values exhibited by Lyman break galaxies. We place upper limits on their individual star formation rates of less than or similar to 248 and less than or similar to 613 M-circle dot yr(-1), and on the cosmic star formation rate density of the z similar to 6: 5 LAE population of less than or similar to 5.0; 10(-2) M-circle dot yr(-1) Mpc(-3). In the two submillimeter pointings, we also serendipitously detect seven sources at 850 mu m that we estimate to lie at 1 < z < 5. C1 McGill Univ, Dept Phys, Montreal, PQ, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. ETH, Astron Inst, Zurich, Switzerland. RP Webb, TMA (reprint author), McGill Univ, Dept Phys, Montreal, PQ, Canada. NR 72 TC 3 Z9 3 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 APR 10 PY 2007 VL 659 IS 1 BP 76 EP 83 DI 10.1086/510061 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300005 ER PT J AU Riess, AG Strolger, LG Casertano, S Ferguson, HC Mobasher, B Gold, B Challis, PJ Filippenko, AV Jha, S Li, WD Tonry, J Foley, R Kirshner, RP Dickinson, M MacDonald, E Eisenstein, D Livio, M Younger, J Xu, C Dahlen, T Stern, D AF Riess, Adam G. Strolger, Louis-Gregory Casertano, Stefano Ferguson, Henry C. Mobasher, Bahram Gold, Ben Challis, Peter J. Filippenko, Alexei V. Jha, Saurabh Li, Weidong Tonry, John Foley, Ryan Kirshner, Robert P. Dickinson, Mark MacDonald, Emily Eisenstein, Daniel Livio, Mario Younger, Josh Xu, Chun Dahlen, Tomas Stern, Daniel TI New hubble space telescope discoveries of type Ia supernovae at z >= 1: Narrowing constraints on the early behavior of dark energy SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : observations; distance scale; galaxies : distances and redshifts; supernovae : general ID HIGH-REDSHIFT SUPERNOVAE; ANISOTROPY-PROBE OBSERVATIONS; DIGITAL SKY SURVEY; COSMOLOGICAL CONSTANT; ACCELERATING UNIVERSE; INTERGALACTIC DUST; OPTICAL-SPECTRA; ADVANCED CAMERA; POWER-SPECTRUM; LEGACY SURVEY AB We have discovered 21 new Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to trace the history of cosmic expansion over the last 10 billion yr. These objects, which include 13 spectroscopically confirmed SNe Ia at z >= 1, were discovered during 14 epochs of reimaging of the GOODS fields North and South over 2 yr with the Advanced Camera for Surveys on HST. Together with a recalibration of our previous HST-discovered SNe Ia, the full sample of 23 SNe Ia at z >= 1 provides the highest redshift sample known. Combining these data with previous SN Ia data sets, we measured H (z) at discrete, uncorrelated epochs, reducing the uncertainty of H (z > 1) from 50% to under 20%, strengthening the evidence for a cosmic jerk - the transition from deceleration in the past to acceleration in the present. The unique leverage of the HST high-redshift SNe Ia provides the first meaningful constraint on the dark energy equation-of-state parameter at z >= 1. The result remains consistent with a cosmological constant [w (z) d - 1] and rules out rapidly evolving dark energy (dw/dz > 1). The defining property of dark energy, its negative pressure, appears to be present at z > 1, in the epoch preceding acceleration, with similar to 98% confidence in our primary fit. Moreover, the z > 1 sample-averaged spectral energy distribution is consistent with that of the typical SN Ia over the last 10 Gyr, indicating that any spectral evolution of the properties of SNe Ia with redshift is still below our detection threshold. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Univ Arizona, Steward Observ, Tucson, AZ USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Riess, AG (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NR 104 TC 984 Z9 991 U1 4 U2 30 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 2007 VL 659 IS 1 BP 98 EP 121 DI 10.1086/510378 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300007 ER PT J AU Jha, S Riess, AG Kirshner, RP AF Jha, Saurabh Riess, Adam G. Kirshner, Robert P. TI Improved distances to type Ia supernovae with multicolor light-curve shapes: MLCS2k2 SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : observations; distance scale; galaxies : distances and redshifts; supernovae : general ID HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT SUPERNOVAE; INFRARED PHOTOMETRY; ULTRAVIOLET EXTINCTION; HOST GALAXY; COSMOLOGICAL CONSTANT; OPTICAL PHOTOMETRY; INTERSTELLAR DUST; PRECISE DISTANCE; MAGELLANIC-CLOUD AB We present an updated version of the multicolor light-curve shape method to measure distances to Type Ia supernovae (SNe Ia), incorporating new procedures for K-correction and extinction corrections. We also develop a simple model to disentangle intrinsic color variations and reddening by dust and expand the method to incorporate U-band light curves and to more easily accommodate prior constraints on any of the model parameters. We apply this method to 133 nearby SNe Ia, including 95 objects in the Hubble flow ( cz >= 2500 km s(-1)), which give an intrinsic dispersion of less than 7% in distance. The Hubble flow sample, which is of critical importance to all cosmological uses of SNe Ia, is the largest ever presented with homogeneous distances. We find that the Hubble flow SNe with H(0)d(SN) >= 7400 km s(-1) yield an expansion rate that is 6.5% +/- 1.8% lower than the rate determined from SNe within that distance, and this can have a large effect on measurements of the dark energy equation of state with SNe Ia. Peculiar velocities of SN Ia host galaxies in the rest frame of the Local Group are consistent with the dipole measured in the cosmic microwave background. Direct fits of SNe Ia that are significantly reddened by dust in their host galaxies suggest that their mean extinction law may be described by R-V similar or equal to 2: 7, but optical colors alone provide weak constraints on R-V. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Berkeley, Miller Inst, Berkeley, CA 94720 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jha, S (reprint author), Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. EM saurabh@slac.stanford.edu NR 114 TC 412 Z9 415 U1 1 U2 19 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 2007 VL 659 IS 1 BP 122 EP 148 DI 10.1086/512054 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300008 ER PT J AU Iono, D Wilson, CD Takakuwa, S Yun, MS Petitpas, GR Peck, AB Ho, PTP Matsushita, S Pihlstrom, YM Wang, Z AF Iono, Daisuke Wilson, Christine D. Takakuwa, Shigehisa Yun, Min S. Petitpas, Glen R. Peck, Alison B. Ho, Paul T. P. Matsushita, Satoki Pihlstrom, Ylva M. Wang, Zhong TI High-resolution imaging of warm and dense molecular gas in the nuclear region of the luminous infrared galaxy NGC 6240 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : formation; galaxies : individual ( NGC 6240); galaxies : interactions; galaxies : kinematics and dynamics; galaxies : starburst ID ACTIVE GALACTIC NUCLEUS; BLACK-HOLES; SPACE-TELESCOPE; STAR-FORMATION; NGC 6240; ULTRALUMINOUS GALAXIES; SUBMILLIMETER GALAXIES; ROTATIONAL-EXCITATION; INTERSTELLAR-MEDIUM; STARBURST GALAXIES AB We present similar to 2" resolution CO (3-2), HCO+(4-3), and 880 mu m continuum images of the luminous infrared galaxy NGC 6240 obtained at the Submillimeter Array. We find that the spatially resolved CO (3-2), HCO+ (4-3), and the 880 mu m emission peaks between the two nuclear components that are both known to harbor AGNs. Our large velocity gradient (LVG) analysis performed on each velocity channel suggests that the peak of the molecular gas emission traced in our observations is warm (T = 20-100 K), dense (n(H2) 10(5.0)-10(5.4) cm(-3)), and moderately optically thin (tau = 0.2-2) in the central 1 kpc. We also find large column densities of similar to 10(23) cm(-2). Such extreme conditions are observed over similar to 300 km s(-1) centered around the CO-derived systemic velocity. The derived molecular gas mass from the CO (3-2) emission and a CO-to-H-2 conversion factor commonly used for ULIRGs is (6.9 +/- 1.7) x 10(9) M-circle dot, and this is consistent with the mass derived from previous CO(2-1) observations. The gas is highly turbulent in the central kpc ( Delta nu(FWZI) similar to 1175 km s(-1)). Furthermore, possible inflow or outflow activity is suggested from the CO (3-2) velocity distribution. We tentatively state that 3. 5 x 10(8) M-circle dot of isolated CO (3-2) emission seen west of the northern disk may be associated with outflows from starburst superwinds, but the gas outflow scenario from one of the central AGN is not completely ruled out. Piecing all of the information together, the central region of NGC 6240 harbors 2 AGNs, similar to 10(10) M-circle dot of molecular gas mass, 5 x 10(7) M-circle dot of dust mass, and has possible evidence of inflow and outflow activity. C1 Natl Astron Observ Japan, Mitaka, Tokyo 1810015, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Iono, D (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan. EM d.iono@nao.ac.jp NR 73 TC 50 Z9 50 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2007 VL 659 IS 1 BP 283 EP 295 DI 10.1086/512362 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300023 ER PT J AU Reid, MJ Menten, KM Trippe, S Ott, T Genzel, R AF Reid, M. J. Menten, K. M. Trippe, S. Ott, T. Genzel, R. TI The position of Sagittarius A*. III. Motion of the stellar cusp SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy : center; masers; stars : AGB and post-AGB; stars : variables : other ID SUPERMASSIVE BLACK-HOLE; OH IR STARS; GALACTIC-CENTER; PROPER-MOTION; MILKY-WAY; RADIO-SOURCE; SIO MASERS; DARK MASS; 86 GHZ; PERFORMANCE AB In the first two papers of this series, we determined the position of Sgr A* on infrared images by aligning the positions of red giant stars with positions measured at radio wavelengths for their circumstellar SiO masers. In this paper, we report the detections of five new stellar SiO masers within 50" (2 pc) of Sgr A* and new and/or improved positions and proper motions of 15 stellar SiO masers. The current accuracies are approximate to 1 mas in position and approximate to 0.3 mas yr(-1) in proper motion. We find that the propermotion of the central stellar cluster with respect to Sgr A* is less than 45 km s(-1). One star, IRS 9, has a three-dimensional speed of approximate to 370 km s(-1) at a projected distance of 0.33 pc from Sgr A*. If IRS 9 is bound to the inner parsec, this requires an enclosed mass that exceeds current estimates of the sum of the mass of Sgr A* and luminous stars in the stellar cusp by approximate to 0.8 x 10(6) M-circle dot. Possible explanations include: (1) that IRS 9 is not bound to the central parsec and has "fallen'' from a radius greater than 9 pc, (2) that a cluster of dark stellar remnants accounts for some of the excess mass, and/or (3) that R-0 is considerably greater than 8 kpc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM reid@cfa.harvard.edu; kmenten@mpifr-bonn.mpg.de; trippe@mpe.mpg.de; ott@mpe.mpg.de; genzel@mpe.mpg.de NR 35 TC 44 Z9 45 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 10 PY 2007 VL 659 IS 1 BP 378 EP 388 DI 10.1086/511744 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300032 ER PT J AU Safi-Harb, S Ribo, M Butt, Y Matheson, H Negueruela, I Lu, FJ Jia, SM Chen, Y AF Safi-Harb, Samar Ribo, Marc Butt, Yousaf Matheson, Heather Negueruela, Ignacio Lu, Fangjun Jia, Shumei Chen, Yong TI A multiwavelength study of 1WGA J1346.5-6255: A new gamma Cas analog unrelated to the background supernova remnant G309.2-00.6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (G309.2-00.6); open clusters and associations : individual (NGC 5281); stars : emission-line, Be; stars : individual (HD 119682); X-rays : individual (1RXS J134633.6-625528, 1WGA J1346.5-6255, SNR G309.2-00.6) ID X-RAY-EMISSION; ALL-SKY SURVEY; PERIOD DETERMINATION; STARS; CASSIOPEIAE; SOUTHERN; REMNANTS; CATALOG; PARAMETERS; ROTATION AB 1WGA J1346.5-6255 is a ROSAT X-ray source found within the radio lobes of the supernova remnant (SNR) G309.2-00.6. It appears to coincide with the bright and early-type star HD 119682, in the galactic open cluster NGC 5281. Its radiomorphology, consisting of two brightened and distorted arcs of emission on opposite sides of the 1WGA J1346.5-6255 source and of a jetlike feature and break in the shell, suggest that 1WGA J1346.5-6255/G309.2-00.6 is a young analog of the microquasar powering the W50 nebula SS 433. This motivated us to study this source at X-ray and optical wavelengths. We present new Chandra observations of 1WGA J1346.5-6255, archival XMM-Newton observations of G309.2-00.6, and optical spectroscopic observations of HD 119682, to search for X-ray jets from 1WGA J1346.5-6255, study its association with the SNR, and test for whether HD 119682 represents its optical counterpart. We find no evidence for jets from 1WGA J1346.5-6255 down to an unabsorbed flux of 2.6 x 10(-13) ergs cm(-2) s (0.5-7.5 keV), we rule out its association with G309.2-00.6, and we confirm that HD 119682 is its optical counterpart. We derive a distance of 1.2 x 0.3 kpc, consistent with the distance estimate to NGC 5281 (1.3 +/- 0.3 kpc), and much smaller than the distance derived to G309.2-00.6. We discuss the nature of the source, unveil that HD 119682 is a Be star, and suggest it is a new member of the recently proposed group of gamma Cas analogs. The Chandra and XMM-Newton X-ray light curves show variability on timescales of hundreds of seconds, and the presence of a possible period of similar to 1500 s that could be the rotational period of an accreting neutron star or white dwarf in this gamma Cas analog. C1 Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. George Washington Univ, Dept Phys, Washington, DC 20052 USA. Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. Univ Paris 07, CEA Saclay, CNRS,Serv Astrophys, UMR 7158,DSM,DAPNIA, F-91191 Gif Sur Yvette, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Alacant, Escuela Politecn Super, Dept Fis Ingn Sistemas & Teoria Senal, Alicante 03080, Spain. Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astophys, Beijing 100049, Peoples R China. RP Safi-Harb, S (reprint author), Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. EM safiharb@cc.umanitoba.ca RI Negueruela, Ignacio/L-5483-2014; Ribo, Marc/B-3579-2015 OI Negueruela, Ignacio/0000-0003-1952-3680; NR 51 TC 8 Z9 8 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 10 PY 2007 VL 659 IS 1 BP 407 EP 418 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300034 ER PT J AU Jorgensen, JK Bourke, TL Myers, PC Di Francesco, J van Dishoeck, EF Lee, CF Ohashi, N Schoier, FL Takakuwa, S Wilner, DJ Zhang, QZ AF Jorgensen, Jes K. Bourke, Tyler L. Myers, Philip C. Di Francesco, James van Dishoeck, Ewine F. Lee, Chin-Fei Ohashi, Nagayoshi Schoier, Fredrik L. Takakuwa, Shigehisa Wilner, David J. Zhang, Qizhou TI PROSAC: A submillimeter array survey of low-mass protostars. I. Overview of program: Envelopes, disks, outflows, and hot cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; ISM : jets and outflows; ISM : molecules; stars : formation; techniques : interferometric ID YOUNG STELLAR OBJECTS; T-TAURI STARS; PROTOSTELLAR ENVELOPES; CONTINUUM OBSERVATIONS; IRAS 16293-2422; CHEMICAL DIFFERENTIATION; PROTOPLANETARY DISKS; SUBARCSECOND SURVEY; INFALLING ENVELOPE; ORGANIC-MOLECULES AB This paper presents a large spectral line and continuum survey of eight deeply embedded, low-mass protostellar cores using the SMA. High-excitation line emission from 11 molecular species originating in warm and dense gas has been imaged at high angular resolution (1"-3", typically 200-600 AU) together with continuum emission at 230 GHz (1.3 mm) and 345 GHz (0.8 mm). Compact continuum emission is observed for all sources, which likely originates in marginally optically thick circumstellar disks, with typical lower limits to their masses of 0.1 M-circle dot (1%-10% of the masses of their envelopes) and a dust opacity law, kappa(nu) proportional to nu(beta), with beta approximate to 1. Prominent collimated outflows are present in CO 2-1 observations in all sources. The most diffuse outflows are found in the sources with the lowest ratios of disk to envelope mass, and it is suggested that these sources are in a phase where accretion of matter from the envelope has almost finished and the remainder of the envelope material is being dispersed by the outflows. Other characteristic dynamical signatures are inverse P Cygni profiles indicative of infalling motions seen in the (CO)-C-13 2-1 lines toward NGC 1333 IRAS 4A and NGC 1333 IRAS 4B. Outflow-induced shocks are present on all scales in the protostellar environments and are most clearly traced by the emission of CH3OH in NGC 1333 IRAS 4A and NGC 1333 IRAS 4B. These observations suggest that the emission of CH3OH and H2CO from these proposed "hot corinos'' is related to the shocks caused by the protostellar outflows. Only one source, NGC 1333 IRAS 2A, has evidence for hot, compact CH3OH emission coincident with the embedded protostar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Leiden Observ, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, Hilo, HI 96720 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Stockholm Observ, SE-10691 Stockholm, Sweden. Natl Astron Observ, ALMA Project Off, Tokyo 1818588, Japan. RP Jorgensen, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jjorgensen@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 73 TC 150 Z9 150 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 10 PY 2007 VL 659 IS 1 BP 479 EP 498 DI 10.1086/512230 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300040 ER PT J AU Lee, CF Ho, PTP Hirano, N Beuther, H Bourke, TL Shang, H Zhang, QZ AF Lee, Chin-Fei Ho, Paul T. P. Hirano, Naomi Beuther, Henrik Bourke, Tyler L. Shang, Hsien Zhang, Qizhou TI HH 212: Submillimeter array observations of a remarkable protostellar jet SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (HH 212); ISM : jets and outflows; stars : formation ID YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; EMISSION; SIO; SIMULATIONS; MODELS; DRIVEN; SHOCKS; CORES; LINE AB HH 212 is a nearby (460 pc) protostellar jet discovered in H-2 powered by a Class 0 source, IRAS 05413 - 0104. We have mapped it in 850 mu m continuum, SiO(J = 8-7), CO(J = 3-2), SO(N-J =8(9)-7(8) ), HCO+(J = 4-3), and (HCO+)-C-13(J = 4-3) emission simultaneously at similar to 1 '' resolution with the Submillimeter Array. Thermal dust emission is seen in continuum around the source, mainly arising from an inner envelope and a possible disk. The inner envelope is also seen with rotation in CO and HCO+ ,and probably in SO. Like H (2) emission, CO and SiO emission are seen along the jet axis but extending closer to the source, tracing the bow shocks and the continuous structures in between. SO emission is seen forming a jetlike structure extending from the source, likely tracing the jet near the launching region. The jet is episodic and bending. It may also be slightly precessing. A hint of jet rotation is also seen across the jet axis. Internal outflow shells are seen in CO and HCO+ associated with the bow shocks in the inner part of the jet. The bases of the HCO+ shells are seen with a hint of rotation, probably consisting mainly of the material extending from the inner envelope and even the possible disk. The bases of the outflow shells are also seen in (HCO+)-C-13 and even the continuum, probably tracing the dense material extending from around the same regions. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Lee, CF (reprint author), Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. EM cflee@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 36 TC 36 Z9 36 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2007 VL 659 IS 1 BP 499 EP 511 DI 10.1086/512540 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300041 ER PT J AU Currie, T Balog, Z Kenyon, SJ Rieke, G Prato, L Young, ET Muzerolle, J Clemens, DP Buie, M Sarcia, D Grabu, A Tollestrup, EV Taylor, B Dunham, E Mace, G AF Currie, Thayne Balog, Zoltan Kenyon, S. J. Rieke, G. Prato, L. Young, E. T. Muzerolle, J. Clemens, D. P. Buie, M. Sarcia, D. Grabu, A. Tollestrup, E. V. Taylor, B. Dunham, E. Mace, G. TI SPITZER IRAC and JHK(S) observations of h and chi Persei: Constraints on protoplanetary disk and massive cluster evolution at similar to 10(7) years SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; open clusters and associations : individual (NGC 869; NGC 884) ID INFRARED ARRAY CAMERA; ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; T-TAURI STARS; SPACE-TELESCOPE; PLANETESIMAL FORMATION; CIRCUMSTELLAR DISKS; PHOTOMETRY; MODELS; ASSOCIATION AB We describe IRAC 3.6-8 mu m observations and ground-based near-IR JHK(s) photometry from Mimir and 2MASS of the massive double cluster h and chi Persei complete to J = 15.5 (M similar to 1.3 M-circle dot). Within 25' of the cluster centers we detect similar to 11,000 sources with J <= 15.5,similar to 7000 sources with [4.5] <= 15, and similar to 5000 sources with [8] <= 14.5. In both clusters the surface density profiles derived from the 2MASS data decline with distance from the cluster centers as expected for a bound cluster. Within 15' of the cluster centers, similar to 50% of the stars lie on a reddened similar to 13 Myr isochrone; at 15'-25' from the cluster centers, similar to 40% lie on this isochrone. Thus, the optical 2MASS color-magnitude diagrams indicate that h and chi Per are accompanied by a halo population with roughly the same age and distance as the two dense clusters. The double cluster lacks any clear IR excess sources for J <= 13.5 (similar to 2.7 M-circle dot). Therefore, disks around highmass stars disperse prior to similar to 10(7) yr. At least 2%-3% of the fainter cluster stars have strong IR excess at both [5.8] and [ 8]. About 4%-8% of sources slightly more massive than the Sun (similar to 1.4M(circle dot)) have IR excesses at [8]. Combined with the lack of detectable excesses for brighter stars, this result suggests that disks around lower mass stars have longer lifetimes. The IR excess population also appears to be larger at longer IRAC bands ([5.8], [8]) than at shorter IRAC/2MASS bands (K-s, [4.5]), a result consistent with an inside-out clearing of disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. RP Currie, T (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. NR 54 TC 37 Z9 37 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 10 PY 2007 VL 659 IS 1 BP 599 EP 615 DI 10.1086/512006 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300049 ER PT J AU Zhao, M Monnier, JD Torres, G Boden, AF Claret, A Millan-Gabet, R Pedretti, E Berger, JP Traub, WA Schloerb, FP Carleton, NP Kern, P Lacasse, MG Malbet, F Perraut, K AF Zhao, M. Monnier, J. D. Torres, G. Boden, A. F. Claret, A. Millan-Gabet, R. Pedretti, E. Berger, J.-P. Traub, W. A. Schloerb, F. P. Carleton, N. P. Kern, P. Lacasse, M. G. Malbet, F. Perraut, K. TI Physical orbit for lambda virginis and a test of stellar evolution models SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; binaries : visual; instrumentation : interferometers; stars : fundamental parameters; stars : individual ( lambda Virginis) ID A-TYPE STARS; INTERMEDIATE ASTROMETRIC DATA; LINED SPECTROSCOPIC BINARIES; UVBY-BETA-PHOTOMETRY; EFFECTIVE TEMPERATURE; ECLIPSING BINARIES; TIDAL-EVOLUTION; F-STARS; B-STAR; ABSOLUTE DIMENSIONS AB The star lambda Virginis is a well-known double-lined spectroscopic Am binary with the interesting property that both stars are very similar in abundance but one is sharp-lined and the other is broad-lined. We present combined interferometric and spectroscopic studies of lambda Vir. The small scale of the lambda Vir orbit (similar to 20 mas) is well resolved by the Infrared Optical Telescope Array (IOTA), allowing us to determine its elements, as well as the physical properties of the components, to high accuracy. The masses of the two stars are determined to be 1.897 and 1.721 M-circle dot, with 0.7% and 1.5% errors, respectively, and the two stars are found to have the same temperature of 8280 +/- 200K. The accurately determined properties of lambda Vir allow comparisons between observations and current stellar evolution models, and reasonable matches are found. The best-fit stellar model gives lambda Vir a subsolar metallicity of Z = 0.0097 and an age of 935 Myr. The orbital and physical parameters of lambda Vir also allow us to study its tidal evolution timescales and status. Although atomic diffusion is currently considered to be the most plausible cause of the Am phenomenon, the issue is still being actively debated in the literature. With the present study of the properties and evolutionary status of lambda Vir, this system is an ideal candidate for further detailed abundance analyses that might shed more light on the source of the chemical anomalies in these A stars. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. CALTECH, Michelson Sci Ctr, Pasadena, CA USA. CSIC, Inst Astrofis Andalucia, Granada, Spain. Lab Astrophys Grenoble, St Martin Dheres, France. Univ Massachusetts, Dept Astron, Amherst, MA USA. RP Zhao, M (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM mingzhao@umich.edu NR 69 TC 22 Z9 22 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 APR 10 PY 2007 VL 659 IS 1 BP 626 EP 641 DI 10.1086/511415 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300051 ER PT J AU Raymond, JC Holman, G Ciaravella, A Panasyuk, A Ko, YK Kohl, J AF Raymond, John C. Holman, Gordon Ciaravella, A. Panasyuk, A. Ko, Y.-K. Kohl, J. TI Transition region emission and energy input to thermal plasma during the impulsive phase of solar flares SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : flares; Sun : UV radiation; Sun : X-rays, gamma rays ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; X-RAY-SPECTRA; CHROMOSPHERIC EVAPORATION; SUN; TEMPERATURES; DENSITY; BALANCE; MODELS; RHESSI; IONS AB The energy released in a solar flare is partitioned between thermal and nonthermal particle energy and lost to thermal conduction and radiation over a broad range of wavelengths. It is difficult to determine the conductive losses and the energy radiated at transition region temperatures during the impulsive phases of flares. We use UVCS measurements of O vi photons produced by five flares and subsequently scattered by O vi ions in the corona to determine the 5.0 <= log T <= 6.0 transition region luminosities. We compare them with the rates of increase of thermal energy and the conductive losses deduced from RHESSI and GOES X-ray data using areas from RHESSI images to estimate the loop volumes, cross-sectional areas, and scale lengths. The transition region luminosities during the impulsive phase exceed the X-ray luminosities for the first few minutes, but they are smaller than the rates of increase of thermal energy unless the filling factor of the X-ray-emitting gas is similar to 0.01. The estimated conductive losses from the hot gas are too large to be balanced by radiative losses or heating of evaporated plasma, and we conclude that the area of the flare magnetic flux tubes is much smaller than the effective area measured by RHESSI during this phase of the flares. For the 2002 July 23 flare, the energy deposited by nonthermal particles exceeds the energy radiated in X-rays, the energy radiated at transition region temperatures, and the rate of increase of the thermal energy. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. INAF Osserv Astron Palermo, I-90134 Palermo, Italy. RP Raymond, JC (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RI Holman, Gordon/C-9548-2012 NR 41 TC 19 Z9 19 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 APR 10 PY 2007 VL 659 IS 1 BP 750 EP 757 DI 10.1086/512604 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300062 ER PT J AU Korreck, KE Zurbuchen, TH Lepri, ST Raines, JM AF Korreck, K. E. Zurbuchen, T. H. Lepri, S. T. Raines, J. M. TI Heating of heavy ions by interplanetary coronal mass ejection driven collisionless shocks SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; Sun : coronal mass ejections (CMEs) ID ADVANCED COMPOSITION EXPLORER; EARTHS BOW SHOCK; WIND MINOR IONS; SOLAR-WIND; DIFFUSE IONS; ACCELERATION; INJECTION; PROTONS; TEMPERATURE; SIMULATIONS AB Shock heating and particle acceleration processes are some of the most fundamental physical phenomena of plasma physics, with countless applications in laboratory physics, space physics, and astrophysics. This study is motivated by previous observations of nonthermal heating of heavy ions in astrophysical shocks. Here we focus on shocks driven by interplanetary coronal mass ejections (ICMEs), which heat the solar wind and accelerate particles. This study focuses specifically on the heating of heavy ions caused by these shocks. Previous studies have focused only on the two dynamically dominant species, H+ and He+2. This study utilizes thermal properties measured by the Solar Wind Ion Composition Spectrometer (SWICS) aboard the Advanced Composition Explorer (ACE) spacecraft to examine heavy ion heating. This instrument provides data for many heavy ions not previously available for detailed study, such as oxygen (O+6, O+7), carbon (C+5, C+6), and iron (Fe+10). The ion heating is found to depend critically on the upstream plasma beta, mass-to-charge ratio of the ion, M/Q, and shock magnetic angle, theta(Bn). Ours is similar to past studies in that there is no strong dependence of ion heating on Mach number. The heating mechanism described in Lee & Wu is examined to explain the observed heating trends in the heavy ion thermal data. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. Univ Michigan, Atmospher Ocean & Space Sci Dept, Ann Arbor, MI 48109 USA. RP Korreck, KE (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RI Lepri, Susan/I-8611-2012 NR 27 TC 15 Z9 15 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 10 PY 2007 VL 659 IS 1 BP 773 EP 779 DI 10.1086/512360 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EF UT WOS:000245773300064 ER PT J AU Whelan, ET Ray, TP Randich, S Bacciotti, F Jayawardhana, R Testi, L Natta, A Mohanty, S AF Whelan, E. T. Ray, T. P. Randich, S. Bacciotti, F. Jayawardhana, R. Testi, L. Natta, A. Mohanty, S. TI Discovery of a bipolar outflow from 2MASSW J1207334-393254, A 24 M-jup brown dwarf SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : jets and outflows; stars : low-mass, brown dwarfs; stars : mass loss; techniques : high angular resolution ID LOW-MASS STARS; T-TAURI STARS; FORBIDDEN EMISSION; ACCRETION; SPECTROSCOPY; MODELS; SCALES; PHASE AB The 24 M (Jup) brown dwarf 2MASS 1207 - 3932 has for some time been known to show clear signs of classical T Tauri - like accretion. Through analysis of its oxygen forbidden emission, we have discovered that it is driving a bipolar outflow. Blue- and redshifted components to the [O I] lambda 6300 forbidden emission line are seen at velocities of -8 and +4 km s(-1) ( on either side of the systemic velocity). Spectroastrometry recovers the position of both components relative to the brown dwarf at similar to 0.08" ( in opposing directions). A position-velocity diagram of the line region supports the spectroastrometric results. The H alpha and He I lambda 6678 lines were also analyzed. These line regions are not offset with respect to the continuum, ruling out the presence of spectroastrometric artifacts and underlining the validity of the [O I] lambda 6300 results. The low radial velocity of the outflow and the relatively large offsets are consistent with 2MASS 1207 - 3932 having a near edge- on disk as proposed by Scholz et al. 2MASS 1207 - 3932 is now the smallest mass galactic object known to drive an outflow. The age of the TW Hydrae association (similar to 8 Myr) also makes this one of the oldest objects with a resolved jet. This discovery not only highlights the robustness of the outflow mechanism over an enormous range of masses but also suggests that it may even be feasible for young giant planets with accretion disks to drive outflows. C1 Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Whelan, ET (reprint author), Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. OI Randich, Sofia/0000-0003-2438-0899; BACCIOTTI, FRANCESCA/0000-0001-5776-9476 NR 34 TC 32 Z9 32 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2007 VL 659 IS 1 BP L45 EP L48 DI 10.1086/516734 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158EM UT WOS:000245774100012 ER PT J AU Woodley, NE AF Woodley, Norman E. TI Notes on South American Dasyomma, with the description of a remarkable new species from Chile (Diptera : Athericidae) SO ZOOTAXA LA English DT Article DE Diptera; Athericidae; Dasyomma; new species; Chile; Bolivia AB A new species of Dasyomma Macquart, D. chrysopilum sp. nov., is described from Chile (Malleco and Nuble Provinces). This species differs from all other known species in having dense golden pilosity on the abdominal tergites of both sexes. Dasyomma basale Malloch is redescribed, with the female described for the first time. C1 USDA, Smithsonian Institut, Systemat Entomol Lab, Washington, DC 20013 USA. RP Woodley, NE (reprint author), USDA, Smithsonian Institut, Systemat Entomol Lab, NHB 168,POB 37012, Washington, DC 20013 USA. EM norman.woodley@ars.usda.gov RI Woodley, Norman/M-6160-2014 NR 5 TC 2 Z9 2 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 9 PY 2007 IS 1443 BP 29 EP 35 PG 7 WC Zoology SC Zoology GA 154MG UT WOS:000245511000003 ER PT J AU Srygley, RB AF Srygley, Robert B. TI Evolution of the wave: aerodynamic and aposematic functions of butterfly wing motion SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE locomotor mimicry; insect flight; mimetic behaviour; mutualism; bird vision; Mullerian mimicry ID HELICONIUS BUTTERFLIES; WARNING SIGNALS; VISUAL NEURONS; MIMICRY; PERCEPTION; FLIGHT; MORPHOLOGY; MODELS; COSTS AB Many unpalatable butterfly species use coloration to signal their distastefulness to birds, but motion cues may also be crucial to ward off predatory attacks. In previous research, captive passion-vine butterflies Heliconius mimetic in colour pattern were also mimetic in motion. Here, I investigate whether wing motion changes with the flight demands of different behaviours. If birds select for wing motion as a warning signal, aposematic butterflies should maintain wing motion independently of behavioural context. Members of one mimicry group ( Heliconius cydno and Heliconius sapho) beat their wings more slowly and their wing strokes were more asymmetric than their sister-species ( Heliconius melpomene and Heliconius erato, respectively), which were members of another mimicry group having a quick and steady wing motion. Within mimicry groups, wing beat frequency declined as its role in generating lift also declined in different behavioural contexts. In contrast, asymmetry of the stroke was not associated with wing beat frequency or behavioural context - strong indication that birds process and store the Fourier motion energy of butterfly wings. Although direct evidence that birds respond to subtle differences in butterfly wing motion is lacking, birds appear to generalize a motion pattern as much as they encounter members of a mimicry group in different behavioural contexts. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Oxford, Dept Zool, Oxford OX1 3PS, England. RP Srygley, RB (reprint author), USDA ARS, NPARL, 1500 N Cent Ave, Sidney, MT 59270 USA. EM bob.srygley@zoo.ox.ac.uk NR 30 TC 11 Z9 12 U1 2 U2 15 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD APR 7 PY 2007 VL 274 IS 1612 BP 913 EP 917 DI 10.1098/rspb.2006.0261 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 138PV UT WOS:000244375600002 PM 17264060 ER PT J AU Faisal, FHM Abdurrouf, A Miyazaki, K Miyaji, G AF Faisal, F. H. M. Abdurrouf, A. Miyazaki, K. Miyaji, G. TI Origin of anomalous spectra of dynamic alignments observed in N-2 and O-2 SO PHYSICAL REVIEW LETTERS LA English DT Article ID ORDER HARMONIC-GENERATION; LASER FIELDS; REVIVAL STRUCTURE; MOLECULES; ORBITALS AB Recent pump-probe experiments with intense femtosecond laser pulses and diatomic molecules N-2 and O-2, have revealed the presence of Raman-forbidden anomalous series and lines in the Fourier spectrum of HHG (high harmonic generation) signals. A theoretical analysis of the problem is made by deriving a general expression of the angle dependent HHG operator that governs the dynamic alignment signals in linear molecules, and applying them to the experiments in N-2 and O-2. A unified interpretation of the origin of the observed Raman-allowed and the anomalous spectral features is given. The results are also used to estimate the molecular temperature in the experiments. C1 Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Kyoto Univ, Inst Adv Energy, Uji, Kyoto 6110011, Japan. RP Faisal, FHM (reprint author), Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany. RI Miyaji, Godai/I-6031-2014 NR 24 TC 24 Z9 24 U1 1 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD APR 6 PY 2007 VL 98 IS 14 AR 143001 DI 10.1103/PhysRevLett.98.143001 PG 4 WC Physics, Multidisciplinary SC Physics GA 154MQ UT WOS:000245512100021 PM 17501269 ER PT J AU Plaut, JJ Picardi, G Safaeinili, A Ivanov, AB Milkovich, SM Cicchetti, A Kofman, W Mouginot, J Farrell, WM Phillips, RJ Clifford, SM Frigeri, A Orosei, R Federico, C Williams, IP Gurnett, DA Nielsen, E Hagfors, T Heggy, E Stofan, ER Plettemeier, D Watters, TR Leuschen, CJ Edenhofer, P AF Plaut, Jeffrey J. Picardi, Giovanni Safaeinili, Ali Ivanov, Anton B. Milkovich, Sarah M. Cicchetti, Andrea Kofman, Wlodek Mouginot, Jeremie Farrell, William M. Phillips, Roger J. Clifford, Stephen M. Frigeri, Alessandro Orosei, Roberto Federico, Costanzo Williams, Iwan P. Gurnett, Donald A. Nielsen, Erling Haegfors, Tor Heggy, Essam Stofan, Ellen R. Plettemeier, Dirk Watters, Thomas R. Leuschen, Carlton J. Edenhofer, Peter TI Subsurface radar sounding of the south polar layered deposits of Mars SO SCIENCE LA English DT Article ID CAP; REGION AB The ice-rich south polar layered deposits of Mars were probed with the Mars Advanced Radar for Subsurface and Ionospheric Sounding on the Mars Express orbiter. The radar signals penetrate deep into the deposits (more than 3.7 kilometers). For most of the area, a reflection is detected at a time delay that is consistent with an interface between the deposits and the substrate. The reflected power from this interface indicates minimal attenuation of the signal, suggesting a composition of nearly pure water ice. Maps were generated of the topography of the basal interface and the thickness of the layered deposits. A set of buried depressions is seen within 300 kilometers of the pole. The thickness map shows an asymmetric distribution of the deposits and regions of anomalous thickness. The total volume is estimated to be 1.6 x 10(6) cubic kilometers, which is equivalent to a global water layer approximately 11 meters thick. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Roma La Sapienza, Infocom Dept, I-00184 Rome, Italy. Lab Planetol Grenoble, F-38041 Grenoble, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Lunar & Planetary Inst, Houston, TX 77058 USA. Univ Perugia, Dipartimento Sci Terra, I-06123 Perugia, Italy. Ist Nazl Astrofis, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. Queen Mary Univ London, Sch Math Sci, Astron Unit, London E1 4NS, England. Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Proxemy Res, Laytonville, MD 20882 USA. Tech Univ Dresden, Fak Elekrtotech & Informat Tech, D-01062 Dresden, Germany. Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA. Ruhr Univ Bochum, Fak Elektrotech & Informat Tech, D-44780 Bochum, Germany. RP Plaut, JJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Kofman, Wlodek/C-4556-2008; Frigeri, Alessandro/F-2151-2010; Heggy, Essam/E-8250-2013; Farrell, William/I-4865-2013; Ivanov, Anton/C-8944-2014; Mouginot, Jeremie/G-7045-2015; OI Frigeri, Alessandro/0000-0002-9140-3977; Heggy, Essam/0000-0001-7476-2735; Ivanov, Anton/0000-0001-8376-8581; CICCHETTI, ANDREA/0000-0002-9588-6531; Williams, Iwan Prys/0000-0002-8069-1344 NR 19 TC 125 Z9 126 U1 2 U2 25 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 APR 6 PY 2007 VL 316 IS 5821 BP 92 EP 95 DI 10.1126/science.1139672 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 153XD UT WOS:000245470500038 PM 17363628 ER PT J AU St Thomas, L AF St. Thomas, Linda TI Small quibbles SO NEW REPUBLIC LA English DT Letter C1 Smithsonian Inst, Washington, DC 20560 USA. RP St Thomas, L (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NEW REPUBLIC INC PI WASHINGTON PA 1331 H STREET, NW STE 700, WASHINGTON, DC 20005 USA SN 0028-6583 J9 NEW REPUBLIC JI New Repub. PD APR 2 PY 2007 VL 236 IS 13 BP 6 EP 6 PG 1 WC Political Science SC Government & Law GA 175OU UT WOS:000247023700003 ER PT J AU Erwin, TL Moore, W AF Erwin, Terry L. Moore, Wendy TI Taxonomic review of the Neotropical genus Moriosomus Motschulsky (Insecta : Coleoptera, Carabidae, Morionini) with notes on the way of life of the species SO ZOOTAXA LA English DT Review DE Colombia; Costa Rica; Nicaragua; Ecuador; Panama; Peru; INBio; Carabidae; Morionini; Moriosomus Motschulsky 1855 AB Moriosomus Motschulsky 1855 is a Neotropical genus containing three species in the carabid beetle tribe Morionini. Moriosomus adults are found under tree bark and in rotting logs in rainforests; larvae are unknown. This revision of Moriosomus includes diagnoses, descriptions, illustrations, and distributional data for all three known species, including Moriosomus motschulskyi Erwin & Moore, new species ("PERU, HUa N[UCO], Divisoria," Cordillera Azul, 1600m, 08 degrees 54' 0 S, 075 degrees 40' 0 W). We provide an identification key to the species based on adult external structure. We clarify the the date of the description of the genus Moriosomus, which is 1855, rather than 1864 as it is often incorrectly cited in the literature. In addition, we define the tribe Morionini and provide a key for identification of the two genera resident in the Western Hemisphere. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Hyper Divers Grp, Washington, DC 20013 USA. Calif Acad Sci, Dept Entomol, San Francisco, CA 94103 USA. RP Erwin, TL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Hyper Divers Grp, MRC 187,POB 37012, Washington, DC 20013 USA. EM erwint@si.edu; wmoore@calacademy.org NR 28 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 2 PY 2007 IS 1438 BP 49 EP 63 PG 15 WC Zoology SC Zoology GA 153HF UT WOS:000245422200003 ER PT J AU Albrecht, L Meyer, CFJ Kalko, EKV AF Albrecht, Larissa Meyer, Christoph F. J. Kalko, Elisabeth K. V. TI Differential mobility in two small phyllostomid bats, Artibeus watsoni and Micronycteris microtis, in a fragmented neotropical landscape SO ACTA THERIOLOGICA LA English DT Article DE fragmentation; home range; islands; radiotracking; Panama ID AMAZONIAN FOREST FRAGMENTS; FRENCH-GUIANA; SPECIES RICHNESS; GLEANING BATS; LOS-TUXTLAS; HABITAT; PANAMA; COMMUNITIES; ISLANDS; MEXICO AB To assess the influence of habitat fragmentation on small bats, we determined home range size and mobility of the frugivorous Artibeus watsoni Thomas, 1901 and the gleaning insectivorous Micronycteris microtis Miller, 1898 by radiotracking on different-sized islands (2.7-17 ha) in Lake Gatun, Panama. The two species differed in their response to fragmentation. Home range size was highly variable in the five tracked A. watsoni, ranging from 1.8 to 17.9 ha with a mean of about 9 ha. Some individuals flew regularly between islands and/or the mainland, thereby traversing up to 180 m of open water. In comparison, home ranges of three M. microtis were with about 3.8 ha only half as large. All of M. microtis exhibited sedentary foraging behaviour and did not cross open water, suggesting that they might persist at least on some of the islands as resident populations. Our findings are consistent with radiotracking data from a previous study and indicate that small habitat patches are still used by small bats, provided the degree of isolation is low and that sufficient resources and larger habitat patches exist in close vicinity, potentially acting as additional feeding grounds and source populations. C1 Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Albrecht, L (reprint author), Univ Ulm, Dept Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM elisabeth.kalko@uni-ulm.de RI Meyer, Christoph/A-4363-2012 OI Meyer, Christoph/0000-0001-9958-8913 NR 40 TC 22 Z9 25 U1 2 U2 11 PU POLISH ACAD SCIENCES PI BIALOWIEZA PA MAMMAL RESEARCH INST, 17-230 BIALOWIEZA, POLAND SN 0001-7051 J9 ACTA THERIOL JI Acta Theriol. PD APR PY 2007 VL 52 IS 2 BP 141 EP 149 DI 10.1007/BF03194209 PG 9 WC Zoology SC Zoology GA 167AA UT WOS:000246421600004 ER PT J AU Heaney, PJ McKeown, DA Post, JE AF Heaney, Peter J. McKeown, David A. Post, Jeffrey E. TI Anomalous behavior at the I2/a to Imab phase transition in SiO2-moganite: An analysis using hard-mode Raman spectroscopy SO AMERICAN MINERALOGIST LA English DT Article DE moganite; phase transition; Raman spectroscopy; silica ID ALPHA-BETA-TRANSITION; MICROCRYSTALLINE SILICA; THERMODYNAMIC PROPERTIES; CRYSTAL-STRUCTURE; LASER RAMAN; MOGANITE; QUARTZ; CRISTOBALITE; POLYMORPH; CATHODOLUMINESCENCE AB The silica polymorph moganite is commonly intergrown with quartz in microcrystalline silica varieties that are less than similar to 100 Ma in age. Synchrotron X-ray diffraction suggests that a displacive phase transition occurs when moganite is heated above similar to 570 K, with an increase in symmetry from I2/a to Imab. In the present study, we employed hard-mode Raman spectroscopy to confirm the existence of the alpha-beta moganite transformation and to offer complementary insight into the transition mechanism. Our analysis of the displacement of the 501 Delta cm(-1) symmetric stretching-bending vibration (B-3g, mode) with changing temperature strongly supports the existence of a monoclinic-to-orthorhombic phase transition between 570 and 590 K. Between 593 and 723 K, however, the mode remained fixed at 496 Delta cm(-1). This behavior was repeated on cooling, but with a hysteresis of over 100 K. We offer three hypotheses that may explain this observation: (1) the intergrowth of nanoscale quartz lamellae within I P moganite may exert a strain that inhibits the transition; (2) the transition may exhibit a martensitic character marked by the co-existence of alpha- and beta-moganite over a finite temperature interval; and (3) the alpha- and beta-moganite transition may occur via an intermediate phase. C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Catholic Univ Amer, Vitreous State Lab, Washington, DC 20064 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Heaney, PJ (reprint author), Penn State Univ, Dept Geosci, 309 Deike, University Pk, PA 16802 USA. EM heaney@geosc.psu.edu NR 53 TC 11 Z9 12 U1 0 U2 9 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD APR PY 2007 VL 92 IS 4 BP 631 EP 639 DI 10.2138/AM.2007.2184 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 154JT UT WOS:000245503700021 ER PT J AU Leece, C AF Leece, Christina TI The woman who mapped labrador: The life and expedition diary of Mina Hubbard. SO AMERICAS LA English DT Book Review C1 Smithsonian Inst, Arctic Studies Inst, Washington, DC 20560 USA. RP Leece, C (reprint author), Smithsonian Inst, Arctic Studies Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ACAD AMER FRANCISCAN HIST PI WEST BETHESDA PA BOX 34440, WEST BETHESDA, MD 20817 USA SN 0003-1615 J9 AMERICAS JI Americas PD APR PY 2007 VL 63 IS 4 BP 658 EP 659 DI 10.1353/tam.2007.0076 PG 2 WC History SC History GA 163MJ UT WOS:000246163600008 ER PT J AU Ibarguengoytia, NR Renner, ML Boretto, JM Piantoni, C Cussac, VE AF Ibarguengoytia, Nora R. Renner, Marianne L. Boretto, Jorgelina M. Piantoni, Carla Cussac, Victor E. TI Thermal effects on locomotion in the nocturnal gecko Homonota darwini (Gekkonidae) SO AMPHIBIA-REPTILIA LA English DT Article ID SPRINT SPEED; CAUDAL-AUTOTOMY; BEHAVIORAL THERMOREGULATION; NIVEOSCINCUS-METALLICUS; BODY TEMPERATURES; LACERTID LIZARDS; TAIL LOSS; PERFORMANCE; GROWTH; EVOLUTION AB Nocturnal lizards show a complex adaptation to environmental temperature. They obtain heat from the substratum, using daytime for performing physiological functions inside thermally suitable shelters, and night-time which involves locomotion and loss of heat for capturing prey. Homonota darwini, the southernmost geckonid in the world, is a small nocturnal insectivorous gecko that occurs in saxicolous habitats of Patagonia, Argentina. Geckos were captured by hand during the day on a rocky hill near Bariloche (Rio Negro, Argentina) in spring and summer. All the geckos were active during daytime and had good limb mobility with a median body temperature of 23 degrees C. Body temperatures showed a direct dependence on the temperature of the roof of the shelter and on the air temperature. Geckos were made to run on a horizontal track and running speed was measured in two experiments: long runs (1 m) and sprint runs (0.20 m) during the day (diurnal) and at night (nocturnal). Speed was significantly greater in sprints than in long runs and speed increased with body temperature, reaching a maximum at a body temperature of 22 degrees C. Thus, we conclude that, although the low temperatures of Patagonia impose heavy constraints on the physiological performance of Homonota darwini, they have a peculiar arrangement of mechanical and biochemical abilities which allows for resource acquisition at night, using cryptic habits and short sprint runs. C1 Univ Nacl Comahue, Ctr Reg Univ Bariloche, Unidad Postal Univ Comahue, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina. Univ Bordeaux 2, UMR 5091, CNRS1, F-33076 Bordeaux, France. Smithsonian Inst, NHB, MRC, Washington, DC 20013 USA. RP Ibarguengoytia, NR (reprint author), Univ Nacl Comahue, Ctr Reg Univ Bariloche, Unidad Postal Univ Comahue, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. EM norai@bariloche.com.ar RI Renner, Marianne/H-5315-2011; Piantoni, Carla/K-2986-2015; OI Renner, Marianne/0000-0002-8727-6581; Piantoni, Carla/0000-0002-1201-0041; Cussac, Victor/0000-0001-6406-1855 NR 42 TC 12 Z9 13 U1 1 U2 11 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0173-5373 J9 AMPHIBIA-REPTILIA JI Amphib. Reptil. PD APR PY 2007 VL 28 IS 2 BP 235 EP 246 DI 10.1163/156853807780202440 PG 12 WC Zoology SC Zoology GA 169BS UT WOS:000246568300006 ER PT J AU Pannuti, TG Schlegel, EM Lacey, CK AF Pannuti, Thomas G. Schlegel, Eric M. Lacey, Christina K. TI A search for Chandra-detected X-ray counterparts to optically identified and candidate radio supernova remnants in five nearby face-on spiral galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual ( M81, M101, NGC 2403; NGC 4736; NGC 6946); supernova remnants ID LARGE-MAGELLANIC-CLOUD; H-II REGION; SCALE KEY PROJECT; ASTRONOMICAL DATA; PARTICLE-ACCELERATION; STATISTICAL-METHODS; UPPER LIMITS; EMISSION; M101; M81 AB We present a search for X-ray counterparts to optically identified and candidate radio supernova remnants (SNRs) in five nearby galaxies, M81, M101, NGC 2403, NGC 4736 (M94), and NGC 6946, using observations made with the Chandra X-Ray Observatory. A total of 138 optically identified SNRs and 50 candidate radio SNRs in these galaxies were sampled by these observations. Nine optically identified SNRs and 12 candidate radio SNRs are positionally coincident with Chandra-detected X-ray sources that were not already known to be time-variable or associated with X-ray binaries. We used survival statistics to determine if the properties of the optically identified SNRs with and without Chandra-detected counterparts (referred to as group A and group NotA, respectively), as well as the candidate radio SNRs with and without Chandra-detected counterparts (referred to as group B and group NotB, respectively) differ in a statistically significant manner. We find that for the SNRs in groups A and NotA, only the mean value of the diameter d differs significantly between the two groups (26 +/- 4 pc compared to 62 +/- 6 pc). In addition, for the SNRs in groups B and NotB, we find that only the spectral index alpha differs significantly between the two groups (0.6 +/- 0.1 compared to 0.9 +/- 0.1). We find no correlation between unabsorbed X-ray and optical luminosities for the group A SNRs and no correlation between unabsorbed X-ray and radio luminosities for the group B SNRs: this result indicates that the interstellar medium surrounding these SNRs is inhomogeneous rather than uniform. We claim that the higher incidence of Chandra-detected counterparts for candidate radio SNRs compared to the optically identified SNRs (as noticed in previous works) illustrates the role played by ambient density in affecting searches for SNRs in nearby galaxies at multiple wavelengths. We argue that deep systematic X-ray, optical, and radio observations of other galaxies are necessary to examine the multiwavelength properties of SNRs, to explore wavelength-dependent selection effects in more detail, and to search for time variability in the emission from X-ray counterparts to optically identified SNRs and candidate radio SNRs. C1 Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Texas, Dept Phys & Astron, San Antonio, TX 78285 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ S Carolina, Dept Phys & Astron, Columbia, SC 29208 USA. RP Pannuti, TG (reprint author), Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. EM t.pannuti@moreheadstate.edu; eric.schlegel@utsa.edu; lacey@sc.edu NR 78 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 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2007 VL 133 IS 4 BP 1361 EP 1372 DI 10.1086/510718 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 154YF UT WOS:000245543700015 ER PT J AU Sankrit, R Blair, WP Cheng, JY Raymond, JC Gaetz, TJ Szentgyorgyi, A AF Sankrit, Ravi Blair, William P. Cheng, Judy Y. Raymond, John C. Gaetz, Terrance J. Szentgyorgyi, Andrew TI Far ultraviolet spectroscopic explorer spectroscopy of the XA region in the Cygnus Loop supernova remnant SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : individual (Cygnus Loop); shock waves; supernova remnants ID RADIATIVE SHOCKS; TELESCOPE OBSERVATIONS; SPECTRAL IMAGES; EMISSION-LINES; FE-X; COEFFICIENTS; DUST; IONS; WAVE; RAY AB Spectra of the XA shock- cloud interaction region in the Cygnus Loop obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) are presented and analyzed. Several weak emission lines never before detected in the spectra of remnants are identified in a combined spectrum from four bright regions. The intensities of the silicon lines measured in this spectrum show that the 120-200 km s(-1) shocks are present in the XA region and are effective at liberating silicon from grains. Differences among the spectra imply that the shocked gas has a complex ionization structure. The strongest lines in the spectra, and also the most uniformly distributed, are O VI lambda lambda 1032, 1038. Approximately 10% of the O VI emission from regions interior to the main shock interaction arises from coronal (million-degree) gas. Model calculations show that the shock at the boundary between the cloud and remnant has a velocity of about 180 km s(-1) and has swept up a hydrogen column N-H = 1.66 x 10(18) cm(-2), indicating that the blast wave encountered the cloud about 5000 years ago. The O vi line profiles imply that the boundary shock is dominated by a single broad component with an intrinsic velocity width parameter, b approximate to 48 km s(-1), which is probably the result of bulk motions due to curvature of the shock front. Differences between the O vi velocity profiles of two regions separated by 2000 on the sky suggest the presence of a concentrated region of dust, which absorbs emission from the shock on the far side of the cloud. C1 Johns Hopkins Univ, Baltimore, MD USA. Smithsonian Astrophys Observ, Cambridge, MA USA. RP Sankrit, R (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NR 41 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 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2007 VL 133 IS 4 BP 1383 EP 1392 DI 10.1086/511768 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 154YF UT WOS:000245543700017 ER PT J AU Wu, JW Dunham, MM Evans, NJ Bourke, TL Young, CH AF Wu, Jingwen Dunham, Michael M. Evans, Neal J., II Bourke, Tyler L. Young, Chadwick H. TI SHARC-II mapping of Spitzer c2d small clouds and cores SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : clouds; stars : formation; stars : low-mass, brown dwarfs; submillimeter; Online material : machine-readable tables ID MASS STAR-FORMATION; NEARBY DENSE CORES; DUST CONTINUUM EMISSION; MOLECULAR CLOUDS; DARK CLOUDS; INTERSTELLAR CLOUDS; SPACE-TELESCOPE; LARGE-SCALE; IRAC; DISTANCE AB We present the results of a submillimeter survey of 53 low-mass dense cores with the Submillimeter High Angular Resolution Camera II (SHARC-II). The survey is a follow-up project to the Spitzer Legacy Program "From Molecular Cores to Planet-Forming Disks,'' with the purpose of creating a complete data set of nearby low-mass dense cores from the infrared to the millimeter. We present maps of 52 cores at 350 mu m and three cores at 450 mu m, two of which were observed at both wavelengths. Of these 52 cores, 41 were detected by SHARC-II; 32 contained one submillimeter source, while 9 contained multiple sources. For each submillimeter source detected, we report various source properties including source position, fluxes in various apertures, size, aspect ratio, and position angle. For the 12 cores that were not detected we present upper limits. The sources detected by SHARC-II have, on average, smaller sizes at the 2 sigma contours than those derived from longer wavelength bolometer observations. We conclude that this is not caused by a failure to integrate long enough to detect the full extent of the core; instead it arises primarily from the fact that the observations presented in this survey are insensitive to smoothly varying extended emission. We find that SHARC-II observations of low-mass cores are much better suited to distinguishing between starless and protostellar cores than observations at longer wavelengths. Very low luminosity objects, a new class of objects being discovered by the Spitzer Space Telescope in cores previously classified as starless, look very similar at 350 mu m to other cores with more luminous protostars. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70310 USA. RP Wu, JW (reprint author), Univ Texas, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jingwen@astro.as.utexas.edu; mdunham@astro.as.utexas.edu NR 60 TC 40 Z9 40 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2007 VL 133 IS 4 BP 1560 EP 1584 DI 10.1086/511959 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 154YF UT WOS:000245543700030 ER PT J AU Winn, JN Holman, MJ Henry, GW Roussanova, A Enya, K Yoshii, Y Shporer, A Mazeh, T Johnson, JA Narita, N Suto, Y AF Winn, Joshua N. Holman, Matthew J. Henry, Gregory W. Roussanova, Anna Enya, Keigo Yoshii, Yuzuru Shporer, Avi Mazeh, Tsevi Johnson, John Asher Narita, Norio Suto, Yasushi TI The transit light curve project. V. System parameters and stellar rotation period of HD 189733 SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planetary systems : formation; stars : individual (HD 189733); stars : rotation ID SPIN-ORBIT ALIGNMENT; LIMB-DARKENING LAW; EXTRASOLAR PLANETS; SURFACE GRAVITIES; ATMOSPHERE MODELS; PHOTOMETRY; EXOPLANETS; EVOLUTION; EMISSION; STARS AB We present photometry of HD 189733 during eight transits of its close-in giant planet, and out-of-transit photometry spanning 2 yr. Using the transit photometry, we determine the stellar and planetary radii and the photometric ephemeris. Outside of transits, there are quasi-periodic flux variations with a 13.4 day period that we attribute to stellar rotation. In combination with previous results, we derive upper limits on the orbital eccentricity and on the true angle between the stellar rotation axis and planetary orbit (as opposed to the angle between the projections of those axes on the sky). C1 MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Univ Tokyo, Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan. Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. RP Winn, JN (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 43 TC 109 Z9 109 U1 1 U2 5 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 2007 VL 133 IS 4 BP 1828 EP 1835 DI 10.1086/512159 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 154YF UT WOS:000245543700050 ER PT J AU Cocchia, F Fiore, F Vignali, C Mignoli, M Brusa, M Comastri, A Feruglio, C Baldi, A Carangelo, N Ciliegi, P D'Elia, V La Franca, F Maiolino, R Matt, G Molendi, S Perola, GC Puccetti, S AF Cocchia, F. Fiore, F. Vignali, C. Mignoli, M. Brusa, M. Comastri, A. Feruglio, C. Baldi, A. Carangelo, N. Ciliegi, P. D'Elia, V. La Franca, F. Maiolino, R. Matt, G. Molendi, S. Perola, G. C. Puccetti, S. TI The HELLAS2XMM survey VIII. Optical identifications of the extended sample SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : diffuse background; surveys; galaxies : active; galaxies : evolution ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCES; DEEP FIELD-SOUTH; DIGITAL SKY SURVEY; XMM-NEWTON; SPECTROSCOPIC IDENTIFICATION; MULTIWAVELENGTH OBSERVATIONS; SPECTRAL PROPERTIES; NUMBER COUNTS; SEXSI PROGRAM AB Aims. Hard X-ray, large-area surveys are a fundamental complement to ultra-deep, pencil-beam surveys in obtaining more complete coverage of the AGN luminosity-redshift plane and finding sizeable samples of "rare" AGN. Methods. We present the results of the photometric and spectroscopic identification of 110 hard X-ray selected sources from 5 additional XMM-Newton fields, nearly doubling the original HELLAS2XMM sample. Their 2-10 keV fluxes cover the range 6 x 10(-15)-4 x 10(-13) erg cm(-2) s(-1) and the total area surveyed is similar to 0.5 deg(2) at the bright flux limit. We spectroscopically identified 59 new sources, bringing the spectroscopic completeness of the full HELLAS2XMM sample to almost 70% over a total area of similar to 1.4 deg(-2) at the bright flux limit. We found optical counterparts for 214 out of the 232 X-ray sources of the full sample down to R similar to 25. We measured the flux and luminosity of the [OIII]lambda 5007 emission line for 59 of these sources. Results. Assuming that most high X-ray-to-optical flux ratio sources are obscured QSOs, we used the full HELLAS2XMM sample and the CDF samples to estimate their log N-log S. We find obscured QSOs surface density of 45 15 and 100-350 deg(-2) down to flux limits of 10(-14) and 10(-15) erg cm-2 s-1, respectively. At these flux limits, the fraction of X-ray-selected obscured QSOs turns out to be similar to that of unobscured QSOs. Since X-ray selection misses most Compton-thick AGN, the number of obscured QSOs may well outnumber the unobscured QSOs. We find that hard X-ray selected AGNs with a detected [OIII] emission span a wide range of L2-10 keV/L-[OIII] with a logarithmic median of 2.14 and interquartile range of 0.38. This is marginally higher than for a sample of optically selected AGNs (median 1.69 and interquatile range 0.30), suggesting that optically selected samples are at least partly incomplete and/or that [OIII] emission is not a perfect isotropic indicator of the nuclear power. The seven X-ray bright, optically normal galaxy (XBONG) candidates in the sample have L2-10 keV/L-[OIII] greater than or similar to 1000, while their X-ray and optical luminosities and obscuring column density are similar to those of narrow-line AGNs in the same redshift interval (0.075-0.32). This suggests that, while the central engine of narrow-line AGNs and XBONGs looks similar, the narrow-line region in XBONGs could be strongly inhibited or obscured. C1 Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. INAF, Osservatorio Astron Brera, I-20121 Milan, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. Max Planck Inst Extraterr Phys, MPE, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, CfA, Cambridge, MA 02138 USA. INAF IASF, I-20133 Milan, Italy. Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. ESRIN, ASI Sci Data Ctr, ASDC, I-00044 Frascati, Italy. RP Cocchia, F (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. EM cocchia@brera.mi.astro.it RI La Franca, Fabio/G-9631-2012; Vignali, Cristian/J-4974-2012; Mignoli, Marco/O-9426-2015; Comastri, Andrea/O-9543-2015; OI Fiore, Fabrizio/0000-0002-4031-4157; D'Elia, Valerio/0000-0002-7320-5862; La Franca, Fabio/0000-0002-1239-2721; Brusa, Marcella/0000-0002-5059-6848; Vignali, Cristian/0000-0002-8853-9611; Mignoli, Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970; Ciliegi, Paolo/0000-0002-0447-4620; Puccetti, Simonetta/0000-0002-2734-7835 NR 55 TC 39 Z9 39 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2007 VL 466 IS 1 BP 31 EP 40 DI 10.1051/0004-6361:20065170 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YV UT WOS:000245686700004 ER PT J AU Palau, A Estalella, R Girart, JM Ho, PTP Zhang, Q Beuther, H AF Palau, A. Estalella, R. Girart, J. M. Ho, P. T. P. Zhang, Q. Beuther, H. TI Star formation in a clustered environment around the UCHII region in IRAS 20293+3952 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : individual objects : IRAS 20293+3952; dust, extinction; ISM : clouds ID HIGH-SPATIAL-RESOLUTION; MASS PROTOSTELLAR CANDIDATES; COLLAPSING PRESTELLAR CORES; HERBIG AE/BE STARS; DENSE CORES; MOLECULAR CLOUD; DARK CLOUDS; AMMONIA; ORION; OUTFLOW AB Aims. We aim at studying the cluster environment surrounding the UCH II region in IRAS 20293 + 3952, a region in the first stages of formation of a cluster around a high-mass star. Methods. BIMA and VLA were used to observe the 3 mm continuum, N2H+ (1-0), NH3 ( 1, 1), NH3 ( 2, 2), and CH3OH(2-1) emission of the surroundings of the UCH II region. We studied the kinematics of the region and computed the rotational temperature and column density maps by fitting the hyperfine structure of N2H+ and NH3. Results. The dense gas traced by N2H+ and NH3 shows two different clouds, a main cloud to the east of the UCH II region, of similar to 0.15 pc and similar to 250 M circle dot, and a western cloud, of similar to 0.15 pc and similar to 30 M-circle dot. The dust emission reveals two strong components in the northern side of the main cloud, BIMA 1 and BIMA 2, associated with Young Stellar Objects (YSOs) driving molecular outflows, and two fainter components in the southern side, BIMA 3 and BIMA 4, with no signs of star forming activity. Regarding the CH3OH, we found strong emission in a fork-like structure associated with outflow B, as well as emission associated with outflow A. The YSOs associated with the dense gas seem to have a diversity of age and properties. The rotational temperature is higher in the northern side of the main cloud, around 22 K, where there are most of the YSOs, than in the southern side, around 16 K. There is strong chemical differentiation in the region, since we determined low values of the NH3/N2H+ ratio, similar to 50, associated with YSOs in the north of the main cloud, and high values, up to 300, associated with cores with no detected YSOs, in the south of the main cloud. Such a chemical differentiation is likely due to abundance/depletion effects. Finally, interaction between the different sources in the region is important. First, the UCH II region is interacting with the main cloud, heating it and enhancing the CN( 1-0) emission. Second, outflow A seems to be excavating a cavity and heating its walls. Third, outflow B is interacting with the BIMA 4 core, likely producing the deflection of the outflow and illuminating a clump located similar to 0.2 pc to the northeast of the shock. Conclusions. The star formation process in IRAS 20293+3952 is not obviously associated with interactions, but seems to take place where density is highest. C1 Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Catalunya, Spain. Fac Ciencias, CSIC, Inst Ciencies Espai, IEEC, Bellaterra 08193, Catalunya, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Palau, A (reprint author), Univ Barcelona, Dept Astron & Meteorol, Av Diagonal 647, E-08028 Barcelona, Catalunya, Spain. EM apalau@am.ub.es RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 NR 58 TC 26 Z9 26 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2007 VL 465 IS 1 BP 219 EP 233 DI 10.1051/0004-6361:20065936 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146JM UT WOS:000244930300026 ER PT J AU Ibarra, A Matt, G Guainazzi, M Kuulkers, E Jimenez-Bailon, E Rodriguez, J Nicastro, F Walter, R AF Ibarra, A. Matt, G. Guainazzi, M. Kuulkers, E. Jimenez-Bailon, E. Rodriguez, J. Nicastro, F. Walter, R. TI The XMM-Newton/INTEGRAL monitoring campaign of IGR J16318-4848 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : individuals : IGR J16318-4848; X-rays : binaries; line : formation; accretion, accretion disks ID ACTIVE GALACTIC NUCLEI; X-RAY BINARY; COMPTON SHOULDER; COLD MATTER; NEWTON; IRON; LINE; SPECTRUM; SOLAR AB Context. IGR J16318-4848 is the prototype and one of the more extreme examples of the new class of highly obscured Galactic X-ray sources discovered by INTEGRAL. A monitoring campaign on this source has been carried out using XMM-Newton and INTEGRAL, consisting of three simultaneous observations performed in February, March and August 2004. Aims. The long-term variability of the Compton-thick absorption and emission line complexes will be used to probe the properties of the circumstellar matter. Methods. A detailed timing and spectral analysis of the three observations is performed, along with the reanalysis of the XMM-Newton observation performed in February 2003. The results are compared with predictions from numerical radiative transfer simulations to derive the parameters of the circumstellar matter. Results. Despite the large flux dynamic range observed (almost a factor 3 between observations performed a few months apart), the source remained bright (suggesting it is a persistent source) and Compton-thick (N-H > 1.2 x 10(24) cm(-2)). Large Equivalent Width (EW) emission lines from Fe K-alpha, Fe K-beta and Ni K-alpha were present in all spectra. The addition of a Fe K-alpha Compton Shoulder improves the fits, especially in the 2004 observations. Sporadic occurrences of rapid X-ray flux risings were observed in three of the four observations. The Fe Ka light curve followed the continuum almost instantaneously, suggesting that the emission lines are produced by illumination of small-scale optically-thick matter around the high-energy continuum source. Using the iron line EW and Compton Shoulder as diagnostic of the geometry of the matter, we suggest that the obscuring matter is in a flattened configuration seen almost edge-on. C1 European Space Astron Ctr, INSA, XMM Newton Sci Operat Ctr, Madrid 28080, Spain. Univ Roma Tre, I-0046 Rome, Italy. European Space Astron Ctr, ESA, XMM Newton Sci Operat Ctr, Madrid 28080, Spain. European Space Astron Ctr, ESA, Integral Sci Operat Ctr, Madrid 28080, Spain. Univ Paris 07, CEA Saclay, Serv Astrophys, AIM UMR 7158,CEA CNRS, F-91191 Gif Sur Yvette, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Integral Sci Data Ctr, CH-1290 Versoix, Switzerland. RP Ibarra, A (reprint author), European Space Astron Ctr, INSA, XMM Newton Sci Operat Ctr, Apartado 50727, Madrid 28080, Spain. EM Aitor.Ibarra@sciops.esa.int OI Nicastro, Fabrizio/0000-0002-6896-1364; Rodriguez, Jerome/0000-0002-4151-4468 NR 31 TC 13 Z9 13 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2007 VL 465 IS 2 BP 501 EP 507 DI 10.1051/0004-6361:20066225 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 148WK UT WOS:000245107900017 ER PT J AU Paladini, R Montier, L Giard, M Bernard, JP Dame, TM Ito, S Macias-Perez, JF AF Paladini, R. Montier, L. Giard, M. Bernard, J. P. Dame, T. M. Ito, S. Macias-Perez, J. F. TI A broadband study of galactic dust emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxy : structure; infrared : ISM; ISM : dust, extinction ID INFRARED-EMISSION; INTERSTELLAR DUST; MILKY-WAY; COLD DUST; SPECTRAL OBSERVATIONS; MOLECULAR CLOUDS; HII-REGIONS; GAMMA-RAYS; GALAXY; GRAINS AB We have combined infrared data with H-I, H-2, and H-II surveys to spatially decompose the observed dust emission into components associated with different phases of the gas. An inversion technique is applied. For the decomposition, we use the IRAS 60 and 100 mu m bands, the DIRBE 140 and 240 mu m bands, as well as Archeops 850 and 2096 mu m wavelengths. In addition, we apply the decomposition to all five WMAP bands. We obtain longitude and latitude profiles for each wavelength and for each gas component in carefully selected Galactic radius bins. We also derive emissivity coefficients for dust in atomic, molecular, and ionized gas in each of the bins. The H-I emissivity appears to decrease with increasing Galactic radius indicating that dust associated with atomic gas is heated by the ambient interstellar radiation field (ISRF). By contrast, we find evidence that dust mixed with molecular clouds is significantly heated by O/B stars still embedded in their progenitor clouds. By assuming a modified blackbody with emissivity law lambda(-1.5), we also derive the radial distribution of temperature for each phase of the gas. All of the WMAP bands except W appear to be dominated by emission from something other than normal dust, most likely a mixture of thermal bremstrahlung from diffuse ionized gas, synchrotron emission, and spinning dust. Furthermore, we find indications of an emissivity excess at long wavelengths (lambda >= 850 mu m) in the outer Galaxy (R > 8.9 kpc). This suggests either the existence of a very cold dust component in the outer Galaxy or a temperature dependence of the spectral emissivity index. Finally, it is shown that similar to 80% of the total FIR luminosity is produced by dust associated with atomic hydrogen, in agreement with earlier findings. The work presented here has been carried out as part of the development of analysis tools for the planned European Space Agency (ESA) Planck mission. C1 Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. CALTECH, Spitzer Sci Infrared Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. RP Paladini, R (reprint author), Ctr Etud Spatiale Rayonnements, 9 Ave Colonel Roche,BP 4346, F-31028 Toulouse, France. EM paladini@ipac.caltech.edu NR 68 TC 22 Z9 22 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 APR PY 2007 VL 465 IS 3 BP 839 EP 854 DI 10.1051/0004-6361:20065835 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151LA UT WOS:000245290400017 ER PT J AU Guieu, S Pinte, C Monin, JL Menard, F Fukagawa, M Padgett, DL Noriega-Crespo, A Carey, SJ Rebull, LM Huard, T Guedel, M AF Guieu, S. Pinte, C. Monin, J-L. Menard, F. Fukagawa, M. Padgett, D. L. Noriega-Crespo, A. Carey, S. J. Rebull, L. M. Huard, T. Guedel, M. TI On the circum(sub) stellar environment of brown dwarfs in Taurus SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; stars : low mass, brown dwarfs; stars : pre-main sequence; stars : planetary systems : protoplanetary disks; stars : circumstellar matter ID INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS; INTERSTELLAR DUST GRAINS; SPITZER-SPACE-TELESCOPE; YOUNG SUBSTELLAR OBJECTS; INFRARED ARRAY CAMERA; DYNAMICAL INTERACTIONS; ABSOLUTE CALIBRATION; CIRCUMSTELLAR DISKS; EVOLUTIONARY MODELS AB Aims. We want to investigate whether brown dwarfs (BDs) form like stars or are ejected embryos. We study the presence of disks around BDs in the Taurus cloud, and discuss implications for substellar formation models. Methods. We use photometric measurements from the visible to the far infrared to determine the spectral energy distributions (SEDs) of Taurus BDs. Results. We use Spitzer color indices, Ha as an accretion indicator, and models fit to the SEDs in order to estimate physical parameters of the disks around these BDs. We study the spatial distribution of BDs with and without disks across the Taurus aggregates, and we find that BDs with and without disks are not distributed regularly across the Taurus cloud. Conclusions. We find that 48% +/- 14% of Taurus BDs have a circumstellar disk signature, a ratio similar to recent results from previous authors in other regions. We fit the SEDs and find that none of the disks around BDs in Taurus can be fitted convincingly with a flaring index beta = 0, indicating that heating by the central object is efficient and that the disks we observe retain a significant amount of gas. We find that BDs with disks are proportionally more numerous in the northern Taurus filament, possibly the youngest filament. We do not find such a clear segregation for classical T Tauri stars (CTTS) and weak-lined T Tauri stars (WTTS), suggesting that, in addition to the effects of evolution, any segregation effects could be related to the mass of the object. A by-product of our study is to propose a recalibration of the Barrado y Navascues & Martin (2003) accretion limit in the substellar domain. The global shape of the limit fits our data points if it is raised by a factor 1.25-1.30. C1 Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, F-38041 Grenoble, France. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Paul Scherrer Inst, CH-5232 Villigen, Switzerland. RP Guieu, S (reprint author), Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, BP 53, F-38041 Grenoble, France. EM Sylvain.Guieu@obs.ujf-groenoble.fr RI Guedel, Manuel/C-8486-2015 OI Rebull, Luisa/0000-0001-6381-515X; Guedel, Manuel/0000-0001-9818-0588 NR 64 TC 32 Z9 32 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2007 VL 465 IS 3 BP 855 EP 864 DI 10.1051/0004-6361:20066140 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151LA UT WOS:000245290400018 ER PT J AU Bisschop, SE Jorgensen, JK van Dishoeck, EF de Wachter, EBM AF Bisschop, S. E. Jorgensen, J. K. van Dishoeck, E. F. de Wachter, E. B. M. TI Testing grain-surface chemistry in massive hot-core regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line : identification; methods : observational; stars : formation; ISM : abundances; ISM : molecules ID DENSE INTERSTELLAR CLOUDS; STAR-FORMING REGIONS; ULTRACOMPACT HII-REGIONS; TIME-DEPENDENT CHEMISTRY; VLT SPECTROSCOPIC SURVEY; MOLECULAR LINE EMISSION; ICE ABSORPTION FEATURES; MU-M; ORGANIC-MOLECULES; PROTOSTELLAR ENVELOPES AB Aims. We study the chemical origin of a set of complex organic molecules thought to be produced by grain surface chemistry in high mass young stellar objects (YSOs). Methods. A partial submillimeter line-survey was performed toward 7 high-mass YSOs aimed at detecting H(2)CO, CH(3)OH, CH(2)CO, CH(3)CHO, C(2)H(5)OH, HCOOH, HNCO and NH(2)CHO. In addition, lines of CH(3)CN, C(2)H(5)CN, CH(3)CCH, HCOOCH(3), and CH(3)OCH(3) were observed. Rotation temperatures and beam-averaged column densities are determined. To correct for beam dilution and determine abundances for hot gas, the radius and H(2) column densities of gas at temperatures > 100 K are computed using 850 mu m dust continuum data and source luminosity. Results. Based on their rotation diagrams, molecules can be classified as either cold (< 100 K) or hot (> 100 K). This implies that complex organics are present in at least two distinct regions. Furthermore, the abundances of the hot oxygen-bearing species are correlated, as are those of HNCO and NH(2)CHO. This is suggestive of chemical relationships within, but not between, those two groups of molecules. Conclusions. The most likely explanation for the observed correlations of the various hot molecules is that they are "first generation" species that originate from solid-state chemistry. This includes H(2)CO, CH(3)OH, C(2)H(5)OH, HCOOCH(3), CH(3)OCH(3), HNCO, NH(2)CHO, and possibly CH(3)CN, and C(2)H(5)CN. The correlations between sources implies very similar conditions during their formation or very similar doses of energetic processing. Cold species such as CH(2)CO, CH(3)CHO, and HCOOH, some of which are seen as ices along the same lines of sight, are probably formed in the solid state as well, but appear to be destroyed at higher temperatures. A low level of non-thermal desorption by cosmic rays can explain their low rotation temperatures and relatively low abundances in the gas phase compared to the solid state. The CH(3)CCH abundances can be fully explained by low temperature gas phase chemistry. No cold N-containing molecules are found. C1 Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bisschop, SE (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM bisschop@strw.leidenuniv.nl RI Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 NR 88 TC 120 Z9 120 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2007 VL 465 IS 3 BP 913 EP U123 DI 10.1051/0004-6361:20065963 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151LA UT WOS:000245290400024 ER PT J AU Szalai, T Kiss, LL Meszaros, S Vinko, J Csizmadia, S AF Szalai, T. Kiss, L. L. Meszaros, Sz. Vinko, J. Csizmadia, Sz. TI Physical parameters and multiplicity of five southern close eclipsing binaries SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : binaries : close; stars : binaries : eclipsing; stars : binaries : spectroscopic; stars : binaries : general ID ORBITAL PERIOD MODULATION; CONTACT BINARIES; RADIAL-VELOCITY; XY-LEONIS; ADDITIONAL COMPONENTS; MASS-RATIO; STARS; SYSTEMS; MAJORIS; HIPPARCOS AB Aims. We detected tertiary components of close binaries from spectroscopy and light curve modelling, investigated the light-travel time effect and the possibility of magnetic activity cycles, measured mass ratios for unstudied systems, and derived absolute parameters. Methods. We carried out new photometric and spectroscopic observations of five bright ( < V > < 10.5 mag) close eclipsing binaries, predominantly in the southern skies. We obtained full Johnson BV light curves, which were modelled with the Wilson-Devinney code. Radial velocities were measured with the cross-correlation method using IAU radial velocity standards as spectral templates. Period changes were studied with the O-C method, utilising published epochs of minimum light ( XY Leo) and ASAS photometry ( VZ Lib). Results. For three objects ( DX Tuc, QY Hya, V870 Ara), absolute parameters have been determined for the first time. We spectroscopically detected the tertiary components in XY Leo and VZ Lib and discovered one in QY Hya. For XY Leo we updated the light-time effect parameters and detected a secondary periodicity of about 5100 d in the O-C diagram that may hint at the existence of short-period magnetic cycles. A combination of recent photometric data shows that the orbital period of the tertiary star in VZ Lib is likely to be over 1500 d. QY Hya is a semi-detached X-ray active binary in a triple system with K and M-type components, while V870 Ara is a contact binary with the third smallest spectroscopic mass ratio for a W UMa star to date ( q = 0.082 +/- 0.030). Being close to the theoretical minimum for contact binaries, this small mass ratio suggests that V870 Ara has the potential of constraining evolutionary scenarios of binary mergers. The inferred distances to these systems are compatible with the Hipparcos parallaxes. C1 Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hungarian Acad Sci, Konkoly Observ Budapest, H-1051 Budapest, Hungary. RP Szalai, T (reprint author), Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. EM l.kiss@physics.usyd.edu.au RI Kiss, Laszlo/A-2539-2008; Meszaros, Szabolcs/N-2287-2014; OI Meszaros, Szabolcs/0000-0001-8237-5209; Vinko, Jozsef/0000-0001-8764-7832 NR 73 TC 18 Z9 19 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2007 VL 465 IS 3 BP 943 EP 952 DI 10.1051/0004-6361:20066768 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151LA UT WOS:000245290400027 ER PT J AU Zand, JJMI Jonker, PG Markwardt, CB AF Zand, J. J. M. in 't Jonker, P. G. Markwardt, C. B. TI Six new candidate ultracompact X-ray binaries SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE X-rays : binaries; X-rays : bursts; accretion, accretion disks ID ACCRETING NEUTRON-STARS; FIELD CAMERAS OBSERVATIONS; XMM-NEWTON OBSERVATIONS; RICH DEGENERATE DONORS; GLOBULAR-CLUSTER M15; GALACTIC-CENTER; ORBITAL PERIOD; ANGULAR-DISTRIBUTION; OPTICAL COUNTERPART; DWARF-NOVA AB Ultracompact X-ray binaries ( UCXBs) appear able to sustain accretion onto the compact accretor at rates lower than in wider X-ray binaries. This may be understood by the smaller accretion disks in UCXBs: a lower X-ray luminosity suffices to keep a disk completely ionized through irradiation and, thus, keep the viscosity at a sufficiently high level to allow effective transport of matter to the compact object. We employ this distinguishing factor on data from RXTE and BeppoSAX to identify six new candidate UCXBs, thus increasing the population by one quarter. The candidates are drawn from the population of persistently accreting and type-I X-ray bursting low-mass X-ray binaries. The X-ray bursts establish the low-mass X-ray binary nature and provide a handle on the accretion rate. We find that the low accretion rates are supported by the long burst recurrence times and the hard X-ray spectra of the persistent emission as derived from the 2nd INTEGRAL catalog of soft gamma-ray sources. We discuss the peculiar light curves of some new UCXB candidates. C1 SRON, Netherland Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Utrecht, Inst Astron, NL-3508 TA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. RP Zand, JJMI (reprint author), SRON, Netherland Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM jeanz@sron.nl NR 111 TC 94 Z9 94 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 APR PY 2007 VL 465 IS 3 BP 953 EP 963 DI 10.1051/0004-6361:20066678 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151LA UT WOS:000245290400028 ER PT J AU Chakrabarti, S Cox, TJ Hernquist, L Hopkins, PF Robertson, B Di Matteo, T AF Chakrabarti, Sukanya Cox, T. J. Hernquist, Lars Hopkins, Philip F. Robertson, Brant Di Matteo, Tiziana TI Feedback-driven evolution of the far-infrared spectral energy distributions of luminous and ultraluminous infrared galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : formation; galaxies : starburst; infrared : galaxies; radiative : transfer; stars : formation ID PARTICLE HYDRODYNAMICS SIMULATIONS; ACTIVE GALACTIC NUCLEI; 2-DIMENSIONAL RADIATIVE-TRANSFER; TRANSIENTLY HEATED PARTICLES; SUPERMASSIVE BLACK-HOLES; STAR-FORMATION HISTORY; X-RAY-EMISSION; LOCAL UNIVERSE; COSMOLOGICAL SIMULATIONS; TEMPERATURE-FLUCTUATIONS AB We calculate infrared spectral energy distributions (SEDs) from simulations of major galaxy mergers, and study the effect of active galactic nucleus (AGN) and starburst-driven feedback on the evolution of the SED as a function of time. We use a self-consistent three-dimensional radiative equilibrium code to calculate the emergent SEDs and to make images. To facilitate a simple description of our findings, we describe our results in reference to an approximate analytic solution for the far-IR SED. We focus mainly on the luminous infrared galaxy (LIRG) and ultraluminous infrared galaxy (ULIRG) phases of evolution. We contrast the SEDs of simulations performed with AGN feedback to simulations performed with starburst-driven wind feedback. We find that the feedback processes critically determine the evolution of the SED. Changing the source of illumination ( whether stellar or AGN) has virtually no impact on the reprocessed far-infrared SED. We find that AGN feedback is particularly effective at dispersing gas and rapidly injecting energy into the ISM. The observational signature of such powerful feedback is a warm SED. In general, simulations performed with starburst-driven winds have colder spectra and reprocess more of their emission into the infrared, resulting in higher infrared to bolometric luminosities compared to (otherwise equivalent) simulations performed with AGN feedback. We depict our results in IRAS, as well as in Spitzer's MIPS bands, and in Herschel's PACS bands. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Chakrabarti, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM schakrabarti@cfa.harvard.edu RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 97 TC 32 Z9 32 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 2007 VL 658 IS 2 BP 840 EP 850 DI 10.1086/510113 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BE UT WOS:000245405900014 ER PT J AU Sawada-Satoh, S Ho, PTP Muller, S Matsushita, S Lim, J AF Sawada-Satoh, S. Ho, P. T. P. Muller, S. Matsushita, S. Lim, J. TI Structure and kinematics of CO J=2-1 emission in the central region of NGC 4258 SO ASTROPHYSICAL JOURNAL LA English DT Article ID SPIRAL GALAXY NGC-4258; NGC 4258; ANOMALOUS ARMS; MOLECULAR GAS; PHYSICAL CONDITIONS; SEYFERT-GALAXIES; STAR-FORMATION; BRAIDED JETS; MASS; LUMINOSITY AB We present (CO)-C-12 J=2-1 observations toward the central region of the type 2 Seyfert galaxy NGC 4258 with the Submillimeter Array (SMA). Our interferometric maps show two armlike elongated components along the major axis of the galaxy, with no strong nuclear concentration. The CO(2-1) morphology and kinematics are similar to previous CO(1-0) results. The velocity field of the components agrees with the general galactic rotation, except for the east elongated component, which shows a significant velocity gradient along the east-west direction. In order to account for the velocity field, we propose a kinematical model in which the warped rotating disk is also expanding. The line ratio of CO(2-1)/CO(1-0) reveals that the eastern component with the anomalous velocity gradient appears to be warmer and denser. This is consistent with the gas in this component being closer to the center, being heated by the central activities, and possibly interacting with expanding motions from the nuclear region. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sawada-Satoh, S (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. OI /0000-0002-9931-1313 NR 42 TC 6 Z9 6 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 2007 VL 658 IS 2 BP 851 EP 858 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BE UT WOS:000245405900015 ER PT J AU Konopelko, A Atkins, RW Blaylock, G Buckley, JH Butt, Y Carter-Lewis, DA Celik, O Cogan, P Chow, YCK Cui, W Dowdall, C Ergin, T Falcone, AD Fegan, DJ Fegan, SJ Finley, JP Fortin, P Gillanders, GH Gutierrez, KJ Hall, J Hanna, D Horan, D Hughes, SB Humensky, TB Imran, A Jung, I Kaaret, P Kenny, GE Kertzman, M Kieda, DB Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Moriarty, P Mukherjee, R Nagai, T Ong, RA Perkins, JS Pohl, M Ragan, K Reynolds, PT Rose, HJ Sembroski, GH Schrodter, M Smith, AW Steele, D Syson, A Swordy, SP Toner, JA Valcarcel, L Vassiliev, VV Wagner, RG Wakely, SP Weekes, TC White, RJ Williams, DA Zitzer, B AF Konopelko, A. Atkins, R. W. Blaylock, G. Buckley, J. H. Butt, Y. Carter-Lewis, D. A. Celik, O. Cogan, P. Chow, Y. C. K. Cui, W. Dowdall, C. Ergin, T. Falcone, A. D. Fegan, D. J. Fegan, S. J. Finley, J. P. Fortin, P. Gillanders, G. H. Gutierrez, K. J. Hall, J. Hanna, D. Horan, D. Hughes, S. B. Humensky, T. B. Imran, A. Jung, I. Kaaret, P. Kenny, G. E. Kertzman, M. Kieda, D. B. Kildea, J. Knapp, J. Kosack, K. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Moriarty, P. Mukherjee, R. Nagai, T. Ong, R. A. Perkins, J. S. Pohl, M. Ragan, K. Reynolds, P. T. Rose, H. J. Sembroski, G. H. Schroedter, M. Smith, A. W. Steele, D. Syson, A. Swordy, S. P. Toner, J. A. Valcarcel, L. Vassiliev, V. V. Wagner, R. G. Wakely, S. P. Weekes, T. C. White, R. J. Williams, D. A. Zitzer, B. CA VERITAS Collaboration TI Observations of the unidentified TeV gamma-ray source TeV J2032+4130 with the Whipple Observatory 10 m telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations; radiation mechanisms : nonthermal ID ATMOSPHERIC CHERENKOV TELESCOPE; STELLAR WINDS; CRAB-NEBULA; CYGNUS OB2; MILKY-WAY; FOLLOW-UP; ENERGIES; EMISSION; SEARCH; SYSTEM AB We report on observations of the sky region around the unidentified TeV gamma-ray source (TeV J2032+ 4130) carried out with the Whipple Observatory 10 m atmospheric Cerenkov telescope for a total of 65.5 hr between 2003 and 2005. The standard two-dimensional analysis developed by the Whipple collaboration for a stand-alone telescope reveals an excess in the field of view at a pretrial significance level of 6.1 sigma. The measured position of this excess is alpha = 20(h)32(m)27(s), delta = 41 degrees 39'17" (J2000.0). The estimated integral flux for this gamma-ray source is about 8% of the Crab Nebula flux. The data are consistent with a pointlike source. Here we present a detailed description of the standard two-dimensional analysis technique used for the analysis of data taken with the Whipple Observatory 10 m telescope and the results for the TeV J2032+ 4130 campaign. We include a short discussion of the physical mechanisms that may be responsible for the observed gamma-ray emission, based on possible association with known astrophysical objects, in particular, Cygnus OB2. C1 Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Smithsonian Astrophys Observ, Cambridge, MA USA. Iowa State Univ, Dept Phys & Astron, Ames, IA USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA. Univ Coll Dublin, Sch Phys, Dublin 2, Ireland. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. McGill Univ, Dept Phys, Montreal, PQ H3A 2T5, Canada. Harvard Smithsonian Ctr Astrophys, Fres Lawrence Whipple Observ, Amado, AZ USA. RP Konopelko, A (reprint author), Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. EM akonopel@purdue.edu RI Hall, Jeter/E-9294-2015; OI Cui, Wei/0000-0002-6324-5772 NR 30 TC 17 Z9 17 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 2007 VL 658 IS 2 BP 1062 EP 1068 DI 10.1086/511262 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BE UT WOS:000245405900030 ER PT J AU Zhang, QZ Hunter, TR Beuther, H Sridharan, TK Liu, SY Su, YN Chen, HR Chen, Y AF Zhang, Qizhou Hunter, Todd R. Beuther, H. Sridharan, T. K. Liu, S. -Y. Su, Y. -N. Chen, H. -R. Chen, Y. TI Multiple jets from the high-mass (proto) stellar cluster AFGL 5142 SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : clouds; ISM : individual (AFGL 5142); ISM : kinematics and dynamics; masers; stars : formation ID STAR-FORMING REGION; ORION NEBULA CLUSTER; HERBIG-HARO OBJECTS; MOLECULAR OUTFLOW; HOT CORE; SUBMILLIMETER ARRAY; IRAS 20126+4104; H2O MASERS; INFRARED SOURCES; EMISSION AB We present studies of the massive protocluster AFGL 5142 in the J = 2-1 transition of the CO isotopologues, SO, CH3OH, and CH3CN lines, as well as in the continuum at 225 GHz and 8.4 GHz. The 225 GHz continuum emission reveals at least five dust continuum peaks. The strongest peaks, MM-1 and MM-2, are associated with hot cores with temperatures of 90 +/- 20 and 250 +/- 40 K, respectively. With similar core mass, the higher temperature and CH3CN abundance in the MM-2 core suggest that it might be at a more evolved stage than the MM-1 core. A total of 22 lines from nine molecules are detected. The line strength varies remarkably in the region. Strong SO emission is found both in molecular outflows and cloud cores. CH3OH emission, on the contrary, is much weaker in molecular outflows, and is detected toward hot cores MM-1 and MM-2, but is absent in the less massive and perhaps less evolved cores MM-3, MM-4, and MM-5. The CO and SO emission reveals at least three molecular outflows originating from the center of the dust core. The outflows are well collimated, with terminal velocities up to 50 km s(-1) from the cloud velocity. Since jetlike outflows and disk-mediated accretion process are physically connected, the well-collimated outflows indicate that even in this cluster environment, accretion is responsible for the formation of individual stars in the cluster. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, Hamburg, Germany. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. RP Zhang, QZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 59 TC 45 Z9 45 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 2007 VL 658 IS 2 BP 1152 EP 1163 DI 10.1086/511381 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BE UT WOS:000245405900039 ER PT J AU Moro-Martin, A Carpenter, JM Meyer, MR Hillenbrand, LA Malhotra, R Hollenbach, D Najita, J Henning, T Kim, JS Bouwman, J Silverstone, MD Hines, DC Wolf, S Pascucci, I Mamajek, EE Lunine, J AF Moro-Martin, Amaya Carpenter, John M. Meyer, Michael R. Hillenbrand, Lynne A. Malhotra, Renu Hollenbach, David Najita, Joan Henning, Thomas Kim, Jinyoung S. Bouwman, Jeroen Silverstone, Murray D. Hines, Dean C. Wolf, Sebastian Pascucci, Ilaria Mamajek, Eric E. Lunine, Jonathan TI Are debris disks and massive planets correlated? SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; Kuiper Belt; infrared : stars; planetary systems; stars : individual (HD 6434, HD 38529, HD 80606, HD 92788, HD 106252, HD 121504, HD 141937, HD 150706, HD 179949, HD 190228) ID SPITZER-SPACE-TELESCOPE; EXTRA-SOLAR PLANETS; INFRARED ARRAY CAMERA; KUIPER-BELT DUST; ABUNDANCE ANALYSES; GIANT PLANETS; PARENT STARS; F-DWARF; EVOLUTION; SYSTEMS AB Using data from the Spitzer Space Telescope Legacy Science Program Formation and Evolution of Planetary Systems (FEPS), we have searched for debris disks around nine FGK stars (2-10 Gyr), known from radial velocity ( RV) studies to have one or more massive planets. Only one of the sources, HD 38529, has excess emission above the stellar photosphere; at 70 mu m the signal-to-noise ratio in the excess is 4.7, while at lambda < 30 mu m there is no evidence of excess. The remaining sources show no excesses at any Spitzer wavelengths. Applying survival tests to the FEPS sample and the results for the FGK survey recently published in Bryden et al., we do not find a significant correlation between the frequency and properties of debris disks and the presence of close-in planets. We discuss possible reasons for the lack of a correlation. C1 Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Natl Opt Astron Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, Heidelberg, Germany. Space Sci Inst, Boulder, CO 80301 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moro-Martin, A (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM amaya@astro.princeton.edu OI Malhotra, Renu/0000-0002-1226-3305 NR 68 TC 61 Z9 61 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 2007 VL 658 IS 2 BP 1312 EP 1321 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BE UT WOS:000245405900052 ER PT J AU Charbonneau, D Winn, JN Everett, ME Latham, DW Holman, MJ Esquerdo, GA O'Donovan, FT AF Charbonneau, David Winn, Joshua N. Everett, Mark E. Latham, David W. Holman, Matthew J. Esquerdo, Gilbert A. O'Donovan, Francis T. TI Precise radius estimates for the exoplanets WASP-1b and WASP-2b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : individual (WASP-1, WASP-2); techniques : photometric ID EXTRASOLAR GIANT PLANETS; LIGHT-CURVE PROJECT; HD 209458B; TRANSITING PLANET; UPPER LIMIT; TAU-BOOTIS; PHOTOMETRY; STARLIGHT; SEARCH; STAR AB We present precise z-band photometric time series spanning times of transit of the two exoplanets recently discovered by the SuperWASP collaboration. We find planetary radii of 1.44 +/- 0.08 and 1.04 +/- 0.06 R-J for WASP-1b and WASP-2b, respectively. These error estimates include both random errors in the photometry and also the uncertainty in the stellar masses. Our results are 5 times more precise than the values derived from the discovery data alone. Our measurement of the radius of WASP-2b agrees with previously published models of hot Jupiters that include both a 20 M-circle plus core of solid material and the effects of stellar insolation. In contrast, we find that the models cannot account for the large size of WASP-1b, even if the planet has no core. Thus, we add WASP-1b to the growing list of hot Jupiters that are larger than expected. This suggests that "inflated'' hot Jupiters are more common than previously thought and that any purported explanations involving highly unusual circumstances are disfavored. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Planetary Sci Inst, Tucson, AZ 85719 USA. CALTECH, Pasadena, CA 91107 USA. RP Charbonneau, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dcharbonneau@cfa.harvard.edu RI O'Donovan, Francis/I-2423-2014; OI O'Donovan, Francis/0000-0002-4858-6106; Charbonneau, David/0000-0002-9003-484X NR 42 TC 48 Z9 48 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 2007 VL 658 IS 2 BP 1322 EP 1327 DI 10.1086/512008 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BE UT WOS:000245405900053 ER PT J AU Croll, B Matthews, JM Rowe, JF Kuschnig, R Walker, A Gladman, B Sasselov, D Cameron, C Walker, GAH Lin, DNC Guenther, DB Moffat, AFJ Rucinski, SM Weiss, WW AF Croll, Bryce Matthews, Jaymie M. Rowe, Jason F. Kuschnig, Rainer Walker, Andrew Gladman, Brett Sasselov, Dimitar Cameron, Chris Walker, Gordon A. H. Lin, Douglas N. C. Guenther, David B. Moffat, Anthony F. J. Rucinski, Slavek M. Weiss, Werner W. TI Looking for giant Earths in the HD 209458 system: A search for transits in MOST space-based photometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; planetary systems ID SUN-LIKE STAR; HD 209458B; EXTRASOLAR PLANETS; TERRESTRIAL PLANETS; KEPLER MISSION; FIELD; LIMIT; ASTEROSEISMOLOGY; PARAMETERS; CLUSTERS AB We have made a comprehensive transit search for exoplanets down to about 2 Earth radii in the HD 209458 system, based on nearly uninterrupted broadband optical photometry obtained with the MOST (Microvariability and Oscillations of Stars) satellite, spanning 14 days in 2004 and 44 days in 2005. We have searched these data for limb-darkened transits at periods other than that of the known giant planet, from about 0.5 days to 2 weeks. Monte Carlo statistical tests of the data with synthetic transits inserted allow us to rule out additional close- in exoplanets with sizes ranging from about 0.20-0.36 R-J ( Jupiter radii), or 2.2-4.0 R-circle plus ( Earth radii) on orbits whose planes are near that of HD 209458b. These null results constrain theories that invoke lower mass planets in orbits similar to HD 209458b to explain its anomalously large radius, and those that predict "hot Earths'' due to the inward migration of HD 209458b. C1 Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Montreal, Dept Phys, Observ Mont Megnat, Montreal, PQ, Canada. Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Croll, B (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. EM croll@astro.utoronto.ca; matthews@phas.ubc.ca; rowe@phas.ubc.ca; kuschnig@phas.ubc.ca; arwalker@sumusltd.com; gladman@phas.ubc.ca; sasselov@cfa.harvard.edu; ccameron@phas.ubc.ca; gordonwa@uvic.ca; lin@ucolick.org; guenther@ap.stmarys.ca; moffat@astro.umontreal.ca; rucinski@astro.utoronto.ca; weiss@astro.univie.ac.at NR 47 TC 20 Z9 20 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 2007 VL 658 IS 2 BP 1328 EP 1339 DI 10.1086/511521 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BE UT WOS:000245405900054 ER PT J AU Grillmair, CJ Charbonneau, D Burrows, A Armus, L Stauffer, J Meadows, V Van Cleve, J Levine, D AF Grillmair, C. J. Charbonneau, D. Burrows, A. Armus, L. Stauffer, J. Meadows, V. Van Cleve, J. Levine, D. TI A Spitzer spectrum of the exoplanet HD 189733b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; planetary systems; stars : individual (HD 189733) ID EXTRASOLAR PLANET; HOT JUPITERS; THERMAL EMISSION; LIGHT CURVES; ATMOSPHERES; HD-189733; DYNAMICS; SEARCH AB We report on the measurement of the 7.5 - 14.7 mu m spectrum for the transiting extrasolar giant planet HD 189733b using the Infrared Spectrograph on the Spitzer Space Telescope. Although the observations comprise only 12 hr of telescope time, the continuum is well measured and has a flux ranging from 0.6 to 1.8 mJy over the wavelength range, or of the flux of the parent star. The variation in the measured fractional 0.49% +/- 0.02% flux is very nearly flat over the entire wavelength range and shows no indication of significant absorption by water or methane, in contrast with the predictions of most atmospheric models. Models with strong day/night differences appear to be disfavored by the data, suggesting that heat redistribution to the night side of the planet is highly efficient. C1 Spitzer Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Ball Aerosp & Technol Corp, Boulder, CO 80306 USA. RP Grillmair, CJ (reprint author), Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM carl@ipac.caltech.edu; dcharbon@ipac.caltech.edu; burrows@as.arizona.edu; lee@ipac.caltech.edu; staufer@ipac.caltech.edu; vsm@ipac.caltech.edu; jvanclev@ball.com; deblev@ipac.caltech.edu NR 18 TC 116 Z9 118 U1 1 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 2007 VL 658 IS 2 BP L115 EP L118 DI 10.1086/513741 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BF UT WOS:000245406000012 ER PT J AU Lin, J Li, J Forbes, TG Ko, YK Raymond, JC Vourlidas, A AF Lin, J. Li, J. Forbes, T. G. Ko, Y. -K. Raymond, J. C. Vourlidas, A. TI Features and properties of coronal mass ejection/flare current sheets SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffusion; Sun : flares; Sun : magnetic fields; turbulence ID MAGNETIC RECONNECTION; SOLAR ERUPTIONS; ACTIVE-REGION; ACCELERATION; SIMULATION; SPECTRA; FLARES; LINES AB Solar eruptions occur when magnetic energy is suddenly converted into heat and kinetic energy by magnetic reconnection in a current sheet ( CS). It is often assumed that CSs are too thin to be observable because the electric resistivity n(e) in CSs is taken to be very small. In this work, we show the implications for the CS thickness d estimated from observations of three eruptions by the UVCS and the LASCO experiments on SOHO. We infer the effective n(e) causing the rapid reconnection, which predicts much faster reconnection in a thick CS than that caused by the classical and anomalous resistivities. We find that in these events CSs are observable and have extremely large values of d and n(e), implying that large-scale turbulence is operating within CSs. We also discuss the properties of the so-called hyperresistivity caused by the tearing mode and the relation to our results. C1 Chinese Acad Sci, Natl Astron Observ, China Yunnan Astron Observ, Kunming 650011, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. USN, Res Lab, Washington, DC 20375 USA. RP Lin, J (reprint author), Chinese Acad Sci, Natl Astron Observ, China Yunnan Astron Observ, Kunming 650011, Peoples R China. RI Vourlidas, Angelos/C-8231-2009; LIN, JUN/B-9890-2017 OI Vourlidas, Angelos/0000-0002-8164-5948; NR 27 TC 52 Z9 59 U1 2 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2007 VL 658 IS 2 BP L123 EP L126 DI 10.1086/515568 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BF UT WOS:000245406000014 ER PT J AU Schmelz, JT Nasraoui, K Del Zanna, G Cirtain, JW DeLuca, EE Mason, HE AF Schmelz, J. T. Nasraoui, K. Del Zanna, G. Cirtain, J. W. DeLuca, E. E. Mason, H. E. TI Coronal diagnostic spectrometer observations of isothermal and multithermal coronal loops SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : corona; sun : fundamental parameters; sun : UV radiation ID SOHO-CDS OBSERVATIONS; SOLAR CORONA; TEMPERATURE-MEASUREMENTS; ATOMIC DATABASE; EMISSION-LINES; ACTIVE-REGION; CHIANTI; MODELS; PLASMA; FILTER AB A data set obtained on 2003 January 17 with the Coronal Diagnostic Spectrometer (CDS) shows two loops sitting side by side on the solar disk. These loops are oriented along the CDS slit, so all pixels in each loop were observed simultaneously. So, although the instrument has a relatively slow time cadence, changes as a function of time that may occur during the CDS raster buildup will not affect the loop temperature results. Differential emission measure (DEM) analysis using a forward-folding technique shows different results for the two loops. For the first loop, the intensities of the lines that remain after background subtraction are well fit with a DEM curve that collapses to a single spike. In other words, the loop plasma at this location is isothermal. This analysis is confirmed with an emission measure loci method and agrees with the results obtained recently by other authors that show that the moderate spatial resolution of CDS can detect isothermal structures. For the second loop, the background-subtracted line intensities require a broad DEM, not consistent with isothermal plasma. This conclusion is confirmed with an automatic-inversion DEM method. In this Letter, we specifically address some of the concerns raised about CDS temperature analysis: the slow CDS temporal resolution, the moderate CDS spatial resolution, the inherent smoothing associated with DEM inversion, and line-of-sight effects on the DEM distribution. C1 Univ Memphis, Dept Phys, Memphis, TN 38152 USA. UCL, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. DAMTP, Ctr Math Sci, Cambridge CB3 OWA, England. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu; kaouther2001@yahoo.com; G.Del-Zanna@damtp.cam.ac.uk; jcirtain@cfa.harvard.edu; edeluca@cfa.harvard.edu; H.E.Mason@damtp.cam.ac.uk RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 NR 26 TC 18 Z9 18 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 APR 1 PY 2007 VL 658 IS 2 BP L119 EP L122 DI 10.1086/514815 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BF UT WOS:000245406000013 ER PT J AU Worrall, DM Birkinshaw, M Kraft, RP Hardcastle, MJ AF Worrall, D. M. Birkinshaw, M. Kraft, R. P. Hardcastle, M. J. TI The effect of a Chandra-measured merger-related gas component on the lobes of a dead radio galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual ( NGC 7237, 3C 442A); galaxies : interactions; radio continuum : galaxies; X-rays : galaxies ID INTERACTING BINARY GALAXIES; X-RAY-EMISSION; NGC-7236/7237; NGC-1587/1588 AB We use Chandra data to infer that an X-ray-bright component of gas is in the process of separating the radio lobes of 3C 442A. This is the first radio galaxy with convincing evidence that central gas, overpressured with respect to the lobe plasma and not simply a static atmosphere, is having a major dynamical effect on the radio structure. We speculate that the expansion of the gas also reexcites electrons in the lobes of 3C 442A through compression and adiabatic heating. Two features of 3C 442A contribute to its dynamical state. First, the radio source is no longer being powered by a detected active jet, so that the dynamical state of the radio plasma is at the mercy of the ambient medium. Second, the two early-type galaxies, NGC 7236 and NGC 7237, one of which was the original host of 3C 442A, are undergoing a merger and have already experienced a close encounter, suggesting that the X-ray-bright gas is mostly the heated combined galaxy atmospheres. The lobes have been swept apart for similar to 10(8) yr by the pressure-driven expansion of the X-ray-bright inner gas. C1 Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. RP Worrall, DM (reprint author), Univ Bristol, Dept Phys, Royal Ft, Bristol BS8 1TL, Avon, England. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 17 TC 12 Z9 12 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2007 VL 658 IS 2 BP L79 EP L82 DI 10.1086/513869 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BF UT WOS:000245406000003 ER PT J AU Kim, M Kim, DW Wilkes, BJ Green, PJ Kim, E Anderson, CS Barkhouse, WA Evans, NR Ivezic, Z Karovska, M Kashyap, VL Lee, MG Maksym, P Mossman, AE Silverman, JD Tananbaum, HD AF Kim, Minsun Kim, Dong-Woo Wilkes, Belinda J. Green, Paul J. Kim, Eunhyeuk Anderson, Craig S. Barkhouse, Wayne A. Evans, Nancy R. Ivezic, Zeljko Karovska, Margarita Kashyap, Vinay L. Lee, Myung Gyoon Maksym, Peter Mossman, Amy E. Silverman, John D. Tananbaum, Harvey D. TI Chandra multiwavelength project X-ray point source catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; surveys; X-rays : general ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; OPTICAL SURVEY; LOCKMAN-HOLE; NORTH SURVEY; GALAXIES; POPULATION; EXPOSURE AB We present the Chandra Multiwavelength Project (ChaMP) X-ray point source catalog with similar to 6800 X-ray sources detected in 149 Chandra observations covering similar to 10 deg(2). The full ChaMP catalog sample is 7 times larger than the initial published ChaMP catalog. The exposure time of the fields in our sample ranges from 0.9 to 124 ks, corresponding to a deepest X-ray flux limit of f(0.5-8.) = 9 x 10(-16) ergs cm(-2) s(-1). The ChaMP X-ray data have been uniformly reduced and analyzed with ChaMP-specific pipelines and then carefully validated by visual inspection. The ChaMP catalog includes X-ray photometric data in eight different energy bands as well as X-ray spectral hardness ratios and colors. To best utilize the ChaMP catalog, we also present the source reliability, detection probability, and positional uncertainty. To quantitatively assess those parameters, we performed extensive simulations. In particular, we present a set of empirical equations: the flux limit as a function of effective exposure time and the positional uncertainty as a function of source counts and off-axis angle. The false source detection rate is similar to 1% of all detected ChaMP sources, while the detection probability is better than similar to 95% for sources with counts greater than or similar to 30 and off-axis angle < 5'. The typical positional offset between ChaMP X-ray source and their SDSS optical counterparts is 0.7 '' +/- 0.4 '', derived from similar to 900 matched sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Max Planck Inst Extraterr Phys, D-84571 Garching, Germany. RP Kim, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mkim@cfa.harvard.edu OI Maksym, Walter/0000-0002-2203-7889; Wilkes, Belinda/0000-0003-1809-2364 NR 33 TC 76 Z9 77 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2007 VL 169 IS 2 BP 401 EP 429 DI 10.1086/511634 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 153BB UT WOS:000245405600010 ER PT J AU Gelfand, JD AF Gelfand, Joseph D. TI The radio nebula produced by the 27 December 2004 giant flare from SGR 1806-20 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE pulsars : individual SGR 1806-20; pulsars : general ID SGR 1806-20; MAGNETAR SGR-1806-20; RADIATIVE MECHANISM; COUNTERPART AB On 27 December 2004, just the third giant flare was observed from a magnetar, in this case SGR 1806-20. This giant flare was the most energetic of the three, and analysis of a Very Large Array observation of SGR 1806-20 after the giant flare revealed the existence of a new, bright, transient radio source at its position. Follow-up radio observations of this source determined that initially, this source underwent a mildly relativistic one-sided expansion which ceased at the same time as a temporary rebrightening of the radio source. These observational results imply that the radio emission is powered by similar to 10(24) g of baryonic material which was ejected off the surface on the neutron star during the giant flare. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gelfand, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jgelfand@cfa.harvard.edu NR 11 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 APR PY 2007 VL 308 IS 1-4 BP 39 EP 42 DI 10.1007/s10509-007-9317-y PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166BC UT WOS:000246351000005 ER PT J AU Gonzalez, ME Kaspi, VM Camilo, F Gaensler, BM Pivovaroff, MJ AF Gonzalez, M. E. Kaspi, V. M. Camilo, F. Gaensler, B. M. Pivovaroff, M. J. TI PSR J1119-6127 and the X-ray emission from high magnetic field radio pulsars SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE ISM : individual (G292.2-0.5); pulsars : individual (PSR J1119-6127); X-rays : ISM ID SUPERNOVA REMNANT G292.2-0.5; NEUTRON-STARS; J1119-6127; YOUNG; SPECTROSCOPY; DISCOVERY AB The existence of radio pulsars having inferred magnetic fields in the magnetar regime suggests that possible transition objects could be found in the radio pulsar population. The discovery of such an object would contribute greatly to our understanding of neutron star physics. Here we report on unusual X-ray emission detected from the radio pulsar PSR J1119-6127 using XMM-Newton. The pulsar has a characteristic age of 1,700 yrs and inferred surface dipole magnetic field strength of 4.1x10(13) G. In the 0.5-2.0 keV range, the emission shows a single, narrow pulse with an unusually high pulsed fraction of similar to 70%. No pulsations are detected in the 2.0-10.0 keV range, where we derive an upper limit at the 99% level for the pulsed fraction of 28%. The pulsed emission is well described by a thermal blackbody model with a high temperature of similar to 2.4x10(6) K. While no unambiguous signature of magnetar-like emission has been found in high-magnetic-field radio pulsars, the X-ray characteristics of PSR J1119-6127 require alternate models from those of conventional thermal emission from neutron stars. In addition, PSR J1119-6127 is now the radio pulsar with the smallest characteristic age from which thermal X-ray emission has been detected. C1 McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Gonzalez, ME (reprint author), McGill Univ, Dept Phys, Rutherford Phys Bldg, Montreal, PQ H3A 2T8, Canada. EM gonzalez@physics.mcgill.ca RI Gaensler, Bryan/F-8655-2010; Pivovaroff, Michael/M-7998-2014; OI Pivovaroff, Michael/0000-0001-6780-6816; Gaensler, Bryan/0000-0002-3382-9558 NR 31 TC 5 Z9 5 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD APR PY 2007 VL 308 IS 1-4 BP 89 EP 94 DI 10.1007/s10509-007-9305-2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166BC UT WOS:000246351000012 ER PT J AU Gaensler, BM McLaughlin, M Reynolds, S Borkowski, K Rea, N Possenti, A Israel, G Burgay, M Camilo, F Chatterjee, S Kramer, M Lyne, A Stairs, I AF Gaensler, Bryan M. McLaughlin, Maura Reynolds, Stephen Borkowski, Kazik Rea, Nanda Possenti, Andrea Israel, Gianluca Burgay, Marta Camilo, Fernando Chatterjee, Shami Kramer, Michael Lyne, Andrew Stairs, Ingrid TI Chandra smells a RRAT SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE pulsars : individual (J1819-1458); stars : flare, neutron; X-rays : stars ID ROTATING RADIO TRANSIENT; X-RAY-EMISSION; NEUTRON-STARS; PULSAR; DISCOVERY; YOUNG AB "Rotating RAdio Transients" (RRATs) are a newly discovered astronomical phenomenon, characterised by occasional brief radio bursts, with average intervals between bursts ranging from minutes to hours. The burst spacings allow identification of periodicities, which fall in the range 0.4 to 7 seconds. The RRATs thus seem to be rotating neutron stars, albeit with properties very different from the rest of the population. We here present the serendipitous detection with the Chandra X-ray Observatory of a bright point-like X-ray source coincident with one of the RRATs. We discuss the temporal and spectral properties of this X-ray emission, consider counterparts in other wavebands, and interpret these results in the context of possible explanations for the RRAT population. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. W Virginia Univ, Morgantown, WV 26506 USA. N Carolina State Univ, Raleigh, NC 27695 USA. SRON, Netherlands Inst Space Res, Utrecht, Netherlands. Osservatorio Astron Cagliari, Cagliari, Italy. Osserv Astron Roma, I-00136 Rome, Italy. Columbia Univ, New York, NY USA. Jodrell Bank Observ, Macclesfield, Cheshire, England. Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. RP Gaensler, BM (reprint author), Univ Sydney, Sydney, NSW 2006, Australia. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; Rea, Nanda/I-2853-2015; OI Rea, Nanda/0000-0003-2177-6388; Burgay, Marta/0000-0002-8265-4344; Israel, GianLuca/0000-0001-5480-6438; Gaensler, Bryan/0000-0002-3382-9558 NR 21 TC 6 Z9 6 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 APR PY 2007 VL 308 IS 1-4 BP 95 EP 99 DI 10.1007/s10509-007-9352-8 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166BC UT WOS:000246351000013 ER PT J AU Weisskopf, MC Karovska, M Pavlov, GG Zavlin, VE Clarke, T AF Weisskopf, M. C. Karovska, M. Pavlov, G. G. Zavlin, V. E. Clarke, T. TI Chandra observations of neutron stars: an overview SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE X-ray astronomy; neutron stars; SNR; crab pulsar; vela pulsar; IC443; B1509-58; 1E 1207.4-5209; SNR 292.0+1.8; 3C58; SNR 1987A; RX J1856.5-3754 ID PULSAR WIND NEBULA; X-RAY-EMISSION; SUPERNOVA REMNANT G292.0+1.8; CRAB-NEBULA; SYNCHROTRON NEBULA; XMM-NEWTON; MAGNETIC-FIELD; 3C 58; 1E-1207.4-5209; ABSORPTION AB We present an overview of Chandra X-ray Observatory observations of neutron stars. The outstanding spatial and spectral resolution of this great observatory have allowed for observations of unprecedented clarity and accuracy. Many of these observations have provided new insights into neutron star physics. We present an admittedly biased and overly brief review of these observations, highlighting some new discoveries made possible by the Observatory's unique capabilities. This includes our analysis of recent multiwavelength observations of the putative pulsar and its pulsar-wind nebula in the IC443 SNR. C1 Smithsonian Astrophy Observ, Cambridge, MA 02138 USA. Penn State Univ, Davey Lab 525, University Pk, PA 16802 USA. Natl Space Sci Technol Ctr, Huntsville, AL 35805 USA. USN, Res Lab, Code 7213, Washington, DC 20375 USA. Interferometr Inc, Herndon, VA 20171 USA. EM martin@smoker.msfc.nasa.gov; karovska@head.cfa.harvard.edu; pavlov@astro.psu.edu; slava.zavlin@nsstc.nasa.gov; tracy.clarke@nrl.navy.mil NR 65 TC 8 Z9 8 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 APR PY 2007 VL 308 IS 1-4 BP 151 EP 160 DI 10.1007/s10509-007-9322-1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166BC UT WOS:000246351000021 ER PT J AU Tam, CR Kaspi, VM Gaensler, BM Gotthelf, EV AF Tam, Cindy R. Kaspi, Victoria M. Gaensler, Bryan M. Gotthelf, Eric V. TI Chandra monitoring of the candidate anomalous X-ray pulsar AX J1845.0-0258 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE pulsar; AXP; neutron star; magnetar; AX J1845.0-0258 ID SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; TRANSIENT MAGNETAR; XTE J1810-197; XTE-J1810-197; DISCOVERY; EMISSION AB The population of clearly identified anomalous X-ray pulsars has recently grown to seven, however, one candidate anomalous X-ray pulsar (AXP) still eludes reconfirmation. Here, we present a set of seven Chandra ACIS-S observations of the transient pulsar AX J1845.0-0258, obtained during 2003. Our observations reveal a faint X-ray point source within the ASCA error circle of AX J1845.0-0258's discovery, which we designate CXOU J184454.6-025653 and tentatively identify as the quiescent AXP. Its spectrum is well described by an absorbed single-component blackbody (kT similar to 2.0 keV) or power law (G similar to 1.0) that is steady in flux on timescales of at least months, but fainter than AX J1845.0-0258 was during its 1993 period of X-ray enhancement by at least a factor of 13. Compared to the outburst spectrum of AX J1845.0-0258, CXOU J184454.6-025653 is considerably harder: if truly the counterpart, then its spectral behavior is contrary to that seen in the established transient AXP XTE J1810-197, which softened from kT similar to 0.67 keV to similar to 0.18 keV in quiescence. This unexpected result prompts us to examine the possibility that we have observed an unrelated source, and we discuss the implications for AXPs, and magnetars in general. C1 McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Tam, CR (reprint author), McGill Univ, Dept Phys, 3600 Univ St,Rutherford Phys Bldg, Montreal, PQ H3A 2T8, Canada. EM tamc@physics.mcgill.ca RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 17 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD APR PY 2007 VL 308 IS 1-4 BP 519 EP 523 DI 10.1007/s10509-007-9295-0 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166BC UT WOS:000246351000068 ER PT J AU King, DI Hernandez-Mayorga, MD Trubey, R Raudales, R Rappole, JH AF King, David I. Hernandez-Mayorga, Martin D. Trubey, Richard Raudales, Raul Rappole, John H. TI An evaluation of the contribution of cultivated allspice (Pimenta dioca) to vertebrate biodiversity conservation in nicaragua SO BIODIVERSITY AND CONSERVATION LA English DT Article DE agroforestry; allspice; amphibians; birds; conservation; mammals; reptiles; tropics ID CACAO PLANTATIONS; COSTA-RICA; COFFEE PLANTATIONS; SOUTHERN VERACRUZ; BIRD POPULATIONS; AVIAN DIVERSITY; PLANTED SHADE; WOOD THRUSH; MEXICO; FOREST AB Tropical deforestation has emerged as one of the most important conservation challenges of our time, both because of the high species diversity and rates of endemism of tropical forests, and because of the rapid rate at which this process is proceeding. Recent studies indicate that areas of low-intensity agroforestry have similar levels of vertebrate diversity as some primary habitats, leading some researchers and conservationists to conclude that this type of commodity production could contribute to the conservation of biodiversity. We compared the composition of bird, mammal and herpetofaunal communities in primary forest, secondary forest, and pasture-and within the allspice productive systems that have replaced pasture. We found that mammal species richness was higher in primary forest than all other habitats; however for resident and migrant birds, amphibians and reptiles, species richness was similar between primary forest and the other habitats. Despite similarities in overall numbers of species, there were numerous species that were encountered only in primary habitats. We conclude that the cultivation of allspice in a mixed productive system can offset some of the losses to biodiversity; however it should be complemented by the establishment and maintenance of protected areas to accommodate populations of primary forest specialists that are unable to persist in altered habitats. C1 Univ Massachusetts, US Forest Serv, USDA, NE Res Stn, Amherst, MA 01003 USA. Cooperat CoopeSiuna, Ecologo, Martin Domingo Mayorga, Siuna, Nicaragua. Mesoamer Dev Inst, Lowell, MA 01851 USA. Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. RP King, DI (reprint author), Univ Massachusetts, US Forest Serv, USDA, NE Res Stn, Amherst, MA 01003 USA. EM dking@fs.fed.us NR 29 TC 5 Z9 6 U1 1 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD APR PY 2007 VL 16 IS 4 BP 1299 EP 1320 DI 10.1007/s10531-006-9068-z PG 22 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 162QJ UT WOS:000246103000031 ER PT J AU Collin, R Chaparro, OR Winkler, F Veliz, D AF Collin, Rachel Chaparro, Oscar R. Winkler, Federico Veliz, David TI Molecular phylogenetic and embryological evidence that feeding larvae have been reacquired in a marine gastropod SO BIOLOGICAL BULLETIN LA English DT Article ID CREPIDULA-DILATATA GASTROPODA; LIFE-HISTORY EVOLUTION; DEVELOPMENTAL MODE; TEMNOPLEURID ECHINOIDS; CALYPTRAEID GASTROPODS; NONFEEDING LARVAE; GEOGRAPHIC RANGE; SOUTHERN CHILE; SEA-URCHINS; INVERTEBRATES AB Evolutionary transitions between different modes of development in marine invertebrates are thought to be biased toward the loss of feeding larvae. Because the morphology of feeding larvae is complex and nonfeeding larvae or encapsulated embryos with benthic development often have simplified morphologies, it is presumed to be easier to lose a larval stage than to reacquire it. Some authors have gone so far as to suggest that feeding larvae, morphologically similar to the ancestral feeding larvae, cannot be reacquired. However, the larval structures of some groups, most notably gastropods, are often retained in the encapsulated embryos of species that hatch as benthic juveniles. Therefore the re-evolution of feeding larvae using the same structures may be possible in these groups. Here we present the first well - substantiated case for the recent re-evolution of feeding larvae within a clade of direct-developers. DNA sequence data show that Crepipatella fecunda, a species of calyptraeid gastropod with planktotrophic development, is nested within a clade of species with direct development, and that Crepipatella dilatata, a species with direct development, appears to be paraphyletic with respect to C. fecunda. Observation of the embryos of C. dilatata shows that the features necessary for larval feeding and swimming are retained in the encapsulated veligers, suggesting that heterochronic shifts in hatching time and changes in nurse-egg allotment could have resulted in the re-evolution of feeding larvae in this species. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Austral Chile, Inst Biol Marina Dr Jurgen Winter, Valdivia, Chile. Univ Catolica Norte, Dept Biol Marina, Coquimbo, Chile. Univ Chile, Fac Ciencias, Dept Ciencias Ecol, Santiago, Chile. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@si.edu RI Chaparro, Oscar/A-5070-2009; Collin, Rachel/G-2001-2010; Veliz, David/J-4205-2013; OI Collin, Rachel/0000-0001-5103-4460 NR 64 TC 49 Z9 49 U1 1 U2 14 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 EI 1939-8697 J9 BIOL BULL-US JI Biol. Bull. PD APR PY 2007 VL 212 IS 2 BP 83 EP 92 PG 10 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 160IH UT WOS:000245933600001 PM 17438201 ER PT J AU Herborg, LM Jerde, CL Lodge, DM Ruiz, GM MacIsaac, HJ AF Herborg, Leif-Matthias Jerde, Christopher L. Lodge, David M. Ruiz, Gregory M. MacIsaac, Hugh J. TI Predicting invasion risk using measures of introduction effort and environmental niche models SO ECOLOGICAL APPLICATIONS LA English DT Article DE ecological niche modeling; Eriocheir sinensis; genetic algorithm for rule set prediction (GARP); introduced range; invasive species; native range; relative risk; risk assessment ID CHINESE MITTEN CRAB; PROPAGULE PRESSURE; BIOLOGICAL INVASIONS; ERIOCHEIR-SINENSIS; NORTH-AMERICA; SPECIES INVASIONS; PLANT INVASIONS; BALLAST-WATER; INVASIBILITY; ECOLOGY AB The Chinese mitten crab (Eriocheir sinensis) is native to east Asia, is established throughout Europe, and is introduced but geographically restricted in North America. We developed and compared two separate environmental niche models using genetic algorithm for rule set prediction (GARP) and mitten crab occurrences in Asia and Europe to predict the species' potential distribution in North America. Since mitten crabs must reproduce in water with >= 15 parts per thousand salinity, we limited the potential North American range to freshwater habitats within the highest documented dispersal distance (1260 km) and a more restricted dispersal limit (354 km) from the sea. Applying the higher dispersal distance, both models predicted the lower Great Lakes, most of the eastern seaboard, the Gulf of Mexico and southern extent of the Mississippi River watershed, and the Pacific northwest as suitable environment for mitten crabs, but environmental match for southern states (below 35 degrees N) was much lower for the European model. Use of the lower range with both models reduced the expected range, especially in the Great Lakes, Mississippi drainage, and inland areas of the Pacific Northwest. To estimate the risk of introduction of mitten crabs, the amount of reported ballast water discharge into major United States ports from regions in Asia and Europe with established mitten crab populations was used as an index of introduction effort. Relative risk of invasion was estimated based on a combination of environmental match and volume of unexchanged ballast water received (July 1999 - December 2003) for major ports. The ports of Norfolk and Baltimore were most vulnerable to invasion and establishment, making Chesapeake Bay the most likely location to be invaded by mitten crabs in the United States. The next highest risk was predicted for Portland, Oregon. Interestingly, the port of Los Angeles/Long Beach, which has a large shipping volume, had a low risk of invasion. Ports such as Jacksonville, Florida, had a medium risk owing to small shipping volume but high environmental match. This study illustrates that the combination of environmental niche- and vector-based models can provide managers with more precise estimates of invasion risk than can either of these approaches alone. C1 Univ Windsor, Great Lakes Inst Environm Res, Windsor, ON N9B 3P4, Canada. Univ Notre Dame, Dept Biol Sci, Notre Dame, IN 46556 USA. Univ Alberta, Dept Biol Sci, Ctr Math Biol, Edmonton, AB T6G 2E9, Canada. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Herborg, LM (reprint author), Fisheries & Oceans Canada, Pacific Biol Stn, 3190 Hammond Bay, Nanaimo, BC V9T 6N7, Canada. EM HerborgL@pac.dfo-mpo.gc.ca RI Jerde, Christopher/K-5111-2012; OI Jerde, Christopher/0000-0003-4448-3561; Ruiz, Gregory/0000-0003-2499-441X NR 62 TC 84 Z9 89 U1 10 U2 72 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD APR PY 2007 VL 17 IS 3 BP 663 EP 674 DI 10.1890/06-0239 PG 12 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 157TS UT WOS:000245744500004 PM 17494387 ER PT J AU Morris, WF Hufbauer, RA Agrawal, AA Bever, JD Borowicz, VA Gilbert, GS Maron, JL Mitchell, CE Parker, IM Power, AG Torchin, ME Vazquez, DP AF Morris, William F. Hufbauer, Ruth A. Agrawal, Anurag A. Bever, James D. Borowicz, Victoria A. Gilbert, Gregory S. Maron, John L. Mitchell, Charles E. Parker, Ingrid M. Power, Alison G. Torchin, Mark E. Vazquez, Diego P. TI Direct and interactive effects of enemies and mutualists on plant performance: A meta-analysis SO ECOLOGY LA English DT Article DE factorial experiment; Hedges' d; herbivore; interaction effect; log response ratio; meta-analysis; mutualist; natural enemy; pathogen; plant performance ID STRESS-GRADIENT HYPOTHESIS; FIELD EXPERIMENTS; DIFFUSE COEVOLUTION; BIOLOGICAL-CONTROL; ARID ENVIRONMENTS; ABIOTIC STRESS; COMPETITION; HERBIVORY; POPULATION; COMMUNITY AB Plants engage in multiple, simultaneous interactions with other species; some ( enemies) reduce and others (mutualists) enhance plant performance. Moreover, effects of different species may not be independent of one another; for example, enemies may compete, reducing their negative impact on a plant. The magnitudes of positive and negative effects, as well as the frequency of interactive effects and whether they tend to enhance or depress plant performance, have never been comprehensively assessed across the many published studies on plant - enemy and plant - mutualist interactions. We performed a meta-analysis of experiments in which two enemies, two mutualists, or an enemy and a mutualist were manipulated factorially. Specifically, we performed a factorial meta-analysis using the log response ratio. We found that the magnitude of ( negative) enemy effects was greater than that of ( positive) mutualist effects in isolation, but in the presence of other species, the two effects were of comparable magnitude. Hence studies evaluating single-species effects of mutualists may underestimate the true effects found in natural settings, where multiple interactions are the norm and indirect effects are possible. Enemies did not on average influence the effects on plant performance of other enemies, nor did mutualists influence the effects of mutualists. However, these averages mask significant and large, but positive or negative, interactions in individual studies. In contrast, mutualists ameliorated the negative effects of enemies in a manner that benefited plants; this overall effect was driven by interactions between pathogens and belowground mutualists ( bacteria and mycorrhizal fungi). The high frequency of significant interactive effects suggests a widespread potential for diffuse rather than pairwise coevolutionary interactions between plants and their enemies and mutualists. Pollinators and mycorrhizal fungi enhanced plant performance more than did bacterial mutualists. In the greenhouse ( but not the field), pathogens reduced plant performance more than did herbivores, pathogens were more damaging to herbaceous than to woody plants, and herbivores were more damaging to crop than to non-crop plants ( suggesting evolutionary change in plants or herbivores following crop domestication). We discuss how observed differences in effect size might be confounded with methodological differences among studies. C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Colorado State Univ, Dept Bioagr Sci & Pest Management, Ft Collins, CO 80523 USA. Cornell Univ, Dept Ecol & Evolut Biol, Ithaca, NY 14853 USA. Indiana Univ, Dept Bot, Bloomington, IN 47405 USA. Illinois State Univ, Behav Ecol Evolut & Systemat Sect, Dept Biol Sci, Normal, IL 61790 USA. Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. Univ N Carolina, Curriculum Ecol, Chapel Hill, NC 27599 USA. Univ Calif Santa Cruz, Dept Ecol & Evolut Biol, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Panama. Ctr Reg Invest Cientificas & Tecnol, Inst Argentino Invest Zonas Aridas, RA-5500 Mendoza, Argentina. RP Morris, WF (reprint author), Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA. EM wfmorris@duke.edu RI Mitchell, Charles/I-3709-2014; OI Mitchell, Charles/0000-0002-1633-1993; Vazquez, Diego P./0000-0002-3449-5748 NR 34 TC 131 Z9 132 U1 6 U2 139 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 2007 VL 88 IS 4 BP 1021 EP 1029 DI 10.1890/06-0442 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 162QV UT WOS:000246104600021 PM 17536717 ER PT J AU Mittelbach, GG Schemske, DW Cornell, HV Allen, AP Brown, JM Bush, MB Harrison, SP Hurlbert, AH Knowlton, N Lessios, HA McCain, CM McCune, AR McDade, LA McPeek, MA Near, TJ Price, TD Ricklefs, RE Roy, K Sax, DF Schluter, D Sobel, JM Turelli, M AF Mittelbach, Gary G. Schemske, Douglas W. Cornell, Howard V. Allen, Andrew P. Brown, Jonathan M. Bush, Mark B. Harrison, Susan P. Hurlbert, Allen H. Knowlton, Nancy Lessios, Harilaos A. McCain, Christy M. McCune, Amy R. McDade, Lucinda A. McPeek, Mark A. Near, Thomas J. Price, Trevor D. Ricklefs, Robert E. Roy, Kaustuv Sax, Dov F. Schluter, Dolph Sobel, James M. Turelli, Michael TI Evolution and the latitudinal diversity gradient: speciation, extinction and biogeography SO ECOLOGY LETTERS LA English DT Review DE biodiversity; biotic interactions; diversification; evolutionary speed; extinction; geographical isolation; latitudinal diversity gradient; speciation; tropics ID RECENT BIVALVE FAUNAS; NEW-WORLD BIRDS; SPECIES RICHNESS; BODY-SIZE; SYMPATRIC SPECIATION; TAXONOMIC DIVERSITY; HYBRID INVIABILITY; MOLECULAR CLOCK; RAIN-FOREST; HISTORICAL BIOGEOGRAPHY AB A latitudinal gradient in biodiversity has existed since before the time of the dinosaurs, yet how and why this gradient arose remains unresolved. Here we review two major hypotheses for the origin of the latitudinal diversity gradient. The time and area hypothesis holds that tropical climates are older and historically larger, allowing more opportunity for diversification. This hypothesis is supported by observations that temperate taxa are often younger than, and nested within, tropical taxa, and that diversity is positively correlated with the age and area of geographical regions. The diversification rate hypothesis holds that tropical regions diversify faster due to higher rates of speciation (caused by increased opportunities for the evolution of reproductive isolation, or faster molecular evolution, or the increased importance of biotic interactions), or due to lower extinction rates. There is phylogenetic evidence for higher rates of diversification in tropical clades, and palaeontological data demonstrate higher rates of origination for tropical taxa, but mixed evidence for latitudinal differences in extinction rates. Studies of latitudinal variation in incipient speciation also suggest faster speciation in the tropics. Distinguishing the roles of history, speciation and extinction in the origin of the latitudinal gradient represents a major challenge to future research. C1 Michigan State Univ, Kellogg Biol Stn, Hickory Corners, MI 49060 USA. Michigan State Univ, Dept Zool, Hickory Corners, MI 49060 USA. Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. Grinnell Coll, Dept Biol, Grinnell, IA 50112 USA. Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biovers & Conservat, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. Cornell Univ, Dept Ecol & Evolut Biol, Ithaca, NY 14853 USA. Acad Nat Sci Philadelphia, Dept Bot, Philadelphia, PA 19103 USA. Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. Yale Univ, Dept Ecol & Evolut Biol, New Haven, CT 06520 USA. Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Univ Calif San Diego, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA. Univ Georgia, Inst Ecol, Athens, GA 30602 USA. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Univ Calif Davis, Sect Evolut & Ecol, Davis, CA 95616 USA. RP Mittelbach, GG (reprint author), Michigan State Univ, Kellogg Biol Stn, Hickory Corners, MI 49060 USA. EM mittelbach@kbs.msu.edu RI Allen, Andrew/B-8045-2011; Mittelbach, Gary/A-2470-2013; OI Allen, Andrew/0000-0003-0304-7544; Bush, Mark/0000-0001-6894-8613; Hurlbert, Allen/0000-0002-5678-9907 NR 156 TC 566 Z9 593 U1 52 U2 554 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD APR PY 2007 VL 10 IS 4 BP 315 EP 331 DI 10.1111/j.1461-0248.2007.01020.x PG 17 WC Ecology SC Environmental Sciences & Ecology GA 145SB UT WOS:000244883700007 PM 17355570 ER PT J AU Feller, IC Lovelock, CE Mckee, KL AF Feller, Ilka C. Lovelock, Catherine E. Mckee, Karen L. TI Nutrient addition differentially affects ecological processes of Avicennia germinans in nitrogen versus phosphorus limited mangrove ecosystems SO ECOSYSTEMS LA English DT Article DE Avicennia germinans; Belize; fertilization experiment; growth; herbivory; Indian River Lagoon; loss of yield; nutrient resorption; biomass allocation; nutrient over-enrichment ID INDIAN RIVER LAGOON; N-P RATIOS; RHIZOPHORA-MANGLE; FOREST STRUCTURE; GROWTH; LIMITATION; FLORIDA; PLANTS; ENRICHMENT; HERBIVORY AB Nutrient over-enrichment is a major threat to marine environments, but system-specific attributes of coastal ecosystems may result in differences in their sensitivity and susceptibility to eutrophication. We used fertilization experiments in nitrogen (N)- and phosphorus (P)-limited mangrove forests to test the hypothesis that alleviating different kinds of nutrient limitation may have different effects on ecosystem structure and function in natural systems. We compared a broad range of ecological processes to determine if these systems have different thresholds where shifts might occur in nutrient limitation. Growth responses indicated N limitation in Avicennia germinans (black mangrove) forests in the Indian River Lagoon (IRL), Florida, and P limitation at Twin Cays, Belize. When nutrient deficiency was relieved, A. germinans grew out of its stunted form by increasing wood relative to leaf biomass and shoot length relative to lateral growth. At the P-limited site, P enrichment (+P) increased specific leaf area, N resorption, and P uptake, but had no effect on P resorption. At the N-limited site, +N increased both N and P resorption, but did not alter biomass allocation. Herbivory was greater at the P-limited site and was unaffected by +P, whereas +N led to increased herbivory at the N-limited site. The responses to nutrient enrichment depended on the ecological process and limiting nutrient and suggested that N- versus P-limited mangroves do have different thresholds. +P had a greater effect on more ecological processes at Twin Cays than did +N at the IRL, which indicated that the P-limited site was more sensitive to nutrient loading. Because of this sensitivity, eutrophication is more likely to cause a shift in nutrient limitation at P-limited Twin Cays than N-limited IRL. C1 Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. RP Feller, IC (reprint author), Smithsonian Environm Res Ctr, Smithsonian Inst, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM felleri@si.edu RI McKee, Karen/D-1365-2014; Lovelock, Catherine/G-7370-2012; OI McKee, Karen/0000-0001-7042-670X; Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 NR 51 TC 46 Z9 52 U1 4 U2 65 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 1432-9840 J9 ECOSYSTEMS JI Ecosystems PD APR PY 2007 VL 10 IS 3 BP 347 EP 359 DI 10.1007/s10021-007-9025-z PG 13 WC Ecology SC Environmental Sciences & Ecology GA 202NX UT WOS:000248911400001 ER PT J AU Miller, CL Mason, RP Gilmour, CC Heyes, A AF Miller, Carrie L. Mason, Robert P. Gilmour, Cynthia C. Heyes, Andrew TI Influence of dissolved organic matter on the complexation of mercury under sulfidic conditions SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Article DE mercury; sulfide; dissolved organic matter; complexation ID DESULFOBULBUS-PROPIONICUS 1PR3; SEDIMENT PORE WATERS; FLORIDA EVERGLADES; NATURAL-WATERS; METHYLATING BACTERIA; PURE CULTURES; TRACE-METALS; METHYLMERCURY; PHASE; BIOAVAILABILITY AB The complexation of Hg under sulfidic conditions influences its bioavailability for microbial methylation. Neutral dissolved Hg-sulfide complexes are readily available to Hg-methylating bacteria in culture, and thermodynamic models predict that inorganic Hg-sulfide complexes dominate dissolved Hg speciation under natural sulfidic conditions. However, these models have not been validated in the field. To examine the complexation of Hg in natural sulfidic waters, octanol/water partitioning methods were modified for use under environmentally relevant conditions, and a centrifuge ultrafiltration technique was developed. These techniques demonstrated much lower concentrations of dissolved Hg-sulfide complexes than predicted. Furthermore, the study revealed an interaction between Hg, dissolved organic matter (DOM), and sulfide that is not captured by current thermodynamic models. Whereas Hg forms strong complexes with DOM under oxic conditions, these complexes had not been expected to form in the presence of sulfide because of the stronger affinity of Hg for sulfide relative to its affinity for DOM. The observed interaction between Hg and DOM in the presence of sulfide likely involves the formation of a DOM-Hg-sulfide complex or results from the hydrophobic partitioning of neutral Hg-sulfide complexes into the higher-molecular-weight DOM. An understanding of the mechanism of this interaction and determination of complexation coefficients for the Hg-sulfide-DOM complex are needed to adequately assess how our new finding affects Hg bioavailability, sorption, and flux. C1 Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Miller, CL (reprint author), Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, 1 William St, Solomons, MD 20688 USA. EM millerc@uncw.edu RI Miller, Carrie/B-8943-2012; Heyes, Andrew/E-5269-2012; Mason, Robert/A-6829-2011; Gilmour, Cynthia/G-1784-2010 OI Gilmour, Cynthia/0000-0002-1720-9498 NR 39 TC 56 Z9 58 U1 6 U2 31 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0730-7268 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD APR PY 2007 VL 26 IS 4 BP 624 EP 633 DI 10.1897/06-375R.1 PG 10 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA 146MJ UT WOS:000244938200007 PM 17447546 ER PT J AU Belanus, BJ AF Belanus, Betty J. TI The lore of the land: A guide to England's legends, from Spring-Heeled Jack to the Witches of Warboys. SO FOLKLORE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Belanus, BJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0015-587X J9 FOLKLORE JI Folklore PD APR PY 2007 VL 118 IS 1 BP 112 EP 112 PG 1 WC Folklore SC Arts & Humanities - Other Topics GA 148WS UT WOS:000245108700011 ER PT J AU Belanus, B AF Belanus, Betty TI The 'rich life and the dance': Weavings from Roman, Byzantine and Islamic Egypt. SO FOLKLORE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Belanus, B (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0015-587X J9 FOLKLORE JI Folklore PD APR PY 2007 VL 118 IS 1 BP 116 EP 117 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA 148WS UT WOS:000245108700015 ER PT J AU Brown, JL Somerville, M Riddle, HS Keele, M Duer, CK Freeman, EW AF Brown, Janine L. Somerville, Malia Riddle, Heidi S. Keele, Mike Duer, Connie K. Freeman, Elizabeth W. TI Comparative endocrinology of testicular, adrenal and thyroid function in captive Asian and African elephant bulls SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Asian elephant; African elephant; hormones; musth; bulls; testosterone; cortisol; TSH; thyroid hormones ID DEER CERVUS-ELAPHUS; LOXODONTA-AFRICANA; AGGRESSIVE-BEHAVIOR; TESTOSTERONE LEVELS; SOCIAL-DOMINANCE; SEASONAL-CHANGES; GROWTH-HORMONE; MUSTH; BOAR; CORTICOSTEROIDS AB Concentrations of serum testosterone, cortisol, thyroxine (free and total T4), triiodothyronine (free and total T3) and thyroid stimulating hormone (TSH) were measured to assess adrenal and thyroid function as they relate to testicular activity and musth in captive elephants. Blood samples were collected approximately weekly from Asian (n = 8) and African (n = 12) bulls at seven facilities for periods of 4 months to 9.5 years. Age ranges at study onset were 8-50 years for Asian and 10-21 years for African elephants. Based on keeper logs, seven Asian and three African bulls exhibited behavioral and/or physical (temporal gland secretion, TGS, or urine dribbling, UD) signs of musth, which lasted 2.8 +/- 2.5 months in duration. Serum testosterone was elevated during musth, with concentrations often exceeding 100 ng/ml. Patterns of testosterone secretion and musth varied among bulls with no evidence of seasonality (P > 0.05). Only three bulls at one facility exhibited classic, well-defined yearly musth cycles. Others exhibited more irregular cycles, with musth symptoms often occurring more than once a year. A number of bulls (I Asian, 9 African) had consistently low testosterone (< 10 ng/ml) and never exhibited significant TGS or UD. At facilities with multiple bulls (n = 3), testosterone concentrations were highest in the oldest, most dominant male. There were positive correlations between testosterone and cortisol for six of seven Asian and all three African males that exhibited musth (range, r = 0.23-0.52; P < 0.05), but no significant correlations for bulls that did not (P > 0.05). For the three bulls that exhibited yearly musth cycles, TSH was positively correlated (range, r = 0.22-0.28; P < 0.05) and thyroid hormones (T3, T4) were negatively correlated (range, r = -0.25 to -0.47; P < 0.05) to testosterone secretion. In the remaining bulls, there were no clear relationships between thyroid activity and musth status. Overall mean testosterone and cortisol concentrations increased with age for all bulls combined, whereas thyroid activity declined. In summary, a number of bulls did not exhibit musth despite being of adequate physical maturity. Cortisol and testosterone were correlated in most bulls exhibiting musth, indicating a possible role for the adrenal gland in modulating or facilitating downstream responses. Data were generally inconclusive as to a role for thyroid hormones in male reproduction, but the finding of discrete patterns in bulls showing clear testosterone cycles suggests they may facilitate expression or control of musth in some individuals. (c) 2007 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Dept Reprod Sci, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. American Univ, Dept Biol, Washington, DC 20016 USA. Oregon Zoo, Portland, OR USA. Oklahoma State Univ, Dept Zool, Stillwater, OK 74078 USA. RP Brown, JL (reprint author), Smithsonian Inst, Dept Reprod Sci, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM brownjan@si.edu NR 37 TC 20 Z9 21 U1 4 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD APR PY 2007 VL 151 IS 2 BP 153 EP 162 DI 10.1016/j.ygcen.2007.01.006 PG 10 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 151JB UT WOS:000245285200002 PM 17336304 ER PT J AU Haggis, DC Mook, MS Fitzsimons, RD Scarry, CM Snyder, LM AF Haggis, Donald C. Mook, Margaret S. Fitzsimons, Rodney D. Scarry, C. Margaret Snyder, Lynn M. TI Excavations at Azoria, 2003-2004, Part 1 - The archaic civic complex SO HESPERIA LA English DT Review ID CRETE; KAVOUSI; LAWS AB This article constitutes the first of two reports on fieldwork conducted at Azoria in eastern Crete during the 2003 and 2004 excavation seasons. The focus of excavation was on the South Acropolis, where buildings of Archaic date (7th-early 5th century B.C.) suggesting public or civic functions have come to light. The complex includes a possible andreion on the west slope, a cult building on the terrace south of the peak, and storerooms and kitchens associated with a monumental public building on the southwest terrace. A 3rd-century B.C. dump on the southeast slope provides important information about the limited reoccupation of the site in the Hellenistic period. C1 Univ N Carolina, Dept Class, Chapel Hill, NC 27599 USA. Iowa State Univ Sci & Technol, Class Studies Program, Ames, IA 50011 USA. Trent Univ, Dept Ancient Hist & Class, Peterborough, ON K9J 7B8, Canada. Univ N Carolina, Dept Anthropol, Chapel Hill, NC 27599 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Haggis, DC (reprint author), Univ N Carolina, Dept Class, 212 Murphey Hall,CB 3145, Chapel Hill, NC 27599 USA. EM dchaggis@email.unc.edu; msmook@iastate.edu; rodneyfitzsimons@trentu.ca; scarry@email.unc.edu; snyderl@si.edu NR 199 TC 17 Z9 17 U1 0 U2 0 PU AMER SCHOOL CLASSICAL STUDIES AT ATHENS PI PRINCETON PA 6-8 CHARLTON STREET, PRINCETON, NJ 08540-5232 USA SN 0018-098X J9 HESPERIA JI Hesperia PD APR-JUN PY 2007 VL 76 IS 2 BP 243 EP 321 DI 10.2972/hesp.76.2.243 PG 79 WC Archaeology SC Archaeology GA 213BF UT WOS:000249640200001 ER PT J AU Cleere, N Kratter, AW Steadman, DW Braun, MJ Huddleston, CJ Filardi, CE Dutson, G AF Cleere, Nigel Kratter, Andrew W. Steadman, David W. Braun, Michael J. Huddleston, Christopher J. Filardi, Christopher E. Dutson, Guy TI A new genus of frogmouth (Podargidae) from the Solomon Islands - results from a taxonomic review of Podargus ocellatus inexpectatus Hartert 1901 SO IBIS LA English DT Article ID HIGHER LAND BIRDS; CAPRIMULGIFORM BIRDS; MIDDLE EOCENE; MESSEL HESSEN; SEQUENCES; NIGHTJARS; GERMANY; ISABEL; ALLIES AB The frogmouth taxon occurring on the Solomon Islands has been known as Podargus ocellatus inexpectatus, a subspecies endemic to four islands in the Solomon Islands of a species that also inhabits New Guinea and Australia. Our morphological, osteological and molecular studies support recognition of inexpectatus at the species level, and further reveal that it merits placement in its own genus, which we describe here. Compared with the two other extant podargid genera, inexpectatus does not seem to be more closely related either to Batrachostomus (confined to the Indo-Malayan faunal region) or to Podargus of the Papuan-Australian faunal region. We also review the specimen history of the Solomon Islands Frogmouth, and discuss what little is known about its ecology, natural history and distribution. C1 Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. Nat Hist Museum, Dept Zool, Bird Grp, Tring HP23 6AP, England. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Suitland, MD 20746 USA. Univ Washington, Burke Museum, Seattle, WA 98195 USA. RP Kratter, AW (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM kratter@flmnh.ufl.edu NR 58 TC 7 Z9 9 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0019-1019 J9 IBIS JI Ibis PD APR PY 2007 VL 149 IS 2 BP 271 EP 286 DI 10.1111/j.1474-919X.2006.00626.x PG 16 WC Ornithology SC Zoology GA 151SV UT WOS:000245312000009 ER PT J AU Kuris, AM Goddard, JHR Torchin, ME Murphy, N Gurney, R Lafferty, KD AF Kuris, Armand M. Goddard, Jeffrey H. R. Torchin, Mark E. Murphy, Nicole Gurney, Robert Lafferty, Kevin D. TI An experimental evaluation of host specificity: The role of encounter and compatibility filters for a rhizocephalan parasite of crabs SO INTERNATIONAL JOURNAL FOR PARASITOLOGY LA English DT Article DE Carcinus maenas; host-parasite evolution; host specificity; host response; Pachygrapsus marmoratus; rhizocephala ID BIOLOGICAL-CONTROL; SACCULINA-CARCINI; ENCAPSULATION; CIRRIPEDIA; CASTRATOR; BRACHYURA; MAENAS AB The encounter/compatibility paradigm of host specificity provides three qualitative pathways to the success or failure of a potential host-parasite interaction. It is usually impossible to distinguish between two of these (encounter and compatibility filters closed versus encounter filter open and compatibility filter closed) because unsuccessful infection attempts are difficult to observe in nature. We were able to open the encounter filter under experimental laboratory conditions. Our analytical system used the rhizocephalan barnacle, Sacculina carcini, a parasitic castrator of the European green crab, Carcinus maenas, and Pachygrapsus marmoratus, a native European crab that occurs with C. mamas but is not parasitized by S. carcini in nature. Penetration followed by unsuccessful infection of P. marmoratus crabs by parasitic barnacle larvae leaves a uniquely permanent record in the thoracic ganglion of the crabs. This provided us with a novel tool to quantify the encounter filter in a host-parasite system in nature. We demonstrated, in the laboratory, that the compatibility filter was closed and that, in nature, even where barnacle larvae were present, the encounter filter was also effectively closed. The closure of both filters in nature explains the failure of this potential host-parasite interaction, an outcome favored by selection in both host and parasite. (c) 2006 Australian Society for Parasitology Inc. Published by Elsevier Ltd. All rights reserved. C1 Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Marine Sci Inst, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Balboa, Panama. CSIRO Marine Res, Ctr Res Introduced Marine Pests, Hobart, Tas 7001, Australia. Univ Calif Santa Barbara, Marine Sci Inst, Western Ecol Res Ctr, Santa Barbara, CA 93106 USA. RP Kuris, AM (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM kuris@lifesci.ucsb.edu RI Lafferty, Kevin/B-3888-2009 OI Lafferty, Kevin/0000-0001-7583-4593 NR 22 TC 26 Z9 27 U1 9 U2 32 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 APR PY 2007 VL 37 IS 5 BP 539 EP 545 DI 10.1016/j.ijpara.2006.12.003 PG 7 WC Parasitology SC Parasitology GA 158ET UT WOS:000245774800009 PM 17275825 ER PT J AU Georgescu, MD Huber, BT AF Georgescu, Marius D. Huber, Brian T. TI Taxonomic revision of the Late Campanian-Maastrichtian (late Cretaceous) planktonic foraminiferal genus Rugotruncana Bronnimann and Brown, 1956, and a new paleontological species concept for planktonic foraminifera SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article; Proceedings Paper CT 3rd Fribourg Obesity Research Conference (FORC-2005) CY SEP 30, 2005 CL Fribourg, SWITZERLAND ID BIOZONATION AB The Late Cretaceous (late Campanian-Maastrichtian) planktonic foraminiferal genus Rugotruncana Bronnimann and Brown, 1956 is thoroughly revised. The genus is monospecific, with Rugotruncana circumnodifer (Finlay, 1940) being the only species included within it. Taxonomic revision of the genus was made by examination of type specimens of all species assigned to Rugotruncana in the past. The genus is characterized by the presence of an imperforate band and a weakly to strongly developed double keel along the test periphery. In addition, detailed scanning electron microscope observations reveal that the test ornamentation is asymmetrical, with variably developed rugae and costellae being parallel to the periphery on the spiral side and meridional on the umbilical side. These features serve to distinguish Rugotruncana from Rugoglobigerina and Globotruncana. Based on the morphological features revealed by the detailed test ultrastructure and ornamentation observations, Rugotruncana is included within Family Rugoglobigerinidae. A new paleontological species concept is proposed to accommodate Rugotruncana circumnodifer and other species of Cretaceous planktonic foraminifera. C1 Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Georgescu, MD (reprint author), Univ Saskatchewan, Dept Geol Sci, 114 Pl, Saskatoon, SK S7N 5E2, Canada. EM mdg335@mail.usask.ca NR 34 TC 10 Z9 12 U1 1 U2 3 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD APR PY 2007 VL 37 IS 2 BP 150 EP 159 DI 10.2113/gsjfr.37.2.150 PG 10 WC Paleontology SC Paleontology GA 157EA UT WOS:000245700200005 ER PT J AU Ando, A Huber, BT AF Ando, Atsushi Huber, Brian T. TI Taxonomic revision of the late Cenomanian planktonic foraminifera Rotalipora greenhornensis (Morrow, 1934) SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID STRATOTYPE SECTION; MONT-RISOU; BIOSTRATIGRAPHY; BOUNDARY; FRANCE; POINT; BASIN AB Rotalipora greenhornensis has long been considered a representative planktonic foraminiferal species of the single-keeled Rotaliporinae of late Cenomanian age. Its taxonomic identity, however, is still ambiguous because this taxon has been distinguished by morphological criteria (numerous, strongly curved chambers, etc.), whereas the other species of Rotalipora are distinguished primarily by their apertural and ornamental characters (raised sutures, periumbilical ridges, etc.). The presence of strongly raised sutures throughout the umbilical and spiral sides has also been used to identify R. greenhornensis, but this criterion is troublesome as it also applies to its direct ancestor Rotalipora globotruncanoides. Reexamination of the holotype and observation of many topotypes and some North Atlantic and Pacific hypotypes reveals that, despite its remarkable morphological variability, R. greenhornensis is distinguishable by having umbilical sutures that are not fully raised, with the last several being depressed, and supplementary apertures that are umbilical in position and surrounded by a continuous series of closely-spaced periumbilical ridges. Moreover, reduction of the raised sutures tends to occur simultaneously on both the umbilical and spiral sides. Such apertural and ornamental characters of R. greenhornensis serve as its primary distinguishing features, allowing a clear-cut differentiation of this taxon from other species of Rotalipora, particularly the closely associated species R. globotruncanoides and piano-convex Rotalipora deeckei. C1 Res Inst Human & Nat, Kyoto 6038047, Japan. Chiba Univ, Fac Sci, Dept Earth Sci, Chiba, Japan. Smithsonian Natl Museum Nat Hist, Dept Paleobiol, MRC NHB 121, Washington, DC 20013 USA. RP Ando, A (reprint author), Res Inst Human & Nat, Motoyama 457-4, Kyoto 6038047, Japan. EM ando@chikyu.ac.jp NR 55 TC 14 Z9 14 U1 0 U2 1 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD APR PY 2007 VL 37 IS 2 BP 160 EP 174 DI 10.2113/gsjfr.37.2.160 PG 15 WC Paleontology SC Paleontology GA 157EA UT WOS:000245700200006 ER PT J AU Wang, W Potts, R Baoyin, Y Huang, WW Cheng, H Edwards, RL Ditchfield, P AF Wang, Wei Potts, Richard Baoyin, Yuan Huang, Weiwen Cheng, Hai Edwards, R. Lawrence Ditchfield, Peter TI Sequence of mammalian fossils, including hominoid teeth, from the Bubing Basin caves, South China SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Bose; fauna; Gigantopithecus; Mohui; stable isotopes; Stegodon/Ailuropoda fauna; U-series dating ID ENAMEL; DIETARY; URANIUM; CARBON; ORIGIN; KENYA; TIME AB A Plio-Pleistocene to Holocene faunal sequence has been recovered from four carefully excavated caves in the Bubing Basin, adjacent to the larger Bose Basin of South China. The caves vary in elevation; we suggest that the higher caves were formed and filled with sediments prior to the lower caves. The highest deposits, which are from Mohui Cave, contain hominoid teeth and other fossilized remains of mammalian taxa most similar to late Pliocene and early Pleistocene faunas. Wuyun Cave (similar to 50 in lower in elevation than Mohui) contains a late middle Pleistocene fauna, which is supported by U-series age constraints from 350 to 200 ka. Lower Pubu Cave (similar to 23 in below Wuyun) is assigned to the late Pleistocene, while the Cunkong Cave (the lowest, similar to 2m in lower elevation than Lower Pubu) preserves a Holocene fauna. The four faunal assemblages indicate species-level changes in Ailuropoda, Stegodon, and Sus, the appearance of Elephas, the local disappearance of Stegodon, and the migration of Equus hemionus to South China. These initial results of our work call into question the continued value of the Stegodon/Ailuropoda Fauna, a category long used to characterize the Pleistocene faunas of South China. Excavation of karstic caves of varying elevation within the basins of South China holds promise for defining local sequences of mammalian fossils that can be used to investigate faunal variations related to climate change, biogeographic events, and evolutionary change over the past two million years. Stable isotopic analysis of a small sample of mammalian teeth from Bubing Basin caves is consistent with 100% C-3 vegetation in the Bubing/Bose region, with certain delta C-13 values consistent with a canopied woodland or forest. A preliminary assessment of the hominoid teeth indicates the presence of diverse molar and premolar morphologies including dental remains of Gigantopithecus blacki and a sample with similarities to the teeth reported from Longgupo. (c) 2006 Elsevier Ltd. All rights reserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. China Univ Geosci, Fac Earth Sci, Wuhan 430074, Peoples R China. Nat Hist Museum Guangxi Zhuang Autonomous Reg, Nanning, Peoples R China. Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. Chinese Acad Sci, Inst Vertebrate Paleontol & Paleoanthropol, Beijing 100044, Peoples R China. Univ Minnesota, Dept Geol & Geophys, Minneapolis, MN 55455 USA. Univ Oxford, Archaeol & Hist Art Res Lab, Oxford OX1 3QY, England. RP Potts, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. EM wangwei@public.nn.gx.cn; pottsr@si.edu; huangweiwen@pa.ivpp.ac.cn; cheng021@umn.edu; Edwar001@tc.umn.edu; peter.ditchfield@archaeology-research.oxford.ac.uk NR 34 TC 50 Z9 60 U1 0 U2 12 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD APR PY 2007 VL 52 IS 4 BP 370 EP 379 DI 10.1016/j.jhevol.2006.10.003 PG 10 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 162NN UT WOS:000246094700002 PM 17198721 ER PT J AU Helgen, KM Kock, D Gomez, RKSC Ingle, NR Sinaga, MH AF Helgen, Kristofer M. Kock, Dieter Gomez, Rai Kristie Salve C. Ingle, Nina R. Sinaga, Martua H. TI Taxonomy and natural history of the southeast Asian fruit-bat genus Dyacopterus SO JOURNAL OF MAMMALOGY LA English DT Article DE biogeography; Dyacopterus; Indonesia; Malaysia; morphology; new species; Philippines; Pteropodidae; taxonomy; Thailand ID DIPTEROCARP RAIN-FOREST; VERTICAL STRATIFICATION; MOLECULAR PHYLOGENY; EAST ASIA; PTEROPODIDAE; CHIROPTERA; MEGACHIROPTERA; SINGAPORE; PHILIPPINES; MORPHOLOGY AB The pteropodid genus Dyacopterus Andersen, 1912, comprises several medium-sized fruit-bat species endemic to forested areas of Sundaland and the Philippines. Specimens of Dyacopterus are sparsely represented in collections of world museums, which has hindered resolution of species limits within the genus. Based on our studies of most available museum material, we review the infrageneric taxonomy of Dyacopterus using craniometric and other comparisons. In the past, 2 species have been described - D. spadiceus (Thomas, 1890), described from Borneo and later recorded from the Malay Peninsula, and D. brooksi Thomas, 1920, described from Sumatra. These 2 nominal taxa are often recognized as species or conspecific subspecies representing these respective populations. Our examinations instead suggest that both previously described species of Dyacopterus co-occur on the Sunda Shelf - the smaller-skulled D. spadiceus in peninsular Malaysia, Sumatra, and Borneo, and the larger-skulled D. brooksi in Sumatra and Borneo. We further identify specimens of Dyacopterus from the large islands of Luzon and Mindanao in the Philippines as representatives of a distinctive new species, Dyacopterus rickarti. This new species differs from the Sundaic taxa in its much larger size, unique palatal ridge formula, and in qualitative craniodental features. The natural history of each species, so far as it is known, is briefly reviewed. C1 Smithsonian Inst, Natl Museum Amer Hist, Div Mammals, Washington, DC 20013 USA. Forschungsinst Senckenberg, D-60325 Frankfurt, Germany. Philippine Eagle Fdn, Davao 8000, Philippines. Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. Field Museum Nat Hist, Div Mammals, Chicago, IL 60605 USA. Museum Zoologicum Bogoriense, Cibinong 16911, Indonesia. RP Helgen, KM (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Mammals, NHB 390,MRC 108,POB 37012, Washington, DC 20013 USA. EM helgen@post.harvard.edu NR 85 TC 8 Z9 10 U1 4 U2 19 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 APR PY 2007 VL 88 IS 2 BP 302 EP 318 DI 10.1644/06-MAMM-A-276R.1 PG 17 WC Zoology SC Zoology GA 165DM UT WOS:000246284100003 ER PT J AU Grier, HJ Uribe, MC Parenti, LR AF Grier, Harry J. Uribe, Mari Carmen Parenti, Lynne R. TI Germinal epithelium, folliculogenesis, and postovulatory follicles in ovaries of rainbow trout, Oncorhynchus mykiss (Walbaum, 1792) (Teleostei, Protacanthopterygii, Salmoniformes) SO JOURNAL OF MORPHOLOGY LA English DT Article DE rainbow trout; Oncorhynchus mykiss; germinal epithelium; folliculogenesis; follicle; oocyte; ovary ID SALMO-GAIRDNERI RICHARDSON; OOCYTE GROWTH; REPRODUCTIVE-CYCLE; SEX-DIFFERENTIATION; SYNGNATHUS-SCOVELLI; STRIPED MULLET; COMMON SNOOK; OOGENESIS; VITELLOGENIN; CELLS AB The rainbow trout, Oncorhynchus mykiss (Walbaum, 1792), is a salmoniform fish that spawns once per year. Ripe females that had ovulated naturally, and those induced to ovulate using salmon gonadotropin-releasing hormone, were studied to determine whether follicles were forming at the time of spawning and to describe the process of folliculogenesis. After ovulation, the ovaries of postspawned rainbow trout were examined histologically, using the periodic acid-Schiff procedure, to stain basement membranes that subtend the germinal epithelium and to interpret and define the activity of the germinal epithelium. After spawning, the ovary contained a few ripe oocytes that did not ovulate, numerous primary growth oocytes including oocytes with cortical alveoli, and postavulatory follicles. The germinal epithelium was active in postspawned rainbow trout, as determined by the presence of numerous cell nests, composed of oogonia, mitotic oogonia, early diplotene oocytes, and prefollicle cells. Cell nests were separated from the stroma by a basement membrane continuous with that subtending the germinal epithelium. Furthermore, follicles containing primary growth oocytes were connected to the germinal epithelium; the basement membrane surrounding the follicle joined that of the germinal epithelium. After ovulation, the basement membrane of the postovulatory follicle was continuous with that of the germinal epithelium. We observed consistent separation of the follicle, composed of. an oocyte and surrounding follicle cells, from the ovarian stroma by a basement membrane. The follicle is derived from the germinal epithelium. As with the germinal epithelium, follicle cells derived from it never contact those of the connective tissue stroma. As with epithelia, they are always separated from connective tissue by a basement membrane. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. Univ Nacl Autonoma Mexico, Fac Ciencias, Lab biol Reprod Anim, Mexico City 04510, DF, Mexico. RP Grier, HJ (reprint author), Florida Fish & Wildlife Res Inst, 100 8th Ave SE, St Petersburg, FL 33701 USA. EM harry.grier@myfwc.com NR 86 TC 37 Z9 39 U1 1 U2 8 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD APR PY 2007 VL 268 IS 4 BP 293 EP 310 DI 10.1002/jmor.10518 PG 18 WC Anatomy & Morphology SC Anatomy & Morphology GA 154EE UT WOS:000245488800003 PM 17309079 ER PT J AU Medina, B Guzman, HM Mair, JM AF Medina, Beatriz Guzman, Hector M. Mair, James M. TI Failed recovery of a collapsed scallop (Argopecten ventricosus) fishery in Las Perlas Archipelago, Panama SO JOURNAL OF SHELLFISH RESEARCH LA English DT Article DE overfishing; scallop; Argopecten; Panama; fishery collapse ID PURPURATUS LAMARCK; NORTHERN CHILE; SOWERBY II; BAY; TEMPERATURE; PREDATORS; IRRADIANS; REFUGE; EVENT/ AB The scallop Argopecten ventricosus (Sowerby II 1842) supported an important fishery in the Gulf of Panama (Pacific Panama) during 1981-1990, but the fishery essentially collapsed in 1991. To determine if the A. ventricosus population in one major fishing ground, Las Perlas Archipelago, has recovered almost 15 years after that collapse, we interviewed fishermen, reviewed historical data about scallop export markets and fishing grounds, and assessed the state of the scallop population using traditional local trawling methods. During four expeditions (2000-2004), we intensively surveyed 183 trawling stations, which included the major shallow fishery sites as well as other deeper areas within the archipelago. We collected hundreds of relic adult and juvenile scallop shells, but we retrieved only 30 live individuals. This suggests that minimal recruitment has occurred in the archipelago and that the fishery remains collapsed. We argue that this population's failure to recover may be because of a lack of suitable available habitats for juveniles, predation and variation in local oceanographic conditions, as previously suggested. Further studies are needed to fully determine why the scallop population has failed to recover. Application of mariculture techniques may be required to restore the stock and repopulate A. ventricosus natural banks in Las Perlas Archipelago. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Heriot Watt Univ, Ctr Marine Biodivers & Biotechnol, Sch Life Sci, Edinburgh EH14 4AS, Midlothian, Scotland. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM guzmanh@si.edu NR 30 TC 6 Z9 6 U1 0 U2 6 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD APR PY 2007 VL 26 IS 1 BP 9 EP 15 DI 10.2983/0730-8000(2007)26[9:FROACS]2.0.CO;2 PG 7 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 164SX UT WOS:000246255800002 ER PT J AU Comita, LS Aguilar, S Perez, R Lao, S Hubbell, SP AF Comita, Liza S. Aguilar, Salomon Perez, Rolando Lao, Suzanne Hubbell, Stephen P. TI Patterns of woody plant species abundance and diversity in the seedling layer of a tropical forest SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE advanced regeneration; Barro Colorado island; forest dynamics plot; life history strategy; recruitment limitation; seedling bank; shade tolerance ID NEOTROPICAL FOREST; RECRUITMENT LIMITATION; TREE DIVERSITY; DEPENDENT RECRUITMENT; SPATIAL-PATTERNS; PIONEER TREES; RAIN-FOREST; DISPERSAL; GAPS; CONSEQUENCES AB Questions: 1. How does the composition and diversity of established seedlings compare to that of larger size classes in tropical forests? 2. How do species abundances in the seedling layer vary with adult abundance and life history strategies'? Location: Barro Colorado Island (BCI), Panama. Methods: We inventoried woody seedlings 2:20 cm tall and < 1 cm DBH in ca. 20 000 1-m(2) quadrats within the BCI 50-ha Forest Dynamics Plot, where all trees and shrubs > 1 cm DBH have been identified. We compared diversity and composition of seedlings to that of larger size classes and tested whether adult abundance, growth form, and shade tolerance contributed to variation in seedling abundance among species. Results: We encountered 60056 seedlings of 332 tree, shrub, and liana species. Diversity of tree seedlings was lower than that of trees 2: 1 cm DBH. Species abundances in the seedling layer increased non-linearly with reproductive adult abundance, such that per capita seedling abundance declined with adult abundance. Per capita seedling abundance was highest for canopy tree species and lowest for understorey trees. For canopy trees, shade-tolerant species had significantly higher per capita seedling abundance than more light-demanding species. Conclusions: The woody seedling layer on BCI is composed of a subset of the species present in larger size classes. Most species were present in less than 1% of seedling plots, suggesting strong recruitment limitation. Tree species abundance in the seedling layer is largely a function of reproductive adult abundance, but is also influenced by life history strategies and compensatory processes. C1 Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Comita, LS (reprint author), Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. EM liza@plantbio.uga.edu; saloagui@hotmail.com; perezro@si.edu; laoz@si.edu; shubbell@plantbio.uga.edu NR 58 TC 46 Z9 56 U1 4 U2 39 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD APR PY 2007 VL 18 IS 2 BP 163 EP 174 DI 10.1658/1100-9233(2007)18[163:POWPSA]2.0.CO;2 PG 12 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 160IC UT WOS:000245933100002 ER PT J AU Cappellaro, P Hodges, JS Havel, TF Cory, DG AF Cappellaro, P. Hodges, J. S. Havel, T. F. Cory, D. G. TI Control of qubits encoded in decoherence-free subspaces SO LASER PHYSICS LA English DT Article ID QUANTUM COMPUTATION; INFORMATION; PRINCIPLES; DYNAMICS; PULSES; DESIGN AB Decoherence-free subspaces protect quantum information from the effects of noise that is correlated across the physical qubits used to implement them. Given the ability to impose suitable Hamiltonians upon such a multi-qubit system, one can also implement a set of logical gates which enables universal computation on this information without compromising this protection. Real physical systems, however, seldom come with the correct Hamiltonians built-in, let alone the ability to turn them off and on at will. In the course of our development of quantum information processing devices based on liquid-state NMR, we have found the task of operating on quantum information encoded in decoherence-free subspaces rather more challenging than is commonly assumed. This contribution presents an overview of these challenges and the methods we have developed for overcoming them in practice. These methods promise to be broadly applicable to many of the physical systems proposed for the implementation of quantum information processing devices. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. MIT, Dept Nucl Sci & Engn, Cambridge, MA 02139 USA. RP Cappellaro, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. EM pcappell@cfa.harvard.edu RI Hodges, Jonathan/G-1034-2010; Cappellaro, Paola/B-1413-2010; OI Cappellaro, Paola/0000-0003-3207-594X; Hodges, Jonathan/0000-0002-3487-6698 NR 25 TC 2 Z9 2 U1 0 U2 0 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1054-660X J9 LASER PHYS JI Laser Phys. PD APR PY 2007 VL 17 IS 4 BP 545 EP 551 DI 10.1134/S1054660X0704038X PG 7 WC Optics; Physics, Applied SC Optics; Physics GA 158QO UT WOS:000245807500038 ER PT J AU Guzman, HM Cortes, J AF Guzman, Hector M. Cortes, Jorge TI Reef recovery 20 years after the 1982-1983 El Nino massive mortality SO MARINE BIOLOGY LA English DT Article ID GALAPAGOS-ISLANDS ECUADOR; SOUTHERN OSCILLATION EVENT; TROPICAL EASTERN PACIFIC; CORAL-REEFS; COSTA-RICA; PHASE-SHIFTS; PANAMA; REPRODUCTION; VARIABILITY; RECRUITMENT AB For over 20 years the El Nino-Southern Oscillation (ENSO) has caused damage to the coral reefs of the eastern Pacific and other regions. In the mid-1980s scientists estimated that coral cover was reduced by 50-100% in several countries across the region. Almost 20 years (2002) after the 1982-1983 event, we assessed the recovery of the virtually destroyed reefs at Cocos Island (Costa Rica), previously evaluated in 1987 and reported to have less than 4% live coral cover. We observed up to fivefold increase in live coral cover which varied among reefs surveyed in 1987 and 2002. Most new recruits and adults belonged to the main reef building species from pre-1982 ENSO, Porites lobata, suggesting that a disturbance as outstanding as El Nino was not sufficient to change the role or composition of the dominant species, contrary to phase shifts reported for the Caribbean. During the 1990s, new species were observed growing on the reefs. Notably, Leptoseris scabra, considered to be rare in the entire Pacific, was commonly found in the area. Recovery may have begun with the sexual and asexual recruits of the few surviving colonies of P. lobata and Pavona spp. and with long distance transport of larvae from remote reefs. We found an overall 23% live coral cover by 2002 and with one reef above 58% indicating that Cocos Island coral reefs are recovering. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Univ Costa Rica, CIMAR, San Jose 2060, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose 2060, Costa Rica. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, Miami, FL 34002 USA. EM guzmanh@si.edu NR 61 TC 44 Z9 47 U1 2 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD APR PY 2007 VL 151 IS 2 BP 401 EP 411 DI 10.1007/s00227-006-0495-x PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 149CX UT WOS:000245125400001 ER PT J AU Perrin, WF Robertson, KM Van Bree, PJH Mead, JG AF Perrin, William F. Robertson, Kelly M. Van Bree, Peter J. H. Mead, James G. TI Cranial description and genetic identity of the holotype specimen of Tursiops aduncus (Ehrenberg, 1832) SO MARINE MAMMAL SCIENCE LA English DT Article DE cetacea; delphinidae; bottlenose dolphin; nomenclature; taxonomy; morphology; genetics; mtDNA; discriminant analysis; Indo-Pacific; Red Sea ID BOTTLE-NOSED DOLPHINS; MITOCHONDRIAL-DNA; GENUS TURSIOPS; SYMPATRIC MORPHOTYPES; CHINESE WATERS; SEQUENCES; AUSTRALIA; WHALE AB Two species of bottlenose dolphins are currently recognized by most cetologists: the pan-tropical and temperate Tursiops truncatus and the endemic Indo-Pacific T aduncus. The latter was described from a specimen from the Red Sea, with nothing in the description that would allow referral of the specimen to one or the other of the two species. Because both species occur in the northern Indian Ocean, it was possible that the holotype specimen was actually a common bottlenose dolphin, not of the Indo-Pacific species. The holotype skull was thought lost but has been found in the Berlin Museum. We describe the skull and examine its affinities through comparison of a partial mtDNA control-region sequence with sequences from South Africa and through application of classification functions from a discriminant analysis of the two putative species from Taiwan. The mtDNA sequence is identical to that of South African specimens referred to the Indo-Pacific species, and the multivariate likelihood assignment associates the skull with Taiwanese specimens referred to that species. These results ensure the correctness of use of the name T aduncus for the species. C1 SW Fisheries Sci Ctr, La Jolla, CA 92037 USA. Univ Amsterdam, Zool Museum, NL-1090 GT Amsterdam, Netherlands. Smithsonian Inst, Div Mammals, MRC 108, Washington, DC 20013 USA. RP Perrin, WF (reprint author), SW Fisheries Sci Ctr, 8604 La Jolla Shores Dr, La Jolla, CA 92037 USA. EM william.perrin@noaa.gov NR 34 TC 11 Z9 15 U1 0 U2 5 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD APR PY 2007 VL 23 IS 2 BP 343 EP 357 DI 10.1111/j.1748-7692.2007.00119.x PG 15 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 154ZF UT WOS:000245546600007 ER PT J AU Perez, GAC Rican, O Orti, G Bermingham, E Doadrio, I Zardoya, R AF Perez, Gustavo A. Concheiro Rican, Oldrich Orti, Guillermo Bermingham, Eldredge Doadrio, Ignacio Zardoya, Rafael TI Phylogeny and biogeography of 91 species of heroine cichlids (Teleostei : Cichlidae) based on sequences of the cytochrome b gene SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cichlidae; Caribbean geology; Greater Antilles biogeography; Middle American biogeography; molecular systematics ID CICHLASOMA-CITRINELLUM; CENTRAL-AMERICA; EVOLUTIONARY HISTORY; DIVERGENCE TIMES; FISHES; SYSTEMATICS; PHYLOGEOGRAPHY; SPECIATION; ISTHMUS; MAMMALS AB Heroini constitute the second largest tribe of Neotropical cichlids and show their greatest diversity in Mesoamerica. Although heroine species are morphologically and ecologically very diverse, they were all historically assigned to one single genus, Cichlasoma that was never formally revised from a phylogenetic point of view. Here, we present the most comprehensive molecular phylogeny of the tribe Heroini to date, based on the complete DNA sequence of the mitochondrial gene cytochrome b, and the analysis of 204 individuals representing 91 species. Phylogenetic analyses did not support the monophyly of heroines because the genus Pterophyllum was placed as the sister group of all remaining heroines plus cichlasomatines. However, the recovered relative position of Pterophyllum was without strong statistical support. Within the remaining heroines, Hyspelecara and Hoplarchus are recovered with low support in a basal position with respect to a clade that includes Heros, Uaru, Mesonauta, and Symphysodon, and the circumamazonian (CAM) heroines. The first clade is restricted to South America. The largest clade of heroines, the CAM heroines, include more than 85% of the species within the tribe. This clade is mostly Mesoamerican, but also contains four species found in the Greater Antilles (Nandopsis), and three genera found in South America (the 'Heros' festae group, Australoheros, and Caquetaia). Up to eight major lineages can be recovered within the CAM heroines, but the phylogenetic relationships among them remain unresolved. Two large suprageneric groups can be distinguished, the amphilophines and the herichthyines. The amphilophines include Amphilophus, Archocentrus, Hypsophrys, Neetroplus, Parachromis, Petenia, and five additional unnamed genera (the 'Heros' istlanus group, the 'Amphilophus' calobrensis group, the 'Heros' urophthalmus group, the 'Heros' wesseli group, and the 'Heros' sieboldii group). The herichthyines include the crown-group herichthyines (Herichthys, Theraps, Vieja, and Paratheraps) and the genera Tomocichla, Herotilapia, and Thorichthys, together with three unnamed genera (the 'Heros' umbriferus group, the 'Heros' grammodes group, and the 'Heros' salvini group). Amphilophines are prevalent in southern Mesomerica south of the Motagua fault. Herichthyines have basal linages in Central America, whereas crown-group herichthyines and three related genera are found north from the Motagua fault. At least two independent origins are required to explain current Mesoamerican heroine distribution. Dispersal of heroines from South America into Mesoamerica was dated between 24 and 16 million years ago (MYA) based on geological calibrations and on standard fish mitochondrial cytochrome b rates, respectively. These datings cannot be reconciled with currently known geological evidence, and the existence of a connection between Central America and South America in the Miocene needs to be postulated in order to explain the origins of Mesoamerican heroine lineages. However, our datings agree with those estimated for the dispersal of other secondary freshwater fishes (Rivulidae, Synbranchus) into Mesoamerica, and predate the invasion of primary freshwater fishes by at least 10 myr. (c) 2006 Elsevier Inc. All rights reserved. C1 Univ S Bohemia, Fac Biol Sci, Dept Zool, Ceske Budejovice 37005, Czech Republic. Smithsonian Trop Res Inst, Balboa, Panama. Acad Sci Czech Republic, Inst Anim Physiol & Genet, CR-27721 Libechov, Czech Republic. Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, E-28006 Madrid, Spain. RP Rican, O (reprint author), Univ S Bohemia, Fac Biol Sci, Dept Zool, Branisovska 31, Ceske Budejovice 37005, Czech Republic. EM oldrichr@yahoo.com RI Zardoya, Rafael/B-2291-2012; OI Zardoya, Rafael/0000-0001-6212-9502; Doadrio, Ignacio/0000-0003-4863-9711 NR 81 TC 66 Z9 67 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 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2007 VL 43 IS 1 BP 91 EP 110 DI 10.1016/j.ympev.2006.08.012 PG 20 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 160JF UT WOS:000245936000008 PM 17045493 ER PT J AU Gutierrez-Rodriguez, C Morris, MR Dubois, NS de Queiroz, K AF Gutierrez-Rodriguez, Carla Morris, Molly R. Dubois, Natalie S. de Queiroz, Kevin TI Genetic variation and phylogeography of the swordtail fish Xiphophorus cortezi (Cyprinodontiformes, Poeciliidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE genetic differentiation; gene flow; monophyletic; mitochondrial DNA; swordtail; Xiphophorus cortezi ID DNA-SEQUENCE DATA; COTTUS-GOBIO L; MITOCHONDRIAL-DNA; POPULATION DIFFERENTIATION; CHONDROSTOMA-LUSITANICUM; CENTRAL-EUROPE; RETICULATA; VARIABILITY; MODEL; HAPLOTYPES AB Swordtail fish have been studied extensively in relation to diverse aspects of biology; however, little attention has been paid to the patterns of genetic variation within and among populations of swordtails. In this study, we sequenced the mtDNA control region from 65 individuals and 10 populations of Xiphophorus cortezi to investigate the genetic variation within and among populations, including tests for correlations between genetic and geographic distances and tests for species monophyly. We found low gene and nucleotide diversity within populations and high degrees of genetic differentiation among populations. Significant and positive correlations between genetic distance and both river and straight-line geographic distance indicate that genetic differentiation among X. cortezi populations can be explained, to some extent, by an isolation-by-distance model and provide evidence of stream capture. Phylogenetic analyses suggest that X. cortezi is paraphyletic relative to X. malinche, raising questions concerning the status of these taxa as separate species. (c) 2006 Elsevier Inc. All rights reserved. C1 Ohio Univ, Dept Biol Sci, Athens, OH 45701 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Gutierrez-Rodriguez, C (reprint author), Inst Ecol, Dept Biol Evolut, AC Km 2-5 Antigua Carretera Coatepec 351, Veracruz 91070, Mexico. EM carla.gutierrez@inecol.edu.mx RI Gutierrez-Rodriguez, Carla/E-1559-2015; OI Morris, Molly/0000-0001-9962-2982 NR 48 TC 14 Z9 14 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2007 VL 43 IS 1 BP 111 EP 123 DI 10.1016/j.ympev.2006.10.022 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 160JF UT WOS:000245936000009 PM 17194605 ER PT J AU Foley, DH Wilkerson, RC Cooper, RD Volovsek, ME Bryan, JH AF Foley, D. H. Wilkerson, R. C. Cooper, R. D. Volovsek, M. E. Bryan, J. H. TI A molecular phylogeny of Anopheles annulipes (Diptera : Culicidae) sensu lato: The most species-rich anopheline complex SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Anopheles annulipes; phylogenetics; Bayesian; maximum parsimony; sibling species; species complex; myxomatosis; DNA barcoding; Australia; Papua New Guinea; ITS2; COI; COII; EF-1 alpha ID NEW-SOUTH-WALES; WALKER DIPTERA; SEQUENCE ALIGNMENT; BAYESIAN ANALYSES; MITOCHONDRIAL; GRIFFITH; EVOLUTION; PATTERNS; GENE; ITS2 AB The Australasian Annulipes Complex is the most species-rich among Anopheles mosquitoes, with at least 15 sibling species suspected. Members of this complex are the most likely vectors of malaria in the past in southern Australia and are involved in the spread of myxomatosis among rabbits. In this, the first comprehensive molecular study of the Annulipes Complex, 23 ITS2 rDNA variants were detected from collections throughout Australia and Papua New Guinea, including diagnostic variants for the previously identified An. annulipes species A-G. Specimens of each ITS2 variant were sequenced for portions of the mitochondrial COI, COII and nuclear EF-1 alpha genes. Partitioned Bayesian and Maximum Parsimony analyses confirmed the monophyly of the Annulipes Complex and revealed at least 17 clades that we designate species A-Q. These species belong to two major clades, one in the north and one mainly in the south, suggesting that climate was a driver of species radiation. We found that 65% (11) of the 17 sibling species recorded here had unique COI sequences, suggesting that DNA barcoding will be useful for diagnosing species within the Annulipes Complex. A comparison of the taxa revealed morphological characters that may be diagnostic for some species. Our results substantially increase the size of the subgenus Cellia in Australasia, and will assist species-level studies of the Annulipes Complex. (c) 2006 Elsevier Inc. All rights reserved. C1 Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD 20910 USA. Australian Army Malaria Inst, Lexington, KY 40511 USA. Univ Queensland, Trop Hlth Program, Brisbane, Qld 4072, Australia. Univ Queensland, Dept Zool & Entomol, Brisbane, Qld 4072, Australia. RP Foley, DH (reprint author), Smithsonian Inst, Walter Red Biosystemat Unit, MSC MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM foleydes@si.edu OI Foley, Desmond/0000-0001-7525-4601 NR 49 TC 33 Z9 35 U1 0 U2 9 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 2007 VL 43 IS 1 BP 283 EP 297 DI 10.1016/j.ympev.2006.10.008 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 160JF UT WOS:000245936000021 PM 17126567 ER PT J AU Ginsburg, I Loeb, A AF Ginsburg, Idan Loeb, Abraham TI Hypervelocity collisions of binary stars at the Galactic Centre SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; stellar dynamics; galaxy : centre; galaxy : kinematics and dynamics ID MAIN-SEQUENCE STARS; GAMMA-RAY BURSTS; BLACK-HOLE; STELLAR COLLISIONS; BLUE STRAGGLERS; SDSS J090745.0+024507; GLOBULAR-CLUSTERS; MULTIPLICITY; ENCOUNTERS; DYNAMICS AB Recent surveys have identified seven hypervelocity stars (HVSs) in the halo of the Milky Way. Most of these stars may have originated from the breakup of binary star systems by the nuclear black hole SgrA*. In some instances, the breakup of the binary may lead to a collision between its member stars. We examine the dynamical properties of these collisions by simulating thousands of different binary orbits around SgrA* with a direct N-body integration code. For some orbital parameters, the two stars collide with an impact velocity lower than their escape velocity and may therefore coalesce. It is possible for a coalescing binary to have sufficient velocity to escape the galaxy. Furthermore, some of the massive S-stars near Sgr A* might be the merger remnants of binary systems, however this production method can not account for most of the S-stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ginsburg, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM iginsburg@cfa.harvard.edu; aloeb@cfa.harvard.edu NR 37 TC 19 Z9 19 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 APR 1 PY 2007 VL 376 IS 2 BP 492 EP 496 DI 10.1111/j.1365-2966.2007.11461.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157CY UT WOS:000245697400003 ER PT J AU McGowan, KE Coe, MJ Schurch, M McBride, VA Galache, JL Edge, WRT Corbet, RHD Laycock, S Udalski, A Buckley, DAH AF McGowan, K. E. Coe, M. J. Schurch, M. McBride, V. A. Galache, J. L. Edge, W. R. T. Corbet, R. H. D. Laycock, S. Udalski, A. Buckley, D. A. H. TI X-ray bright sources in the Chandra Small Magellanic Cloud Wing Survey - detection of two new pulsars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE X-rays : binaries; stars : emission-line, Be; Magellanic Clouds ID GRAVITATIONAL LENSING EXPERIMENT; SMC REGION; RADIO-CONTINUUM; BINARIES; CATALOG; PHOTOMETRY; PERIOD; VARIABILITY; BEHAVIOR; STARS AB We investigate the X-ray and optical properties of a sample of X-ray bright sources from the Small Magellanic Cloud (SMC) Wing Survey. We have detected two new pulsars with pulse periods of 65.8 s (CXOU J010712.6-723533) and 700 s (CXOU J010206.6-714115), and present observations of two previously known pulsars RX J0057.3-7325 (SXP101) and SAX J0103.2-7209 (SXP348). Our analysis has led to three new optical identifications for the detected pulsars. We find long-term optical periods for two of the pulsars, CXOU J010206.6-714115 and SXP101, of 267 and 21.9d, respectively. Spectral analysis of a subset of the sample shows that the pulsars have harder spectra than the other sources detected. By employing a quantile-based colour-colour analysis we are able to separate the detected pulsars from the rest of the sample. Using archival catalogues we have been able to identify counterparts for the majority of the sources in our sample. Combining this with our results from the temporal analysis of the Chandra data and archival optical data, the X-ray spectral analysis, and by determining the X-ray to optical flux ratios we present preliminary classifications for the sources. In addition to the four detected pulsars, our sample includes two candidate foreground stars, 12 probable active galactic nuclei, and five unclassified sources. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Space Res Assoc, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. S African Astron Observ, ZA-7935 Cape Town, South Africa. So African Large Telescope Fdn, ZA-7935 Cape Town, South Africa. RP McGowan, KE (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM kern@astro.soton.ac.uk NR 47 TC 17 Z9 17 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 APR 1 PY 2007 VL 376 IS 2 BP 759 EP 770 DI 10.1111/j.1365-2966.2007.11468.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157CY UT WOS:000245697400024 ER PT J AU Wang, T Rajapakse, R Yelin, SF AF Wang, T. Rajapakse, R. Yelin, S. F. TI Electromagnetically induced transparency and slow light with n-doped GaAs SO OPTICS COMMUNICATIONS LA English DT Article ID PHOTON TURNSTILE DEVICE; ATOMIC ENSEMBLES; QUANTUM-WELLS; BOUND EXCITONS; COMMUNICATION; ENTANGLEMENT; COHERENCE; STORAGE; STATES; GAS AB The suitability of bound exciton system in semiconductors is studied for use in nonlinear optical schemes based on EIT, such as "slow" or "stored" photons. We match the desired properties of such a system exhibiting EIT with the known physical realities of a semiconductor system, and suggest, in particular, two suitable schemes using donor impurities in GaAs. In addition to generic properties, we also focus on the influence of many neighboring levels and continuum levels, and on the effect of strong hole-mixing. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Wang, T (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM tunwang@phys.uconn.edu NR 48 TC 10 Z9 10 U1 2 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0030-4018 J9 OPT COMMUN JI Opt. Commun. PD APR 1 PY 2007 VL 272 IS 1 BP 154 EP 160 DI 10.1016/j.optcom.2006.11.033 PG 7 WC Optics SC Optics GA 143MU UT WOS:000244727200024 ER PT J AU Woodroffe, R Davies-Mostert, H Ginsberg, J Graf, J Leigh, K McCreery, K Mills, G Pole, A Rasmussen, G Robbins, R Somers, M Szykman, M AF Woodroffe, Rosie Davies-Mostert, Harriet Ginsberg, Joshua Graf, Jan Leigh, Kellie McCreery, Kim Mills, Gus Pole, Alistair Rasmussen, Gregory Robbins, Robert Somers, Michael Szykman, Micaela TI Rates and causes of mortality in Endangered African wild dogs Lycaon pictus: lessons for management and monitoring SO ORYX LA English DT Article DE African wild dog; carnivore; human-wildlife conflict; intraguild predation; Lycaon pictus; radio telemetry; snare; wildlife disease ID TELEMETRY; SURVIVAL AB Effective species conservation depends upon correctly identifying the threats that cause decline or hinder recovery. Because estimates of the relative viability of different populations of Endangered African wild dogs Lycaon pictus are most strongly influenced by adult and pup mortality, we analysed rates and causes of mortality in eight wild dog populations under study in southern and eastern Africa. The probabilities of detecting wild dog deaths were influenced by the monitoring methods used. The least biased estimates of mortality causes were obtained through intensive monitoring of radio-collared individuals; this is impossible for pups, however. Mortality patterns varied substantially between populations. Rates of human-caused mortality were higher for wild dogs radio-collared outside protected areas than for those collared inside, but rates of natural mortality were comparable, suggesting that anthropogenic mortality is additive to natural mortality. The relative importance of factors such as snaring and infectious disease also varied regionally. Hence, although our analyses identified no new threats beyond those highlighted in a 1997 range-wide Action Plan, they suggest that local plans will be valuable to target conservation activities more precisely. C1 Univ Calif Davis, Dept Wildlife Fish & Conservat Biol, Davis, CA 95616 USA. Venetia Limpopo & Marakele Wild Dog Projects Enda, ZA-0900 Musina, South Africa. Wildlife Conservat Soc, Bronx, NY 10460 USA. Univ KwaZulu Natal, Sch Biol & Conservat Sci, ZA-4041 Durban, South Africa. African Wild Dog Conservat, Eastern Province, Zambia. African Wild Dog Conservancy, Tucson, AZ 85751 USA. SANParks Endangered Wildlife Trust, ZA-1350 Skukuza, South Africa. Univ Pretoria, Ctr Invas Biol, Ctr Wildlife Managment, ZA-0002 Pretoria, South Africa. Smithsonian Natl Zool Pk Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Woodroffe, R (reprint author), Univ Calif Davis, Dept Wildlife Fish & Conservat Biol, 1 Shields Ave, Davis, CA 95616 USA. EM rwoodroffe@ucdavis.edu RI Somers, Michael/A-1523-2008; OI Szykman Gunther, Micaela/0000-0002-7822-8094; /0000-0002-5836-8823 NR 21 TC 26 Z9 26 U1 8 U2 57 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0030-6053 J9 ORYX JI Oryx PD APR PY 2007 VL 41 IS 2 BP 215 EP 223 DI 10.1017/S0030605307001809 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 181ML UT WOS:000247440700018 ER PT J AU Cappellaro, P Hodges, JS Havel, TF Cory, DG AF Cappellaro, P. Hodges, J. S. Havel, T. F. Cory, D. G. TI Subsystem pseudopure states SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM ERROR-CORRECTION; EXPERIMENTAL REALIZATION; CORRECTING CODES; COMPUTATION; INFORMATION; DECOHERENCE; IMPLEMENTATION; RESONANCE AB A critical step in experimental quantum information processing (QIP) is to implement control of quantum systems protected against decoherence via informational encodings, such as quantum error-correcting codes, noiseless subsystems, and decoherence-free subspaces. These encodings lead to the promise of fault-tolerant QIP, but they come at the expense of resource overheads. Part of the challenge in studying control over multiple logical qubits is that QIP testbeds have not had sufficient resources to analyze encodings beyond the simplest ones. The most relevant resources are the number of available qubits and the cost to initialize and control them. Here we demonstrate an encoding of logical information that permits control over multiple logical qubits without full initialization, an issue that is particularly challenging in liquid-state NMR. The method of subsystem pseudopure states will allow the study of decoherence control schemes on up to six logical qubits using liquid-state NMR implementations. C1 MIT, Dept Nucl Sci & Engn, Cambridge, MA 02139 USA. RP Cappellaro, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Hodges, Jonathan/G-1034-2010; Cappellaro, Paola/B-1413-2010; OI Cappellaro, Paola/0000-0003-3207-594X; Hodges, Jonathan/0000-0002-3487-6698 NR 42 TC 4 Z9 4 U1 0 U2 1 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 APR PY 2007 VL 75 IS 4 AR 042321 DI 10.1103/PhysRevA.75.042321 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 162GJ UT WOS:000246074600046 ER PT J AU Zhao, B Chen, ZB Pan, JW Schmiedmayer, J Recati, A Astrakharchik, GE Calarco, T AF Zhao, Bo Chen, Zeng-Bing Pan, Jian-Wei Schmiedmayer, Joerg Recati, Alessio Astrakharchik, Grigory E. Calarco, Tommaso TI High-fidelity entanglement via molecular dissociation in integrated atom optics SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATE; CONTROLLED COLLISIONS; FESHBACH RESONANCES; QUANTUM COMPUTATION; NEUTRAL ATOMS; GAS; LATTICE; STATE; WIRES; CHIP AB High-fidelity entanglement of neutral cold atoms can be achieved by combining several already available techniques such as the creation or dissociation of neutral diatomic molecules, manipulating atoms with microfabricated structures (atom chips), and detecting single atoms with almost 100% efficiency. The fidelity of the resulting entanglement is robust against the details of dissociation process. Manipulating this entanglement with integrated or linear atom optics will open a perspective for quantum-information processing with neutral atoms. C1 Univ Heidelberg, Inst Phys, D-69120 Heidelberg, Germany. Univ Sci & Technol China, Hefei Natl Lab Phys Sci Microscale, Hefei 230026, Anhua, Peoples R China. Univ Sci & Technol China, Dept Modern Phys, Hefei 230026, Anhua, Peoples R China. Vienna Univ Technol, Atominst Osterreichischen Univ, A-1020 Vienna, Austria. Univ Trent, Dipartimento Fis, BEC INFM, I-38050 Trento, Italy. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Zhao, B (reprint author), Univ Heidelberg, Inst Phys, Philosophenweg 12, D-69120 Heidelberg, Germany. RI Schmiedmayer, Jorg/B-4717-2008; Pan, Jian-Wei/A-2332-2010; Astrakharchik, Gregory/L-6181-2014; Recati, Alessio/J-7566-2015 OI Schmiedmayer, Jorg/0000-0001-7799-5614; Pan, Jian-Wei/0000-0002-6100-5142; Astrakharchik, Gregory/0000-0003-0394-8094; NR 44 TC 12 Z9 12 U1 1 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 2007 VL 75 IS 4 AR 042312 DI 10.1103/PhysRevA.75.042312 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 162GJ UT WOS:000246074600037 ER PT J AU Afshordi, N Chung, DJH Geshnizjani, G AF Afshordi, Niayesh Chung, Daniel J. H. Geshnizjani, Ghazal TI Causal field theory with an infinite speed of sound SO PHYSICAL REVIEW D LA English DT Article ID SMALL COSMOLOGICAL CONSTANT; ACCELERATION AB We introduce a model of scalar field dark energy, Cuscuton, which can be realized as the incompressible (or infinite speed of sound) limit of a scalar field theory with a noncanonical kinetic term (or k-essence). Even though perturbations of Cuscuton propagate superluminally, we show that they have a locally degenerate phase space volume (or zero entropy), implying that they cannot carry any microscopic information, and thus the theory is causal. Even coupling to ordinary scalar fields cannot lead to superluminal signal propagation. Furthermore, we show that the family of constant field hypersurfaces is the family of constant mean curvature hypersurfaces, which are the analogs of soap films (or soap bubbles) in Euclidian space. This enables us to find the most general solution in 1+1 dimensions, whose properties motivate conjectures for global degeneracy of the phase space in higher dimensions. Finally, we show that the Cuscuton action can model the continuum limit of the evolution of a field with discrete degrees of freedom and argue why it is protected against quantum corrections at low energies. While this paper mainly focuses on interesting features of Cuscuton in a Minkowski space-time, a companion paper examines cosmology with Cuscuton dark energy. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. RP Afshordi, N (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, MS-51,60 Garden St, Cambridge, MA 02138 USA. EM nafshordi@cfa.harvard.edu; Danielchung@wisc.edu; ghazal@physics.wisc.edu NR 22 TC 63 Z9 63 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 APR PY 2007 VL 75 IS 8 AR 083513 DI 10.1103/PhysRevA.75.083513 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 162HG UT WOS:000246076900028 ER PT J AU Ikegami, M Whigham, DF Werger, MJA AF Ikegami, Makihiko Whigham, Dennis F. Werger, Marinus J. A. TI Responses of rhizome length and ramet production to resource availability in the clonal sedge Scirpus olneyi A. Gray SO PLANT ECOLOGY LA English DT Article DE architecture; clonal plant; foraging; life history strategy; Scirpus olneyi ID HERB GLECHOMA-HEDERACEA; MORPHOLOGICAL PLASTICITY; PLANTS; INTEGRATION; DYNAMICS AB The clonal plant Scirpus olneyi has two types of ramets within one clone; a ramet with a very long rhizome (LRR) and a ramet with a very short rhizome (SRR). Based on foraging theory of clonal plants, we hypothesised that these two types of ramets were functionally specialised to different tasks: the task of LRRs is for exploring while SRRs is for consolidating the patches. We also hypothesised that LRRs tended to produce LRRs continuously during a growing season to reach further patches while SRRs tended to produce SRRs fewer times to stay in the same patches. To evaluate these hypotheses, we analysed the sequence of two ramets of plants growing in four communities in the field and five treatments in garden experiments. In the garden experiments, plants in high quality treatments (e.g. low salinity, full sun, and sufficient nutrient) produced proportionally more SRRs and branched more frequently than plants in low quality treatments (e.g. strong salinity or less light or less nutrient). LRRs kept producing LRRs in every treatment, but LRRs in low quality treatments produced less SRRs than LRRs in high quality treatments did. The field observations showed LRRs kept producing LRRs in every community in the same growing season, but SRRs production varied among communities. In the communities with larger biomass and high SRR ratio, LRRs produced more SRRs and those SRRs produced proportionally more SRRs. On the other hand, in the communities with smaller biomass and low SRR ratio, LRRs produced less SRRs and those SRRs produced proportionally less SRRs. The results of garden experiments and field observations support our hypotheses. Two ramets are functionally specialised to perform different tasks. And their production patterns are suitable to perform their tasks. And their production patterns are suitable to perform their tasks: the sequential production of LRRs allows plants to have higher chance to reach new locations, and the limited but sequential production of SRRs allows plants to consolidate the patches. The observed production patterns of two ramets are associated with phalanx and guerrilla strategies by Lovett Doust, and S. olneyi shows both strategies within relatively small scale environments. C1 Univ Utrecht, Dept Plant Ecol, NL-3508 TB Utrecht, Netherlands. Smithsonian Environm Res Ctr, Plant Ecol Lab, Edgewater, MD 21037 USA. Univ Utrecht, Dept Landscape Ecol, NL-3508 TB Utrecht, Netherlands. RP Ikegami, M (reprint author), Forest Res, Alice Holt Lodge, Farnham GU10 4LH, Surrey, England. EM makihiko.ikegami@forestry.gsi.gov.uk RI IKEGAMI, Makihiko/E-6612-2012; OI Whigham, Dennis/0000-0003-1488-820X NR 20 TC 20 Z9 23 U1 1 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD APR PY 2007 VL 189 IS 2 BP 247 EP 259 DI 10.1007/s11258-006-9181-9 PG 13 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 146SD UT WOS:000244954100008 ER PT J AU Brown, JW Nishida, K AF Brown, John W. Nishida, Kenji TI A new gall-inducing Tortricid (Lepidoptera : Tortricidae : Olethreutinae) on lima bean (Phaseolus lunatus; Fabaceae) from Costa Rica SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE gall; life history; neotropics; new genus; new species; taxonomy; Cydia torostoma; Dolichogenidea ID WALSINGHAM LEPIDOPTERA AB Lusterala phaseolana, new genus and new species, is described and illustrated from Costa Rica. The new genus can be distinguished from all other Olethreutinae by its unusual male genitalia, with a digitate uncus covered with long hairs and the absence of socii, and its distinctive forewing maculation (i.e., dark brown with scattered iridescent scales). Assignment of the new genus to Grapholitini is provisional based on the general appearance and chaetotaxy of the larva and a feature of the wing venation (i.e., M-2 and M-3 parallel and widely separated at the base). The entire type series was reared from stem galls on lima bean, Phaseolus lunatus L. (Fabaceae). C1 USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. Univ Costa Rica, Escuela Biol, San Jose 2060, Costa Rica. RP Brown, JW (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM john.brown@ars.usda.gov; kenji.nishida@gmail.com NR 25 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 2007 VL 109 IS 2 BP 265 EP 276 PG 12 WC Entomology SC Entomology GA 157GZ UT WOS:000245708100001 ER PT J AU Henry, TJ AF Henry, Thomas J. TI A newly discovered Brazilian species of the stilt bug genus Jalysus (Hemiptera : Heteroptera : Berytidae) associated with myrmecophytic plants SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Hemiptera; Heteroptera; Berytidae; stilt bug; Jalysus; new species; distribution; hosts; Maeita AB The newly discovered stilt bug Jalysus ossesae, the smallest known species of the genus, is described from specimens collected near Manaus, Amazonas, Brazil, on two myrmecophytic species of the genus Maeita (Melastomataceae) associated with two species of ants (Formicidae). A diagnosis, description, photographs of the adult male, scanning electron photomicrographs of selected structures, and illustrations of male genitalia are provided to facilitate recognition. A discussion of the relationship with certain species of the genus is given. C1 USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Henry, TJ (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov NR 8 TC 2 Z9 3 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 2007 VL 109 IS 2 BP 324 EP 330 PG 7 WC Entomology SC Entomology GA 157GZ UT WOS:000245708100006 ER PT J AU Lucia, M Abrahamovich, AH Trejo, E Smith, DR AF Lucia, Mariano Abrahamovich, Alberto Horacio Trejo, Eleonora Smith, David R. TI First record of the raspberry pest Priophorus brullei (Dahlbom) (Hymenoptera : Tenthredinidae : Nematinae : Cladiini) in South America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 Natl Univ La Plata, Div Entomol, Museo La Plata, RA-1900 La Plata, Argentina. FAUBA, El Bolson, Rio Negro, Argentina. USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Lucia, M (reprint author), Natl Univ La Plata, Div Entomol, Museo La Plata, Paseo Bosque S-N, RA-1900 La Plata, Argentina. EM mlucia@fcnym.unlp.edu.ar; dave.smith@ars.usda.gov NR 11 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2007 VL 109 IS 2 BP 496 EP 498 PG 3 WC Entomology SC Entomology GA 157GZ UT WOS:000245708100024 ER PT J AU Gagne, RJ AF Gagne, Raymond J. TI Species numbers of Cecidomyiidae (Diptera) by zoogeographical region SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Gagne, RJ (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, NHB 168,POB 37012, Washington, DC 20013 USA. EM raymond.gagne@ars.usda.gov NR 1 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 2007 VL 109 IS 2 BP 499 EP 499 PG 1 WC Entomology SC Entomology GA 157GZ UT WOS:000245708100025 ER PT J AU Baeza, JA AF Baeza, J. Antonio TI The origins of symbiosis as a lifestyle in marine crabs (genus Petrolisthes) from the eastern Pacific: Does interspecific competition play a role? SO REVISTA DE BIOLOGIA MARINA Y OCEANOGRAFIA LA English DT Article DE symbiosis evolution; competition; phylogeny; comparative method; Petrolisthes ID ALLOPETROLISTHES-SPINIFRONS; CHARACTER DISPLACEMENT; PHYLOGENETIC ANALYSIS; HOST CHARACTERISTICS; PORCELLANID CRAB; PORCELAIN CRABS; SEA-ANEMONES; DECAPODA; CRUSTACEA; EVOLUTION AB The adoption of a symbiotic lifestyle is one of the main environmental adaptations in marine crustaceans. Interspecific competition might be considered important in explaining the evolution of symbiosis in this and other groups of marine invertebrates. Here, the historical origin of symbiosis as a lifestyle in marine crabs (genus Petrolisthes) from the eastern Pacific was examined, and the evolutionary role of intra-guild interspecific competition in explaining this ecological trait was explored. A previously published phylogenetic hypothesis for 29 species of Petrolisthes generated by Minimum Evolution and Maximum Parsimony methods of inference (using sequences of 16s rRNA mitochondrial DNA as a genetic marker) was used as framework for this analysis. When the lifestyle of each species was mapped onto the phylogenetic tree for Petrolisthes, a free-living habit was inferred to be the ancestral character state and symbiosis appeared to evolve independently at least twice in this group. Crabs with symbiotic associations occur in temperate waters in the southern hemisphere; Allopetrolisthes spinifrons inhabiting sea anemones, and Liopetrolisthes mitra inhabiting sea urchins. A comparative analysis by independent contrasts suggested that interspecific competition is not important in explaining either the evolution of symbiosis or the occurrence of less frequent partnerships between Petrolisthes crabs and other macro invertebrates. On the other hand, the adoption of a symbiotic lifestyle has important consequences for the social life of crabs. Symbiotic crabs are proposed as model system to examine the role of the environment in shaping the social behavior of marine invertebrates. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. OI Baeza, Juan Antonio/0000-0002-2573-6773 NR 58 TC 6 Z9 7 U1 0 U2 8 PU INST OCEANOLOGIA, UNIV VALPARAISO PI VINA DEL MAR PA CASILLA 13-D, VINA DEL MAR, 00000, CHILE SN 0717-3326 J9 REV BIOL MAR OCEANOG JI Rev. Biol. Mar. Oceanogr. PD APR PY 2007 VL 42 IS 1 BP 7 EP 21 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 208YK UT WOS:000249354900002 ER PT J AU Adelekan, AM Meyer, JJM Hussein, AA Urena, LD AF Adelekan, A. M. Meyer, J. J. M. Hussein, A. A. Urena, L. D. TI Bioactivity of novel compounds from Croton steenkampianus SO SOUTH AFRICAN JOURNAL OF BOTANY LA English DT Meeting Abstract C1 Univ Pretoria, Dept Bot, ZA-0002 Pretoria, South Africa. Natl Res Ctr, Dept Chem Med Plants, Cairo, Egypt. Smithsonian Trop Res Inst, Balboa, Panama. RI Meyer, Marion/E-3042-2010 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0254-6299 J9 S AFR J BOT JI S. Afr. J. Bot. PD APR PY 2007 VL 73 IS 2 BP 276 EP 276 DI 10.1016/j.sajb.2007.02.010 PG 1 WC Plant Sciences SC Plant Sciences GA 165NR UT WOS:000246312700025 ER PT J AU Ramirez, MJ Coddington, JA Maddison, WP Midford, PE Prendini, L Miller, J Griswold, CE Hormiga, G Sierwald, P Scharff, N Benjamin, SP Wheeler, WC AF Ramirez, Martin J. Coddington, Jonathan A. Maddison, Wayne P. Midford, Peter E. Prendini, Lorenzo Miller, Jeremy Griswold, Charles E. Hormiga, Gustavo Sierwald, Petra Scharff, Nikolaj Benjamin, Suresh P. Wheeler, Ward C. TI Linking of digital images to phylogenetic data matrices using a morphological ontology SO SYSTEMATIC BIOLOGY LA English DT Article DE AToL; Araneae; bioinformatics; digital images; documentation; morphology; ontology; phylogenetics; spiders; systematics ID DATA SETS; TAXONOMY; ARANEAE; DISCIPLINE; ARANEOIDEA; DATABASES; INFERENCE; SPIDERS; THINGS; MODEL AB Images are paramount in documentation of morphological data. Production and reproduction costs have traditionally limited bow many illustrations taxonomy could afford to publish, and much comparative knowledge continues to be lost as generations turn over. Now digital images are cheaply produced and easily disseminated electronically but pose problems in maintenance, curation, sharing, and use, particularly in long-term data sets involving multiple collaborators and institutions. We propose an efficient linkage of images to phylogenetic data sets via an ontology of morphological terms; an underlying, fine-grained database of specimens, images, and associated metadata; fixation of the meaning of morphological terms (homolog names) by ostensive references to particular taxa; and formalization of images as standard views. The ontology provides the intellectual structure and fundamental design of the relationships and enables intelligent queries to populate phylogenetic data sets with images. The database itself documents primary morphological observations, their vouchers, and associated metadata, rather than the conventional data set cell, and thereby facilitates data maintenance despite character redefinition or specimen reidentification. It minimizes reexamination of specimens, loss of information or data quality, and echoes the data models of web-based repositories for images, specimens, and taxonomic names. Confusion and ambiguity in the meanings of technical morphological terms are reduced by ostensive definitions pointing to features in particular taxa, which may serve as reference for globally unique identifiers of characters. Finally, the concept of standard views (an image illustrating one or more homologs in a specific sex and life stage, in a specific orientation, using a specific device and preparation technique) enables efficient, dynamic linkage of images to the data set and automatic population of matrix cells with images independently of scoring decisions. [AToL; Araneae; bioinformatics; digital images; documentation; morphology; ontology; phylogenetics; spiders; systematics.]. C1 Consejo Nacl Invest Cient & Tecn, Museo Argentino Ciencias Nat Bernardino Rivadavia, RA-1405 Buenos Aires, DF, Argentina. Smithsonian Inst, Washington, DC 20013 USA. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. Calif Acad Sci, Dept Entomol, San Francisco, CA 94103 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Field Museum Nat Hist, Chicago, IL USA. Univ Copenhagen, Dept Entomol, Zool Museum, DK-2100 Copenhagen, Denmark. RP Ramirez, MJ (reprint author), Consejo Nacl Invest Cient & Tecn, Museo Argentino Ciencias Nat Bernardino Rivadavia, Ave Angel Gallardo 470, RA-1405 Buenos Aires, DF, Argentina. EM ramirez@macn.gov.ar RI Midford, Peter/B-5946-2008; Hormiga, Gustavo/C-3874-2009; Scharff, Nikolaj/A-4787-2013; Smith, Barry/A-9525-2011; OI Scharff, Nikolaj/0000-0001-6809-2878; Smith, Barry/0000-0003-1384-116X; Miller, Jeremy/0000-0001-8918-9775; Midford, Peter/0000-0001-6512-3296 NR 65 TC 38 Z9 40 U1 0 U2 14 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD APR PY 2007 VL 56 IS 2 BP 283 EP 294 DI 10.1080/10635150701313848 PG 12 WC Evolutionary Biology SC Evolutionary Biology GA 167JP UT WOS:000246448300010 PM 17464883 ER PT J AU Brake, I Mathis, WN AF Brake, Irina Mathis, Wayne N. TI Revision of the genus Australimyza Harrison (Diptera : Australimyzidae) SO SYSTEMATIC ENTOMOLOGY LA English DT Article AB The species of Australimyza Harrison are revised and the saprophagous larvae are described for the first time. The phylogenetic analysis revealed two species groups and one ungrouped species. One species group is distributed in New Zealand and associated subantarctic islands; all other species occur in Australia. Four new species, A. glandulifera, A. kaikoura, A. mcalpinei and A. victoria, are described, A. anisotomae is synonymized with A. australensis and a neotype is designated for the latter species. A lectotype is designated for A. macquariensis. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Brake, I (reprint author), Nat Hist Museum, Dept Entomol, Cromwell Rd, London SW7 5BD, England. EM i.brake@nhm.ac.uk NR 26 TC 3 Z9 3 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0307-6970 J9 SYST ENTOMOL JI Syst. Entomol. PD APR PY 2007 VL 32 IS 2 BP 252 EP 275 DI 10.1111/j.1365-3113.2006.00363.x PG 24 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 157UF UT WOS:000245745800004 ER PT J AU Stine, JK AF Stine, Jeffrey K. TI A sense of place - Donald Worster's Dust Bowl SO TECHNOLOGY AND CULTURE LA English DT Article ID TECHNOLOGY; HISTORY C1 Smithsonian Inst, Amer Museum Nat Hist, Div Med & Sci, Washington, DC 20560 USA. RP Stine, JK (reprint author), Smithsonian Inst, Amer Museum Nat Hist, Div Med & Sci, Washington, DC 20560 USA. NR 33 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2007 VL 48 IS 2 BP 377 EP 385 DI 10.1353/tech.2007.0092 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA 163CS UT WOS:000246136900006 ER PT J AU Hacker, BC AF Hacker, Barton C. TI Warfare state: Britain, 1920-1970. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2007 VL 48 IS 2 BP 459 EP 460 DI 10.1353/tech.2007.0072 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 163CS UT WOS:000246136900039 ER PT J AU Miller, JA AF Miller, Jeremy A. TI Review of erigonine spider genera in the neotropics (Araneae : Linyphiidae, Erigoninae) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review ID WALCKENAERIA BLACKWALL ARANEAE; NORTH-AMERICA; GENUS; ARACHNIDA; MORPHOLOGY; RELATIVES; ISLANDS AB The Neotropical genera of the linyphiid spider subfamily Erigoninae are revised at the genus level. Emphasis was placed on genera endemic to the Neotropics and species with dubious relationships to their nominal genera, especially species from the older literature. This work recognizes 50 genera in the Neotropics, of which 39 genera are strictly endemic to the Neotropics, three are represented outside the Neotropics by one species, and eight genera have significant representation both in and beyond the Neotropics. Three additional genera, Ceraticelus Simon, 1884, Idionella Banks, 1893, and Eulaira Chamberlin & Ivie, 1933, are represented in northern Mexico and/or the West Indies, but are best classified as having a Nearctic or Holarctic distribution. Species previously placed in the typically northern hemisphere genera Gongylidiellum Simon, 1884, Leptorhoptrum Kulczynski, 1894, Macrargus Dahl, 1886, Minyriolus Simon, 1884, Oedothorax Bertkau, 1883, Phanetta Keyserling, 1886, and Tmeticus Menge, 1868 are found to be misplaced or nomina dubia; two genera endemic to the Neotropics, Clitistes Simon, 1902 and Zilephus Simon, 1902 are nomina dubia. The genus Beauchenia Usher, 1983 is an erigonine, not a mynoglenine; there are no known representatives of the Mynogleninae in the Neotropics. One hundred and forty new combinations are established; 19 genera are synonymized including Micromaso Tambs-Lyche, 1954, revalidation rejected; 34 species are synonymized. The following new genera are established: Gigapassus gen. nov., Intecymbium gen. nov., Moyosi gen. nov., Orfeo gen. nov. and Toltecaria gen. nov. Malkinella Millidge, 1991 and Valdiviella Millidge, 1985 are preoccupied; Malkinola nom. nov. and Valdiviola nom. nov. are established as replacement names. The following new species are described: Asemostera daedalus sp. nov., Asemostera enkidu sp. nov., Asemostera janetae sp. nov., Fissiscapus attercop sp. nov., Gonatoraphis lysistrata sp. nov., Gravipalpus standifer sp. nov., Microplanus odin sp. nov., Moyosi chumota sp. nov., Myrmecomelix leucippus sp. nov., Neomaso damocles sp. nov., Notiomaso exonychus sp. nov., Paraletes pogo sp. nov., Psilocymbium acanthodes sp. nov., Smermisia holdridgi sp. nov. and Smermisia parvoris sp. nov. The following species remain misplaced in inappropriate genera: Erigone fellita Keyserling, 1886, Erigone zabluta Keyserling, 1886, and Oedothorax fuegianus (Simon, 1902). For 23 species, type specimens could not be located and the species could not be unambiguously identified; the type of Macrargus pacificus Berland, 1924 could not be located, but it is transferred to Laminacauda Millidge, 1985. The female of Onychembolus subalpinus Millidge, 1985 described by Millidge in 1991 is mismatched; this female is Notiomaso exonychus sp. nov.; the true female of Onychembolus subalpinus was described as both Neomaso bidentatus Millidge, 1991 syn. nov. and Neomaso tridentatus Millidge, 1991 syn. nov. The male and female of Asemonetes [now Asemostera] arcana (Millidge, 1991) are not conspecific; a male thought to be conspecific with the female of A. arcana is newly described; the true female of A. arcana is unknown. The transfer of Emenista dentichelis Berland, 1913 to Laminacauda comb. nov. renders Laminacauda dentichelis Millidge, 1991 a junior homonym; the replacement name Laminacauda baerti nom. nov. is provided for Laminacauda dentichelis Millidge. The following species were erroneously placed in erigonine genera: Oedothorax bisignatus Mello-Leitao, 1945 is synonymized with Theridion calcynatum Holmberg, 1876 syn. nov (Theridiidae); Liger incomta O. Pickard-Cambridge, 1896 is transferred to Theridion Walckenaer, 1805 (Theridiidae) [Theridion incomtum comb. nov.]; Erigone ectrapela Keyserling, 1886 is transferred to Dictyna Sundevall, 1833 (Dictynidae) [Dictyna ectrapela comb. nov.]; Erigone peruana Keyserling, 1886 is transferred to Thymoites Keyserling, 1884 (Theridiidae) [Thymoites peruanus comb. nov.]; Adelonetria dubiosa Millidge, 1991 is not a linyphiid and will be dealt with elsewhere. Lomaita darlingtoni Bryant, 1948 is confirmed as a linyphiid, not a mysmenid. (c) 2007 The Linnean Society of London. C1 Museum Natl Hist Nat, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Miller, JA (reprint author), Calif Acad Sci, Dept Entomol, 875 Howard St, San Francisco, CA 94103 USA. EM jmiller@calacademy.org NR 191 TC 32 Z9 37 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD APR PY 2007 VL 149 SU 1 BP 1 EP 263 DI 10.1111/j.1096-3642.2007.00233.x PG 263 WC Zoology SC Zoology GA 156UX UT WOS:000245676500002 ER PT J AU Larsson, HCE Sues, HD AF Larsson, Hans C. E. Sues, Hans-Dieter TI Cranial osteology and phylogenetic relationships of Hamadasuchus rebouli (Crocodyliformes : Mesoeucrocodylia) from the Cretaceous of Morocco SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Crocodylomorpha; Hamadasuchus; skull ID SOUTH-ATLANTIC; CROCODYLOMORPHA; NIGER; CROCODILE; AFRICA; BRAZIL; CHINA; MADAGASCAR; PATAGONIA; SAHARA AB This paper presents a detailed description of the skull and part of the mandible of the crocodyliform reptile Hamadasuchus rebouli from the Kem Kem beds (Upper Cretaceous: Albian-Cenomanian) of south-eastern Morocco. This taxon of deep-snouted ziphodont crocodyliform can be diagnosed by a number of autapomorphies. Phylogenetic analysis of a diverse array of crocodylomorph taxa found strong support for a clade comprising H. rebouli, Peirosauridae, and Sebecus. The name Sebecia nom. nov. is proposed for this grouping, which is diagnosed by numerous characters, including the participation of the quadratojugal in the mandibular condyle. The distribution of this diverse and long-lived clade lends further support to the biogeographical hypothesis that faunal connections existed between Africa and South America well into mid-Cretaceous times. (c) 2007 The Linnean Society of London, Zoological Journal of the Linnean Society, 2007, 149, 533-567. C1 McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada. Natl Museum Nat Hist, Smithsonian Inst, NHB MRC 106, Washington, DC 20013 USA. RP Larsson, HCE (reprint author), McGill Univ, Redpath Museum, 859 Sherbrooke St W, Montreal, PQ H3A 2K6, Canada. EM hans.ce.larsson@mcgill.ca OI Larsson, Hans/0000-0002-6377-4770 NR 69 TC 70 Z9 73 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 APR PY 2007 VL 149 IS 4 BP 533 EP 567 DI 10.1111/j.1096-3642.2007.00271.x PG 35 WC Zoology SC Zoology GA 156UW UT WOS:000245676400002 ER PT J AU Fu, TM Jacob, DJ Palmer, PI Chance, K Wang, YXX Barletta, B Blake, DR Stanton, JC Pilling, MJ AF Fu, Tzung-May Jacob, Daniel J. Palmer, Paul I. Chance, Kelly Wang, Yuxuan X. Barletta, Barbara Blake, Donald R. Stanton, Jenny C. Pilling, Michael J. TI Space-based formaldehyde measurements as constraints on volatile organic compound emissions in east and south Asia and implications for ozone SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AMERICAN ISOPRENE EMISSIONS; BIOMASS-BURNING EMISSIONS; NITROGEN-OXIDE EMISSIONS; TRACE-P OBSERVATIONS; ART. NO. 4100; SATELLITE-OBSERVATIONS; NORTH-AMERICA; INTERANNUAL VARIABILITY; ANTHROPOGENIC EMISSIONS; TROPOSPHERIC CHEMISTRY AB We use a continuous 6-year record (1996 - 2001) of GOME satellite measurements of formaldehyde (HCHO) columns over east and south Asia to improve regional emission estimates of reactive nonmethane volatile organic compounds (NMVOCs), including isoprene, alkenes, HCHO, and xylenes. Mean monthly HCHO observations are compared to simulated HCHO columns from the GEOS-Chem chemical transport model using state-of-science, "bottom-up" emission inventories from Streets et al. (2003a) for anthropogenic and biomass burning emissions and Guenther et al. (2006) for biogenic emissions (MEGAN). We find that wintertime GOME observations can diagnose anthropogenic reactive NMVOC emissions from China, leading to an estimate 25% higher than Streets et al. (2003a). We attribute the difference to vehicular emissions. The biomass burning source for east and south Asia is almost 5 times the estimate of Streets et al. (2003a). GOME reveals a large source from agricultural burning in the North China Plain in June missing from current inventories. This source may reflect a recent trend toward in-field burning of crop residues as the need for biofuels diminishes. Biogenic isoprene emission in east and south Asia derived from GOME is 56 +/- 30 Tg yr(-1), similar to 52 Tg yr(-1) from MEGAN. We find, however, that MEGAN underestimates emissions in China and overestimates emissions in the tropics. The higher Chinese biogenic and biomass burning emissions revealed by GOME have important implications for ozone pollution. We find 5 to 20 ppb seasonal increases in surface ozone in GEOS-Chem for central and northern China when using GOME-derived versus bottom-up emissions. Our methodology can be adapted for other regions of the world to provide top-down constraints on NMVOC emissions where multiple emission source types overlap in space and time. C1 Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA. Univ Leeds, Dept Chem, Leeds LS2 9JT, W Yorkshire, England. RP Fu, TM (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland. EM fu@fas.harvard.edu RI Palmer, Paul/F-7008-2010; Wang, Yuxuan/C-6902-2014; Chem, GEOS/C-5595-2014; Fu, Tzung-May/N-3418-2015 OI Wang, Yuxuan/0000-0002-1649-6974; NR 76 TC 117 Z9 118 U1 8 U2 52 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 31 PY 2007 VL 112 IS D6 AR D06312 DI 10.1029/2006JD007853 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 155BW UT WOS:000245553800007 ER PT J AU Smith, BD AF Smith, Bruce D. TI The ultimate ecosystem engineers SO SCIENCE LA English DT Editorial Material ID DOMESTICATION C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. EM smithb@si.edu NR 6 TC 54 Z9 56 U1 3 U2 17 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAR 30 PY 2007 VL 315 IS 5820 BP 1797 EP 1798 DI 10.1126/science.1137740 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 151HC UT WOS:000245280100025 PM 17395815 ER PT J AU Davis, CC Latvis, M Nickrent, DL Wurdack, KJ Baum, DA AF Davis, Charles C. Latvis, Maribeth Nickrent, Daniel L. Wurdack, Kenneth J. Baum, David A. TI Floral gigantism in rafflesiaceae SO SCIENCE LA English DT Article ID FLOWERING PLANTS; GENE-TRANSFER; MALPIGHIALES C1 Harvard Univ Hebaria, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. So Illinois Univ, Dept Plant Biol, Carbondale, IL 62901 USA. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. RP Davis, CC (reprint author), Harvard Univ Hebaria, Dept Organism & Evolutionary Biol, 22 Divin Ave, Cambridge, MA 02138 USA. EM cdavis@oeb.harvard.edu RI Baum, David/D-6804-2015 OI Baum, David/0000-0001-8334-6311 NR 10 TC 74 Z9 80 U1 5 U2 31 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 30 PY 2007 VL 315 IS 5820 BP 1812 EP 1812 DI 10.1126/science.1135260 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 151HC UT WOS:000245280100033 PM 17218493 ER PT J AU Liao, YL Pawson, DL Liu, W AF Liao, Yulin Pawson, David L. Liu, Wei TI Rediscovery of the sea cucumber "Toxodora" pacifica Ohshima, 1915 (Echinodermata : Holothuroidea : Apodida) SO ZOOTAXA LA English DT Article DE Toxodora; Neotoxodora pacifica; Holothuroidea; Apodida; Yellow Sea AB The apodous holothurian species originally described by Ohshima ( 1915) as Toxodora pacifica has been rediscovered, and its known geographic range extended from Suruga Bay, Japan to the western side of the Yellow Sea, China. As the genus name Toxodora is no longer available, a new genus name, Neotoxodora Liao, Pawson, and Wei, is proposed. The type material of Neotoxodora pacifica is lost, and a Neotype is named for this species. C1 Chinese Acad Sci, Inst Oceanol, Qingdao 266071, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Wei Fang Marine Environm Monitoring Cent Stn Shan, Wei Fang 261041, Peoples R China. RP Liao, YL (reprint author), Chinese Acad Sci, Inst Oceanol, Qingdao 266071, Peoples R China. EM pawsond@si.edu NR 9 TC 0 Z9 0 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 29 PY 2007 IS 1435 BP 37 EP 40 PG 4 WC Zoology SC Zoology GA 151JG UT WOS:000245285700004 ER PT J AU Jaron-Becker, A Becker, A Faisal, FHM AF Jaron-Becker, A. Becker, A. Faisal, F. H. M. TI Single-active-electron ionization of C-60 in intense laser pulses to high charge states SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID S-MATRIX THEORY; RARE-GAS ATOMS; MULTIPHOTON IONIZATION; TUNNEL IONIZATION; ELECTROMAGNETIC-FIELD; COMPLEX ATOMS; MOLECULES; FRAGMENTATION; HELIUM; LIMIT AB Sequential ionization of the C-60 fullerene to high charge states in ultrashort intense laser pulses is investigated within the strong-field S-matrix approach. Ion yields are calculated and saturation intensities are determined for a broad range of laser wavelengths between 395 and 1800 nm at different pulse lengths. Comparisons of the S-matrix predictions for the saturation intensities with recent experimental data are in an overall satisfactory agreement, indicating that saturation of ionization of this complex molecule can be well described using the single-active-electron approach. The analysis of the results shows that the contributions from the h(u)-highest occupied molecular orbital to the ion yields dominate as compared to those from the inner valence shells h(g) and g(g). Finally, it is demonstrated that the suppression of ionization of C-60 and its ions, as observed in experiments, can be interpreted within the present theory as due to the finite cage size of the fullerenes and a multi-slit-like interference effect between partial waves emitted from the different nuclei of the fullerenes. (c) 2007 American Institute of Physics. C1 Tech Univ Dresden, Inst Phys Chem & Elektrochem, D-01062 Dresden, Germany. Max Planck Inst Phys Komplexer Syst, D-01187 Dresden, Germany. Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Jaron-Becker, A (reprint author), Tech Univ Dresden, Inst Phys Chem & Elektrochem, D-01062 Dresden, Germany. RI Becker, Andreas/K-4402-2013; Jaron-Becker, Agnieszka/C-1227-2014 OI Jaron-Becker, Agnieszka/0000-0003-2339-8544 NR 57 TC 9 Z9 9 U1 1 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 MAR 28 PY 2007 VL 126 IS 12 AR 124310 DI 10.1063/1.2712844 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 151VB UT WOS:000245317800027 PM 17411126 ER PT J AU O'Dea, A Jackson, JBC Fortunato, H Smith, JT D'Croz, L Johnson, KG Todd, JA AF O'Dea, Aaron Jackson, Jeremy B. C. Fortunato, Helena Smith, J. Travis D'Croz, Luis Johnson, Kenneth G. Todd, Jonathan A. TI Environmental change preceded Caribbean extinction by 2 million years SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Isthmus of Panama; paleoenvironments; time-lag; macroevolution; paleocommunities ID DEL-TORO ARCHIPELAGO; PANAMA; EVOLUTION; ECOSYSTEMS; ECOLOGY; CLOSURE; OCEAN; CIRCULATION; NUTRIENTS; ATLANTIC AB Paleontologists typically treat major episodes of extinction as single and distinct events in which a major environmental perturbation results in a synchronous evolutionary response. Alternatively, the causes of biotic change may be multifaceted and extinction may lag behind the changes ultimately responsible because of nonlinear ecological dynamics. We examined these alternatives for the major episode of Caribbean extinction 2 million years ago (Ma). Isolation of the Caribbean from the Eastern Pacific by uplift of the Panamanian Isthmus was associated with synchronous changes in Caribbean near shore environments and community composition between 4.25 and 3.45 Ma. Seasonal fluctuations in Caribbean seawater temperature decreased 3-fold, carbonate deposition increased, and there was a striking, albeit patchy, shift in dominance of benthic ecosystems from heterotrophic mollusks to mixotrophic reef corals and calcareous algae. All of these changes correspond well with a simple model of decreased upwelling and collapse in planktonic productivity associated with the final stages of the closure of the isthmian barrier. However, extinction rates of mollusks and corals did not increase until 3-2 Ma and sharply peaked between 2 and 1 Ma, even though extinction overwhelmingly affected taxa commonly associated with high productivity. This time lag suggests that something other than environmental change per se was involved in extinction that does not occur as a single event. Understanding cause and effect will require more taxonomically refined analysis of the changing abundance and distribution patterns of different ecological guilds in the 2 million years leading up to the relatively sudden peak in extinction. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Nat Hist Museum, London SW7 5BD, England. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Panama. EM odeaa@si.edu RI O'Dea, Aaron/D-4114-2011; OI Todd, Jonathan/0000-0002-0433-1611 NR 43 TC 99 Z9 106 U1 3 U2 17 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 27 PY 2007 VL 104 IS 13 BP 5501 EP 5506 DI 10.1073/pnas.0610947104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 152AE UT WOS:000245331700045 PM 17369359 ER PT J AU Blum, JC Chang, AL Liljesthrom, M Schenk, ME Steinberg, MK Ruiz, GM AF Blum, Julia C. Chang, Andrew L. Liljesthrom, Marcela Schenk, Michelle E. Steinberg, Mia K. Ruiz, Gregory M. TI The non-native solitary ascidian Ciona intestinalis (L.) depresses species richness SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT 1st International Invasive Sea Squirt Conference CY APR 21-22, 2005 CL Woods Hole Oceanog Inst, Wood Hole, MA HO Woods Hole Oceanog Inst DE ascidian; Ciona; fouling community; impact; invasion; nonindigenous; species richness ID NEW-ENGLAND; COMMUNITY; DIVERSITY; IMPACT; INVERTEBRATES; COMPLEXITY; INVASION; DEFENSE; HARBORS; CHILE AB Non-native ascidians are a dominant feature of many sessile marine communities throughout the world and may have negative effects on species diversity. We tested effects of the non-native Ciona intestinalis on the sessile invertebrate community in San Francisco Bay, where it occurs in dense aggregations. In particular, we compared species richness between PVC panels from which C. intestinalis were experimentally removed to panels with naturally dense C. intestinalis growth, using fouling panels of four sizes (between 49 cm(2) and 1177 cm(2)) to measure the effect of C. intestinalis recruitment on species-area relationships. We initially deployed 120 fouling panels (30 of each size) at a site known to have dense populations of C. intestinalis, assigning these to three different treatments: (1) Experimental removal, whereby new recruits of C. intestinalis were removed on a weekly basis, pulling panels out of the water for a short time period to do so; (2) Manipulated control, whereby panels were removed from the water each week (as in the experimental removal) but without C. intestinalis removal; and (3) Unmanipulated control, which remained in the water throughout the experiment. After 4 months, all of the panels were collected and analyzed to estimate species richness and relative abundance (percent cover) of sessile invertebrates and of C. intestinalis. Across all panels, species richness was negatively correlated with C. intestinalis abundance. The removal of C. intestinalis produced communities with significantly higher species richness than the controls. The overall species composition of treated and control panels was also distinctly different, with many species occurring more often in the absence of C. intestinalis, while others occurred more often on C. intestinalis-dominated panels. These data suggest that C. intestinalis both depress local species diversity and alter community assembly processes to fundamentally change sessile community composition. (c) 2006 Elsevier B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Blum, JC (reprint author), Univ Calif Davis, Sect Evolut & Ecol, 1 Shields Ave, Davis, CA 95616 USA. EM jcblum@ucdavis.edu RI Chang, Andrew/J-8058-2016; OI Chang, Andrew/0000-0002-7870-285X; Ruiz, Gregory/0000-0003-2499-441X NR 47 TC 66 Z9 72 U1 2 U2 45 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 MAR 26 PY 2007 VL 342 IS 1 SI SI BP 5 EP 14 DI 10.1016/j.jembe.2006.10.010 PG 10 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 142SE UT WOS:000244669400003 ER PT J AU Altman, S Whitlatch, RB AF Altman, Safra Whitlatch, Robert B. TI Effects of small-scale disturbance on invasion success in marine communities SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT 1st International Invasive Sea Squirt Conference CY APR 21-22, 2005 CL Woods Hole Oceanog Inst, Wood Hole, MA HO Woods Hole Oceanog Inst DE ascidians; bioinvasion; bryozoans; disturbance; fouling community; Long Island Sound ID BIOLOGICAL INVASIONS; SPECIES-DIVERSITY; RESIDENT ADULTS; INVASIBILITY; COMPETITION; SETTLEMENT; CALIFORNIA; ESTABLISHMENT; ENVIRONMENTS; CONSERVATION AB Introductions of non-indigenous species have resulted in many ecological problems including the reduction of biodiversity, decline of commercially important species and alteration of ecosystems. The link between disturbance and invasion potential has rarely been studied in the marine environment where dominance hierarchies, dynamics of larval supply, and resource acquisition may differ greatly from terrestrial systems. In this study, hard substrate marine communities in Long Island Sound, USA were used to assess the effect of disturbance on resident species and recent invaders, ascidian growth form (i.e. colonial and solitary growth form), and the dominant species-specific responses within the community. Community age was an additional factor considered through manipulation of 5-wk old assemblages and 1-yr old assemblages. Disturbance treatments, exposing primary substrate, were characterized by frequency (single, biweekly, monthly) and magnitude (20%, 48%, 80%) of disturbance. In communities of different ages, disturbance frequency had a significant positive effect on space occupation of recent invaders and a significant negative effect on resident species. In the 5-wk community, magnitude of disturbance also had a significant effect. Disturbance also had a significant effect on ascidian growth form; colonial species occupied more primary space than controls in response to increased disturbance frequency and magnitude. In contrast, solitary species occupied significantly less space than controls. Species-specific responses were similar regardless of community age. The non-native colonial ascidian Diplosoma listerianum responded positively to increased disturbance frequency and magnitude, and occupied more primary space in treatments than in controls. The resident solitary ascidian Molgula manhattensis responded negatively to increased disturbance frequency and magnitude, and occupied less primary space in treatments than in controls. Small-scale biological disturbances, by creating space, may facilitate the success of invasive species and colonial organisms in the development of subtidal hard substrate communities. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. RP Altman, S (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM altmans@si.edu NR 69 TC 43 Z9 46 U1 1 U2 29 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 MAR 26 PY 2007 VL 342 IS 1 SI SI BP 15 EP 29 DI 10.1016/j.jembe.2006.10.011 PG 15 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 142SE UT WOS:000244669400004 ER PT J AU Osman, RW Whitlatch, RB AF Osman, Richard W. Whitlatch, Robert B. TI Variation in the ability of Didemnum sp to invade established communities SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT 1st International Invasive Sea Squirt Conference CY APR 21-22, 2005 CL Woods Hole Oceanog Inst, Woods Hole, MA HO Woods Hole Oceanog Inst DE ascidians; Didemnum; epifauna; fouling; invasion; Long Island Sound; Southern New England; temperature ID BIOLOGICAL INVASIONS; MARINE ECOSYSTEM; CONSEQUENCES; RESISTANCE; PREDATION; PATTERN; OCEAN AB Over the past 30 years southern New England, USA has been invaded by several species of ascidians, including Botrylloides violaceus, Diplosoma listerianum, Styela clava, and Ascidiella aspersa. These species have become dominate in coastal embayments and marinas but are usually absent from more open water coastal areas. A colonial ascidian, Didemnum sp. has invaded southern New England during the past 10 years and we first observed this species in eastern Long Island Sound in 2000. It has become the dominant at several field sites while remaining in low abundance at others. We conducted an experiment at two places, a protected marina and an open coast site, to examine its ability to compete with the established fouling community. Small colonies of Didemnum were transplanted onto panels with communities that varied in age from one to four weeks old and these treatments along with controls with only Didemnum were exposed at both sites. In most treatments Didemnum became a dominant species in the communities at both sites but it reached higher abundances at the open coast site. Potential causes of the observed differences are predation on other species of ascidians at the open coast site reducing recruitment of these species and competition, lower tolerance for elevated temperatures at the marina site, or other environmental parameters that might affect growth rates. (c) 2006 Published by Elsevier B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. RP Osman, RW (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM osmanr@si.edu NR 24 TC 45 Z9 49 U1 0 U2 24 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 MAR 26 PY 2007 VL 342 IS 1 BP 40 EP 53 DI 10.1016/j.jembe.2006.10.013 PG 14 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 142SE UT WOS:000244669400006 ER PT J AU Bullard, SG Lambert, G Carman, MR Byrnes, J Whitlatch, RB Ruiz, G Miller, RJ Harris, L Valentine, PC Collie, JS Pederson, J McNaught, DC Cohen, AN Asch, RG Dijkstra, J Heinonen, K AF Bullard, S. G. Lambert, G. Carman, M. R. Byrnes, J. Whitlatch, R. B. Ruiz, G. Miller, R. J. Harris, L. Valentine, P. C. Collie, J. S. Pederson, J. McNaught, D. C. Cohen, A. N. Asch, R. G. Dijkstra, J. Heinonen, K. TI The colonial ascidian Didemnum sp A: Current distribution, basic biology and potential threat to marine communities of the northeast and west coasts of North America SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT 1st International Invasive Sea Squirt Conference CY APR 21-22, 2005 CL Woods Hole Oceanog Inst, Woods Hole, MA HO Woods Hole Oceanog Inst DE ascidian; Didemnum; distribution; fouling; Georges Bank; invasive species; nonindigenous; Stellwagen Bank; Tillies Bank; tunicate ID PYURA-PRAEPUTIALIS; CHEMICAL DEFENSES; SESSILE ORGANISMS; TOMIOKA BAY; RECRUITMENT; HARBORS; ADULT; JAPAN; REEFS; SHORE AB Didemnum sp. A is a colonial ascidian with rapidly expanding populations on the east and west coasts of North America. The origin of Didemum sp. A is unknown. Populations were first observed on the northeast coast of the U.S. in the late 1980s and on the west coast during the 1990s. It is currently undergoing a massive population explosion and is now a dominant member of many subtidal communities on both coasts. To determine Didemnum sp. A's current distribution, we conducted surveys from Maine to Virginia on the east coast and from British Columbia to southern California on the west coast of the U.S. between 1998 and 2005. In nearshore locations Didemnum sp. A currently ranges from Eastport, Maine to Shinnecock Bay, New York on the east coast. On the west coast it has been recorded from Humboldt Bay to Port San Luis in California, several sites in Puget Sound, Washington, including a heavily fouled mussel culture facility, and several sites in southwestern British Columbia on and adjacent to oyster and mussel farms. The species also occurs at deeper subtidal sites (up to 81 m) off New England, including Georges, Stellwagen and Tillies Banks. On Georges Bank numerous sites within a 230 km(2) area are 50-90% covered by Didemnum sp. A; large colonies cement the pebble gravel into nearly solid mats that may smother infaunal organisms. These observations suggest that Didemnum sp. A has the potential to alter marine communities and affect economically important activities such as fishing and aquaculture. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Hartford, Hillyer Coll, Hartford, CT 06117 USA. Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA. Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Massachusetts, Dept Biol, Boston, MA 02125 USA. Univ New Hampshire, Dept Zool, Durham, NH 03824 USA. US Geol Survey, Coastal & Marine Geol Program, Woods Hole, MA 02543 USA. Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. MIT, Sea Grant Coll Program, MITSG Ctr Coastal Resources, Cambridge, MA 02139 USA. Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. San Francisco Estuary Inst, Oakland, CA 94621 USA. Univ Connecticut, Natl Undersea Res Ctr, Groton, CT 06340 USA. RP Bullard, SG (reprint author), Univ Hartford, Hillyer Coll, 200 Bloomfield Ave, Hartford, CT 06117 USA. EM bullard@hartford.edu OI Byrnes, Jarrett/0000-0002-9791-9472; Ruiz, Gregory/0000-0003-2499-441X NR 34 TC 88 Z9 94 U1 2 U2 37 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 MAR 26 PY 2007 VL 342 IS 1 BP 99 EP 108 DI 10.1016/j.jembe.2006.10.020 PG 10 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 142SE UT WOS:000244669400013 ER PT J AU McCarthy, A Osman, RW Whitlatch, RB AF McCarthy, Anna Osman, Richard W. Whitlatch, Robert B. TI Effects of temperature on growth rates of colonial ascidians: A comparison of Didemnum sp to Botryllus schlosseri and Botrylloides violaceus SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article; Proceedings Paper CT 1st International Invasive Sea Squirt Conference CY APR 21-22, 2005 CL Woods Hole Oceanog Inst, Woods Hole, MA HO Woods Hole Oceanog Inst DE Botrylloides violaceus; Botryllus schlosseri; Didemnum; fouling; invasion; temperature C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Whitman Coll, Dept Biol, Walla Walla, WA 99362 USA. Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. RP Osman, RW (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM osmanr@si.edu NR 8 TC 28 Z9 28 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD MAR 26 PY 2007 VL 342 IS 1 BP 172 EP 174 DI 10.1016/j.jembe.2006.10.036 PG 3 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 142SE UT WOS:000244669400023 ER PT J AU Day, JW Boesch, DF Clairain, EJ Kemp, GP Laska, SB Mitsch, WJ Orth, K Mashriqui, H Reed, DJ Shabman, L Simenstad, CA Streever, BJ Twilley, RR Watson, CC Wells, JT Whigham, DF AF Day, John W., Jr. Boesch, Donald F. Clairain, Ellis J. Kemp, G. Paul Laska, Shirley B. Mitsch, William J. Orth, Kenneth Mashriqui, Hassan Reed, Denise J. Shabman, Leonard Simenstad, Charles A. Streever, Bill J. Twilley, Robert R. Watson, Chester C. Wells, John T. Whigham, Dennis F. TI Restoration of the Mississippi Delta: Lessons from Hurricanes Katrina and Rita SO SCIENCE LA English DT Review ID LOUISIANA COAST; WETLAND LOSS; RIVER DELTA; LAND LOSS; VEGETATION; BASIN; PLAIN; USA; SEDIMENTATION; INTENSITY AB Hurricanes Katrina and Rita showed the vulnerability of coastal communities and how human activities that caused deterioration of the Mississippi Deltaic Plain (MDP) exacerbated this vulnerability. The MDP formed by dynamic interactions between river and coast at various temporal and spatial scales, and human activity has reduced these interactions at all scales. Restoration efforts aim to re-establish this dynamic interaction, with emphasis on reconnecting the river to the deltaic plain. Science must guide MDP restoration, which will provide insights into delta restoration elsewhere and generally into coasts facing climate change in times of resource scarcity. C1 Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. Univ Maryland, Ctr Environm Sci, Cambridge, MD 21613 USA. USA, Corps Engineers, Engineer Res & Dev Ctr, Vicksburg, MS 39180 USA. Louisiana State Univ, Hurricane Ctr, Baton Rouge, LA 70803 USA. Univ New Orleans, Dept Sociol, New Orleans, LA 70148 USA. Ohio State Univ, Columbus, OH 43202 USA. USA, Inst Water Resources, Corps Engineers, Alexandria, VA 22315 USA. Louisiana State Univ, Dept Civil & Environm Engn, Baton Rouge, LA 70803 USA. Univ New Orleans, Dept Geol & Geophys, New Orleans, LA 70148 USA. Resources Future Inc, Washington, DC 20036 USA. Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98015 USA. BP Explorat Alaska, Anchorage, AK 99519 USA. Colorado State Univ, Engn Res Ctr, Ft Collins, CO 80523 USA. Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Day, JW (reprint author), Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. EM johnday@lsu.edu OI Whigham, Dennis/0000-0003-1488-820X NR 57 TC 278 Z9 283 U1 34 U2 222 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 23 PY 2007 VL 315 IS 5819 BP 1679 EP 1684 DI 10.1126/science.1137030 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 148WA UT WOS:000245106900029 PM 17379799 ER PT J AU Novotny, V Drozd, P Miller, SE Kulfan, M Janda, M Basset, Y Weiblen, GD AF Novotny, Vojtech Drozd, Pavel Miller, Scott E. Kulfan, Miroslav Janda, Milan Basset, Yves Weiblen, George D. TI Response to comment on "Why are there so many species of herbivorous insects in tropical rainforests?" SO SCIENCE LA English DT Editorial Material ID PAPUA-NEW-GUINEA; COMMUNITIES; PLANTS C1 Acad Sci Czech Republic, Inst Entomol, Ceske Budejovice 37005, Czech Republic. Univ S Bohemia, Dept Zool, Ceske Budejovice 37005, Czech Republic. Univ Ostrava, Dept Biol, Ostrava 71000, Czech Republic. Smithsonian Inst, Washington, DC 20013 USA. Comenius Univ, Dept Zool, Bratislava 84215, Slovakia. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Minnesota, Dept Plant Biol, Ctr Biol Sci, St Paul, MN 55108 USA. RP Novotny, V (reprint author), Acad Sci Czech Republic, Inst Entomol, Bramsovska 31, Ceske Budejovice 37005, Czech Republic. EM novotny@entu.cas.cz RI Drozd, Pavel/J-3943-2013; Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; Janda, Milan/H-7216-2014; OI Drozd, Pavel/0000-0002-4602-8856; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 14 TC 4 Z9 4 U1 1 U2 22 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 23 PY 2007 VL 315 IS 5819 DI 10.1126/science.1139702 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 148WA UT WOS:000245106900019 ER PT J AU Mukhopadhyay, B AF Mukhopadhyay, Banibrata TI Gravity-induced neutrino-antineutrino oscillation: CPT and lepton number non-conservation under gravity SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID EQUIVALENCE PRINCIPLE; ASYMMETRY; VIOLATION; ACCRETION; FIELDS; TESTS AB We introduce a new effect in the neutrino oscillation phase which shows that the neutrino-antineutrino oscillation is possible under gravity even if the rest masses of the corresponding eigenstates are the same. This is due to CPT violation, and is possible to demonstrate if the neutrino mass eigenstates are expressed as a combination of neutrino and antineutrino eigenstates, as of the neutral kaon system, with the plausible breaking of lepton number conservation. For Majorana neutrinos, this oscillation is expected to significantly affect the inner edge of neutrino-dominated accretion discs around compact objects by influencing the neutrino sphere which controls the accretion dynamics, and then the related type-II supernova evolution and the r-process nucleosynthesis. On the other hand, in the early universe, in the presence of various lepton number violating processes, this oscillation, we argue, might have led to neutrino asymmetry which resulted in baryogenesis from the B-L symmetry by electro-weak sphaleron processes. C1 Indian Inst Sci, Dept Phys, Bangalore 560012, Karnataka, India. Harvard Smithsonian Ctr Astrophys, Div Theory, Cambridge, MA 02138 USA. RP Mukhopadhyay, B (reprint author), Indian Inst Sci, Dept Phys, Bangalore 560012, Karnataka, India. EM bm@physics.iisc.ernet.in NR 35 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAR 21 PY 2007 VL 24 IS 6 BP 1433 EP 1442 DI 10.1088/0264-9381/24/6/004 PG 10 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 145KU UT WOS:000244864600004 ER PT J AU Wright, SA Larkin, JE Barczys, M Erb, DK Iserlohe, C Krabbe, A Law, DR McElwain, MW Quirrenbach, A Steidel, CC Weiss, J AF Wright, S. A. Larkin, J. E. Barczys, M. Erb, D. K. Iserlohe, C. Krabbe, A. Law, D. R. McElwain, M. W. Quirrenbach, A. Steidel, C. C. Weiss, J. TI Integral field spectroscopy of a candidate disk galaxy at z similar to 1.5 using laser guide star adaptive optics SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : high-redshift; galaxies : kinematics and dynamics; infrared : galaxies ID HIGH-REDSHIFT GALAXIES; LYMAN BREAK GALAXIES; FORMING GALAXIES; ROTATION CURVES; KINEMATICS; KECK; PARAMETERS; EVOLUTION; SELECTION; EMISSION AB We present 0.1" resolution near-infrared integral field spectroscopy of H alpha in a z = 4781 star- forming galaxy, Q2343 - BM133. These observations were obtained with the OH Suppressing Infra- Red Imaging Spectrograph ( OSIRIS) using the W. M. Keck Observatory laser guide star adaptive optics ( LGS AO) system. H alpha emission is resolved over a 0: 800( 6: 8kpc); 0: 500( 4: 3 kpc) region with a 0.1" spatial resolution. We find a global flux of 4: 2 +/- 0: 6; 10(-16) ergs s(-1) cm(-2), and detect a spatially resolved velocity gradient of similar to 134 km s(-1) across the galaxy and a global velocity dispersion of 73 +/- 9 km s(-1). An upper limit of [N II]/ H alpha less than or similar to 0:12 is inferred, which implies that this galaxy is not dominated by an active galactic nucleus and has a metallicity at or below 1/2 solar metallicity. We derive a star formation rate ( SFR) of 47 +/- 6 M-circle dot yr(-1) and a dereddened SFR of 66 +/- 9 M-circle dot yr(-1). Two- dimensional kinematics for Q2343 - BM133 fit well with an inclined diskmodel, with which we estimate an enclosed mass of 4: 3; 10(9) M-circle dot within 5.5 kpc. A possible merger scenario is also presented, and cannot be fully ruled out. We derive a virial mass of 1: 1; 10(10) M-circle dot for a disk geometry, using the observed velocity dispersion. We propose that Q2343 - BM133 is currently at an early stage of disk formation at a look- back time of 9.3 Gyr. C1 Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cologne, Inst Phys, D-5000 Cologne 41, Germany. ZAH Landessternwarte, Koenigstuhl, Heidelberg, Germany. RP Wright, SA (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. EM saw@astro.ucla.edu; larkin@astro.ucla.edu; barczysm@astro.ucla.edu; derb@cfa.harvard.edu; iserlohe@ph1.unikoeln.de; krabbe@ph1.uni-koeln.de; drlaw@astro.caltech.edu; mcelwain@astro.ucla.edu; a.quirrenbach@lsw.uniheidelberg.de; ccs@astro.caltech.edu; weiss@astro.ucla.edu RI McElwain, Michael/D-3607-2012 OI McElwain, Michael/0000-0003-0241-8956 NR 38 TC 58 Z9 58 U1 0 U2 7 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 2007 VL 658 IS 1 BP 78 EP 84 DI 10.1086/511632 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IY UT WOS:000244928900008 ER PT J AU O'Sullivan, E Vrtilek, JM Harris, DE Ponman, TJ AF O'Sullivan, E. Vrtilek, J. M. Harris, D. E. Ponman, T. J. TI On the anomalous temperature distribution of the intergalactic medium in the NGC 3411 group of galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (USGC S152); galaxies : individual (NGC 3411); radio continuum : galaxies; X-rays : galaxies : clusters ID XMM-NEWTON OBSERVATION; X-RAY; THERMAL CONDUCTION; PERSEUS CLUSTER; CHANDRA OBSERVATIONS; ELLIPTICAL GALAXIES; INTRACLUSTER MEDIUM; METAL ABUNDANCES; VIRGO CLUSTER; SKY SURVEY AB We present XMM-Newton, Chandra, and VLA observations of the USGC S152 group and its central elliptical NGC 3411. Imaging of the group X-ray halo suggests that it is relaxed with little apparent structure. We investigate the temperature and metal abundance structure of the group halo and find that while the abundance distribution is fairly typical, the temperature profile is highly unusual, showing a hot inner core surrounded by a cool shell of gas with a radius of similar to 20 - 40 kpc, at the center of the larger group halo. Spectral mapping confirms an irregular ring of gas similar to 0.15 keV cooler than its surroundings. We estimate the total mass, entropy, and cooling time profiles within similar to 200 kpc, and find that the cool shell contains similar to 9 x 10(9) M(circle dot) of gas. VLA observations at 1.4, 5, and 8 GHz reveal a relatively weak nuclear radio source, with a core radio luminosity L(R) 2.7 x 10(38) ergs s(-1) and a diffuse component extended on scales of a few arcseconds (or more). A lack of evidence for activity at optical or X-ray wavelengths supports the conclusion that the central black hole is currently in a quiescent state. We discuss possible mechanisms for the formation of temperature features observed in the halo, including a previous period of AGN activity, and settling of material stripped from the halo of one of the other group member galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Birmingham, Sch Phys & Astron, Birmingham, W Midlands, England. 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; harris@head.cfa.harvard.edu; tjp@star.sr.bham.ac.uk OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 72 TC 27 Z9 27 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2007 VL 658 IS 1 BP 299 EP 313 DI 10.1086/511778 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IY UT WOS:000244928900024 ER PT J AU Ho, LC Keto, E AF Ho, Luis C. Keto, Eric TI The mid-infrared fine-structure lines of neon as an indicator of star formation rate in galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; galaxies : starburst; infrared : galaxies ID H-II REGIONS; HII-REGIONS; STARBURST GALAXIES; DWARF GALAXIES; METALLICITY; EXCITATION; EMISSION; ABUNDANCES; EVOLUTION; RECOMBINATION AB The fine-structure lines of singly ([Ne II] 12.8 mu m) and doubly ([Ne III] 15.6 mu m) ionized neon are among the most prominent features in the mid-infrared spectra of star-forming regions and have the potential to be a powerful new indicator of the star formation rate in galaxies. Using a sample of star-forming galaxies with measurements of the fine-structure lines available from the literature, we show that the sum of the [Ne II] and [Ne III] luminosities obeys a tight, linear correlation with the total infrared luminosity over 5 orders of magnitude in luminosity. We discuss the formation of the lines and their relation with the Lyman continuum luminosity. A simple calibration between star formation rate and the [Ne II]+[Ne III] luminosity is presented. C1 Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ho, LC (reprint author), Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. NR 32 TC 62 Z9 61 U1 1 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 MAR 20 PY 2007 VL 658 IS 1 BP 314 EP 318 DI 10.1086/511260 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IY UT WOS:000244928900025 ER PT J AU Lane, BF Sokoloski, JL Barry, RK Traub, WA Retter, A Muterspaugh, MW Thompson, RR Eisner, JA Serabyn, E Mennesson, B AF Lane, B. F. Sokoloski, J. L. Barry, R. K. Traub, W. A. Retter, A. Muterspaugh, M. W. Thompson, R. R. Eisner, J. A. Serabyn, E. Mennesson, B. TI Interferometric observations of RS Ophiuchi and the origin of the near-infrared emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE techniques : interferometric ID PALOMAR TESTBED INTERFEROMETER; 2006 OUTBURST; NOVA OUTBURSTS; OPTICALLY THICK; RECURRENT NOVAE; IA SUPERNOVAE; SYSTEMS; PHASE; MODELS; STARS AB We report observations of the recurrent nova RS Oph using long-baseline near-IR interferometry. We are able to resolve emission from the nova for several weeks after the 2006 February outburst. The near-IR source initially expands to a size of similar to 5 mas. However, beginning around day 10, the IR source appears to begin to shrink, reaching similar to 2 mas by day 100. We combine our measured angular diameters with previously available interferometric and photometric data to derive an emission measure for the source, and hence are able to determine the mass-loss rate of the nova in the days following the outburst. C1 MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Smithsonian Astrophys Observ, Cambridge, MA USA. Johns Hopkins Univ, Baltimore, MD USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Jet Propuls Lab, Pasadena, CA USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. RP Lane, BF (reprint author), MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM blane@mit.edu; jsokolos@cfa.harvard.edu; retter@astro.psu.edu; thompson@ipac.caltech.edu NR 37 TC 21 Z9 21 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 MAR 20 PY 2007 VL 658 IS 1 BP 520 EP 524 DI 10.1086/511414 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IY UT WOS:000244928900044 ER PT J AU Phan-Bao, N Osten, RA Lim, J Martin, EL Ho, PTP AF Phan-Bao, Ngoc Osten, Rachel A. Lim, Jeremy Martin, Eduardo L. Ho, Paul T. P. TI Discovery of radio emission from the tight M8 binary LP 349-25 SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum : stars; stars : activity; stars : coronae; stars : individual (LP 349-25); stars : low mass; brown dwarfs ID EPSILON-INDI-BAB; X-RAY-EMISSION; LATE M-DWARF; BROWN DWARFS; MAIN-SEQUENCE; LARGE-SCALE; MAGNETIC-FIELDS; STARS; SEARCH; TVLM-513-46546 AB We present radio observations of eight ultracool dwarfs with a narrow spectral type range (M8-M9.5) using the Very Large Array at 8.5 GHz. Only the tight M8 binary LP 349 - 25 was detected. LP 349 - 25 is the tenth ultracool dwarf system detected in radio wavelengths and its trigonometric parallax pi = 67.6 mas, recently measured by Gatewood and coworkers, makes it the furthest ultracool system detected by the Very Large Array to date, and the most radio luminous outside of obvious flaring activity or variability. With a separation of only 1.8 AU, masses of the components of LP 349 - 25 can be measured precisely without any theoretical assumptions, allowing us to clarify their fully convective status and hence the kind of magnetic dynamo in these components, which may play an important role in explaining our detection of radio emissions from these objects. This also makes LP 349 - 25 an excellent target for further studies with better constraints on the correlations between X-ray, and radio emission and stellar parameters such as mass, age, temperature, and luminosity in ultracool dwarfs. C1 Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Phan-Bao, N (reprint author), Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. EM pngoc@physics.ucf.edu; rosten@milkyway.gsfc.nasa.gov; jlim@asiaa.sinica.edu.tw; ege@iac.es; ho@cfa.harvard.edu NR 32 TC 27 Z9 27 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 MAR 20 PY 2007 VL 658 IS 1 BP 553 EP 556 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IY UT WOS:000244928900047 ER PT J AU Kaltenegger, L Traub, WA Jucks, KW AF Kaltenegger, Lisa Traub, Wesley A. Jucks, Kenneth W. TI Spectral evolution of an Earth-like planet SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; planetary systems ID EXTRASOLAR TERRESTRIAL PLANETS; PROTEROZOIC OCEAN CHEMISTRY; ARCHEAN SULFUR CYCLE; ATMOSPHERIC OXYGEN; THERMAL EMISSION; LIFE; DARWIN; STARS; MODEL; BIOSIGNATURES AB We have developed a characterization of the geological evolution of the Earth's atmosphere and surface in order to model the observable spectra of an Earth-like planet through its geological history. These calculations are designed to guide the interpretation of an observed spectrum of such a planet by future instruments that will characterize exoplanets. Our models focus on planetary environmental characteristics whose resultant spectral features can be used to imply habitability or the presence of life. These features are generated by H2O, CO2, CH4, O-2, O-3, N2O, and vegetation- like surface albedos. We chose six geological epochs to characterize. These epochs exhibit a wide range in abundance for these molecules, ranging from a CO2-rich early atmosphere, to a CO2/CH4-rich atmosphere around 2 billion years ago, to a present-day atmosphere. We analyzed the spectra to quantify the strength of each important spectral feature in both the visible and thermal infrared spectral regions, and the resolutions required to optimally detect the features for each epoch. We find a wide range of spectral resolutions required for observing the different features. For example, H2O and O-3 can be observed with relatively low resolution, while O-2 and N2O require higher resolution. We also find that the inclusion of clouds in our models significantly affects both the strengths of all spectral features and the resolutions required to observe all these. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Jet Propuls Lab, Pasadena, CA USA. RP Kaltenegger, L (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM lkaltenegger@cfa.harvard.edu NR 65 TC 121 Z9 123 U1 3 U2 26 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 2007 VL 658 IS 1 BP 598 EP 616 DI 10.1086/510996 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IY UT WOS:000244928900052 ER PT J AU Patel, NA Curiel, S Zhang, QZ Sridharan, TK Ho, PTP Torrelles, JM AF Patel, Nimesh A. Curiel, Salvador Zhang, Qizhou Sridharan, T. K. Ho, Paul T. P. Torrelles, Jose M. TI Submillimeter array observations of 321 GHz water maser emission in Cepheus A SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Cepheus A); ISM : jets and outflows; masers; stars : formation ID STAR-FORMING REGION; H2O MASERS; PROPER MOTION; PROTOSTAR; HW2; KINEMATICS; DISCOVERY; EJECTION; OUTFLOW; DISK AB Using the Submillimeter Array (SMA) we have imaged for the first time the 321.226 GHz, 10(29)-9(36) ortho-H2O maser emission. This is also the first detection of this line in the Cepheus A high-mass star-forming region. The 22.235 GHz, 6(16)-5(23) water masers were also observed with the Very Large Array 43 days following the SMA observations. Three of the nine detected submillimeter maser spots are associated with the centimeter masers spatially as well as kinematically, while there are 36 22 GHz maser spots without corresponding submillimeter masers. In the HW2 source, both the 321 and 22 GHz masers occur within the region of similar to 1 '', which includes the disk-jet system, but the position angles of the roughly linear structures traced by the masers indicate that the 321 GHz masers are along the jet while the 22 GHz masers are perpendicular to it. We interpret the submillimeter masers in Cepheus A to be tracing significantly hotter regions (600-2000 K) than the centimeter masers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Univ Barcelona, Fac Fis, Inst Ciencias Espacio, CSIC,IEEC, E-08028 Barcelona, Spain. RP Patel, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM npatel@cfa.harvard.edu; scuriel@astroscu.unam.mx; qzhang@cfa.harvard.edu; tksridha@cfa.harvard.edu; pho@cfa.harvard.edu; torrelle@europa.ieec.fcr.es OI Torrelles, Jose Maria/0000-0002-6896-6085; Zhang, Qizhou/0000-0003-2384-6589 NR 34 TC 11 Z9 11 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 MAR 20 PY 2007 VL 658 IS 1 BP L55 EP L58 DI 10.1086/513508 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146JD UT WOS:000244929400014 ER PT J AU Miller, SE AF Miller, Scott E. TI DNA barcoding and the renaissance of taxonomy SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID BIODIVERSITY C1 Smithsonian Inst, Washington, DC 20013 USA. RP Miller, SE (reprint author), Smithsonian Inst, Washington, DC 20013 USA. EM millers@si.edu OI Miller, Scott/0000-0002-4138-1378 NR 17 TC 111 Z9 140 U1 2 U2 20 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 20 PY 2007 VL 104 IS 12 BP 4775 EP 4776 DI 10.1073/pnas.0700466104 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 150YY UT WOS:000245256700002 PM 17363473 ER PT J AU Gilbert, GS Webb, CO AF Gilbert, Gregory S. Webb, Campbell O. TI Phylogenetic signal in plant pathogen-host range SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE fungal pathogen; plant disease ecology; tropical forest; plant quarantine; host specificity ID SEEDLING MORTALITY; TROPICAL FORESTS; RAIN-FOREST; TREE; DIVERSITY; PATTERNS; DISEASE; SPECIFICITY; HERBIVORES; INVASIONS AB What determines which plant species are susceptible to a given plant pathogen is poorly understood. Experimental inoculations with fungal pathogens of plant leaves in a tropical rain forest show that most fungal pathogens are polyphagous but that most plant species in a local community are resistant to any given pathogen. The likelihood that a pathogen can infect two plant species decreases continuously with phylogenetic distance between the plants, even to ancient evolutionary distances. This phylogenetic signal in host range allows us to predict the likely host range of plant pathogens in a local community, providing an important tool for plant ecology, design of agronomic systems, quarantine regulations in international trade, and risk analysis of biological control agents. In particular, the results suggest that the rate of spread and ecological impacts of a disease through a natural plant community will depend strongly on the phylogenetic structure of the community itself and that current regulatory approaches strongly underestimate the local risks of global movement of plant pathogens or their hosts. C1 Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Panama. Harvard Univ, Arnold Arboretum, Harvard Univ Hebaria, Cambridge, MA 02138 USA. RP Gilbert, GS (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, 1156 High St,405 ISB, Santa Cruz, CA 95064 USA. EM ggilbert@ucsc.edu OI Webb, Campbell/0000-0003-1031-3249 NR 35 TC 234 Z9 244 U1 14 U2 117 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 20 PY 2007 VL 104 IS 12 BP 4979 EP 4983 DI 10.1073/pnas.0607968104 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 150YY UT WOS:000245256700040 PM 17360396 ER PT J AU Carney, KM Hungate, BA Drake, BG Megonigal, JP AF Carney, Karen M. Hungate, Bruce A. Drake, Bert G. Megonigal, J. Patrick TI Altered soil microbial community at elevated CO2 leads to loss of soil carbon SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE carbon cycling; global change; microbes; priming effect ID SCRUB-OAK ECOSYSTEM; ATMOSPHERIC CO2; ENRICHMENT FACE; ORGANIC-MATTER; DECOMPOSITION; RESPONSES; DIOXIDE; BIOMASS; PHOTOSYNTHESIS; GRASSLAND AB Increased carbon storage in ecosystems due to elevated CO2 may help stabilize atmospheric CO2 concentrations and slow global warming. Many field studies have found that elevated CO2 leads to higher carbon assimilation by plants, and others suggest that this can lead to higher carbon storage in soils, the largest and most stable terrestrial carbon pool. Here we show that 6 years of experimental CO2 doubling reduced soil carbon in a scrub-oak ecosystem despite higher plant growth, offsetting approximate to 52% of the additional carbon that had accumulated at elevated CO2 in aboveground and coarse root biomass. The decline in soil carbon was driven by changes in soil microbial composition and activity. Soils exposed to elevated CO2 had higher relative abundances of fungi and higher activities of a soil carbon-degrading enzyme, which led to more rapid rates of soil organic matter degradation than soils exposed to ambient CO2. The isotopic composition of microbial fatty acids confirmed that elevated CO2 increased microbial utilization of soil organic matter. These results show how elevated CO2, by altering soil microbial communities, can cause a potential carbon sink to become a carbon source. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. No Arizona Univ, Environm Res Ctr, Dept Biol Sci & Merriam Powell, Flagstaff, AZ 86011 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM megonigalp@si.edu RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 35 TC 242 Z9 263 U1 27 U2 209 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 20 PY 2007 VL 104 IS 12 BP 4990 EP 4995 DI 10.1073/pnas.0610045104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 150YY UT WOS:000245256700042 PM 17360374 ER PT J AU Wang, YX McElroy, MB Martin, RV Streets, DG Zhang, Q Fu, TM AF Wang, Yuxuan McElroy, Michael B. Martin, Randall V. Streets, David G. Zhang, Qiang Fu, Tung-May TI Seasonal variability of NOx emissions over east China constrained by satellite observations: Implications for combustion and microbial sources SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING EXPERIMENT; TROPOSPHERIC NITROGEN-DIOXIDE; UNITED-STATES; NORTH-AMERICA; OXIDE EMISSIONS; AIR-QUALITY; ART.; GOME; MODEL; AEROSOLS AB Observations of tropospheric column densities of NO2 obtained from the Global Ozone Monitoring Experiment ( GOME) for a 3-year period ( 1997, 1998, and 2000) are used to derive average seasonal variations in surface emissions of NOx from east China ( 100-123 degrees E, 20-42 degrees N). The retrieval allows for zonal variations in the contribution of the stratosphere to the NO2 column and removes a bias of +/- 10% on the seasonality of retrieved columns introduced by cloud screening. The top-down inventory is constructed using an inversion approach with a global 3-D chemical transport model ( GEOS-Chem) and combined subsequently with the a priori inventory to develop an a posteriori inventory. The contribution of background NO2 arising from nonsurface sources ( lightning) and long-range transport of emissions originating outside of east China is accounted for in the inversion. The a posteriori estimate of overall emissions for east China, 4.66 Tg N/yr ( +/- 30% uncertainty), is 33% higher than the a priori value and is shown to improve agreement with surface measurements of nitrate wet deposition and concentrations of NOy observed in China. On the basis of multiple constraints on the spatial and seasonal variations of combustion and microbial processes, the a posteriori inventory is partitioned among emissions from biomass burning, fuel combustion, and microbial activity ( or soil emissions). Emission of NOx from biomass burning in east China is estimated as 0.08 TgN/yr +/- 50% in the a posteriori inventory, increased by about a factor of 2 from the a priori estimate. The resulting a posteriori inventory for fuel combustion ( 3.72 TgN/yr +/- 32%) is about 15% higher than the a priori and exhibits a distinct maximum in winter, in contrast to the weak seasonality indicated in the a priori inventory. The a posteriori value for the microbial source of NOx ( 0.85 TgN/yr +/- 40%) is about a factor of 3 higher than the a priori value, amounting to 23% of combustion sources for east China and significantly higher than a priori value of 7%. The microbial source is unimportant in winter. It peaks in summer, accounting for as much as 43% of the combustion source for that season, and is significant also in spring and fall. This seasonality is attributed to the timing of fertilizer application and to the influence of seasonally variable environmental factors including temperature and precipitation. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Harvard Smithsonian Ctr Astrophys, Atmospher & Mol Phys Div, Cambridge, MA 02138 USA. Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. RP Wang, YX (reprint author), Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. EM wang3@fas.harvard.edu RI Martin, Randall/A-2051-2008; 欧阳, 冰洁/G-2925-2011; Zhang, Qiang/D-9034-2012; Martin, Randall/C-1205-2014; Wang, Yuxuan/C-6902-2014; Chem, GEOS/C-5595-2014; Fu, Tzung-May/N-3418-2015; OI Martin, Randall/0000-0003-2632-8402; Wang, Yuxuan/0000-0002-1649-6974; Streets, David/0000-0002-0223-1350 NR 66 TC 65 Z9 66 U1 5 U2 24 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 16 PY 2007 VL 112 IS D6 AR D06301 DI 10.1029/2006JD007538 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 147QM UT WOS:000245017500006 ER PT J AU Chambers, DP Tamisiea, ME Nerem, RS Ries, JC AF Chambers, Don P. Tamisiea, Mark E. Nerem, R. Steven Ries, John C. TI Effects of ice melting on GRACE observations of ocean mass trends SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GRAVITY; SYSTEM AB The Gravity Recovery and Climate Experiment (GRACE) was designed to measure variations in the Earth's gravity field from space at monthly intervals. Researchers have used these data to measure changes in water mass over various regions, including the global oceans and continental ice sheets covering Greenland and Antarctica. However, GRACE data must be smoothed in these analyses and the effects of geocenter motions are not included. In this study, we examine what effect each of these has in the computation of ocean mass trends using a simulation of ice melting on Greenland, Antarctica, and mountain glaciers. We find that the recovered sea level change is systematically lower when coefficients are smoothed and geocenter terms are not included. Assuming current estimates of ice melting, the combined error can be as large as 30-50% of the simulated sea level rise. This is a significant portion of the long-term sea level change signal, and needs to be considered in any application of GRACE data to estimating long-term trends in sea level due to gain of water mass from melting ice. C1 Univ Texas, Space Res Ctr, Austin, TX 78759 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Chambers, DP (reprint author), Univ Texas, Space Res Ctr, 3925 W Braker Lane,Suite 200, Austin, TX 78759 USA. EM chambers@csr.utexas.edu OI Chambers, Don/0000-0002-5439-0257 NR 13 TC 31 Z9 32 U1 2 U2 10 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 15 PY 2007 VL 34 IS 5 AR L05610 DI 10.1029/2006GL029171 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 147PY UT WOS:000245016100007 ER PT J AU Guz, SS AF Schroll Guz, Savannah TI The encyclopedia of sixties cool: A celebration of the grooviest people, events, and artifacts of the 1960s. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 7 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 15 PY 2007 VL 132 IS 5 BP 94 EP 94 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 148JZ UT WOS:000245072000218 ER PT J AU Averianov, AO Sues, HD AF Averianov, Alexander O. Sues, Hans-Dieter TI A new Troodontid (Dinosauria : Theropoda) from the Cenomanian of Uzbekistan, with a review of troodontid records from the territories of the former Soviet Union SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Review ID STENONYCHOSAURUS-INEQUALIS SAURISCHIA; FAR-EASTERN RUSSIA; REPUBLIC-OF-CHINA; YIXIAN FORMATION; OLDMAN FORMATION; INFORMATION; AFFINITIES; MONGOLIA; FORMOSUS; MAMMALS AB Based on a review of troodontid specimens from the territories of the former Soviet Union, including new discoveries from Uzbekistan, two dental morphotypes can be distinguished among Troodontidae from the Cretaceous of Asia: (1) unserrated teeth, present in Mei from Lujiatun (China; Early Cretaceous: Hauterivian-Barremian), an unnamed taxon from Hovoor (Mongolia; Early Cretaceous: Aptian-Albian), Urbacodon itemirensis, gen. et sp. nov. from Itemir and Urbacodon sp. from Dzharakuduk (Uzbekistan; Late Cretaceous: Cenomanian and Turonian, respectively), and Archaeornithoides from Bayn Dzak and Byronosaurus from Ukhaa Tolgod (Mongolia; Late Cretaceous: Campanian); and (2) serrated teeth, present in Sinornithoides from Huamuxiao (China; Early Cretaceous) and Sinornithoides-like taxa from Khamryn Us (Mongolia; Early Cretaceous: Aptian-Albian), Shestakovo (Russia; Early Cretaceous: Aptian-Albian), and Sheikhdzheili (Uzbekistan; Late Cretaceous: Cenomanian); Troodontidae indet. from Kansai (Tajikistam Late Cretaceous: Santonian) and Alymtau (Kazakhstan; Late Cretaceous: Campanian), Saurornithoides (Mongolia and China; Late Cretaceous: Campanian-Maastrichtian), and Troodon from Kakanaut and Blagoveshchensk (Russia; Late Cretaceous: Maastrichtian). C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 106,POB 37012, Washington, DC 20013 USA. EM lepus@zin.ru; suesh@si.edu RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 NR 107 TC 29 Z9 31 U1 1 U2 7 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR 12 PY 2007 VL 27 IS 1 BP 87 EP 98 DI 10.1671/0272-4634(2007)27[87:ANTDTF]2.0.CO;2 PG 12 WC Paleontology SC Paleontology GA 147CH UT WOS:000244980500009 ER PT J AU Cornelisse, R Casares, J Steeghs, D Barnes, AD Charles, PA Hynes, RI O'Brien, K AF Cornelisse, R. Casares, J. Steeghs, D. Barnes, A. D. Charles, P. A. Hynes, R. I. O'Brien, K. TI A detection of the donor star of Aquila X-1 during its 2004 outburst? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars : individual : Aquila X-1; X-rays : binaries ID X-RAY TRANSIENT; COMPANION STAR; NEUTRON-STAR; MASS; SPECTROSCOPY; EMISSION; QUIESCENCE; DISCOVERY; X1822-371; CURVE AB Phase-resolved high-resolution optical spectroscopy has revealed narrow NIII and He II emission lines from the soft X-ray transient Aquila X-1 during its 2004 outburst that move as a function of the orbit consistent with the phasing of the donor star. Under the assumption that these lines come from the irradiated side of the donor star, we can constrain its K-2 velocity to >= 247 +/- 8 km s(-1) and derive a mass function of f (M-1) >= 1.23 +/- 0.12 M-.. Estimates for the rotational broadening based on the emission components suggest a possible massive neutron star of >= 1.6 M-. (at 95 per cent confidence). However, an updated ephemeris and additional high-resolution spectroscopy of Aql X-1 during a future outburst are warranted in order to confirm that the narrow lines indeed originate on the donor star surface, and reliably characterize the system parameters of this important X-ray binary. Spectra taken during the end of the outburst show that the morphology of the emission lines changed dramatically. No donor star signature was present anymore, while the presence of narrow low-velocity emission lines became clear, making Aql X-1 a member of the slowly growing class of low-velocity emission-line sources. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Inst Astrofis Canarias, E-38200 Santa Cruz de Tenerife, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. S African Astron Observ, ZA-7935 Cape Town, South Africa. Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. European So Observ, Santiago 19, Chile. RP Cornelisse, R (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM corneli@iac.es RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 36 TC 18 Z9 18 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 11 PY 2007 VL 375 IS 4 BP 1463 EP 1470 DI 10.1111/j.1365-2966.2006.11409.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139GE UT WOS:000244419500030 ER PT J AU Schnee, S Kauffmann, J Goodman, A Bertoldi, F AF Schnee, S. Kauffmann, J. Goodman, A. Bertoldi, F. TI The effect of noise in dust emission maps on the derivation of column density, temperature, and emissivity spectral index SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; stars : formation; submillimeter ID MASS STAR-FORMATION; MOLECULAR CLOUD; RADIATIVE-TRANSFER; PRESTELLAR CORES; SUBMILLIMETER; ABSORPTION; DISKS; EXTINCTION; MICRONS; COMPLEX AB We have mapped the central 10' x 10' of the dense core TMC-1C at 450, 850, and 1200 mu m using SCUBA on the James Clerk Maxwell Telescope and MAMBO on the IRAM 30 m telescope. We show that although one can, in principle, use images at these wavelengths to map the emissivity spectral index, temperature, and column density independently, noise and calibration errors would have to be less than similar to 2% to accurately derive these three quantities from a set of three emission maps. Because our data are not this free of errors, we use our emission maps to fit the dust temperature and column density assuming a constant value of the emissivity spectral index and explore the effects of noise on the derived physical parameters. We find that the derived extinction values for TMC-1C are large for a starless core (similar to 80 mag A(V)) and the derived temperatures are low (similar to 6 K) in the densest regions of the core, using our derived value of beta = 1.8. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Bonn, Argelander Inst Astron, D-5300 Bonn, Germany. Max Planck Inst Radioastron, D-5300 Bonn, Germany. 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 31 TC 24 Z9 24 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 MAR 10 PY 2007 VL 657 IS 2 BP 838 EP 848 DI 10.1086/511054 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IU UT WOS:000244928500014 ER PT J AU Mohanty, S Jayawardhana, R Huelamo, N Mamajek, E AF Mohanty, Subhanjoy Jayawardhana, Ray Huelamo, Nuria Mamajek, Eric TI The planetary mass companion 2MASS 1207-3932B: Temperature, mass, and evidence for an edge-on disk SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; planetary systems; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence; techniques : spectroscopic ID TW-HYDRAE ASSOCIATION; MEASURING FUNDAMENTAL PARAMETERS; SPECTRAL ENERGY-DISTRIBUTIONS; AURIGA MOLECULAR CLOUD; NEAR-INFRARED SPECTRA; BROWN DWARF BINARIES; EMBEDDED YOUNG STARS; SUBSTELLAR OBJECTS; KH 15D; CIRCUMSTELLAR DISKS AB We present J-band imaging and H+K-band low-resolution spectroscopy of 2MASS 1207-3932AB, obtained with VLT NACO. For the putative planetary mass secondary, we find J = 20.0 +/- 0.2 mag. The HK spectra of both components imply low gravity and a dusty atmosphere for the secondary. Comparisons to synthetic spectra yield T-eff,(A) approximate to 2550 +/- 150 K and T-eff,T-B approximate to 1600 +/- 100 K, consistent with their late-M and mid-to late-L types. For these Teff and an age of 5-10 Myr, evolutionary models imply M-A approximate to 24 +/- 6 M-Jup and M-B approximate to 8 +/- 2 M-Jup. Independent comparisons of these models to the observed colors, spanning similar to I to L', also yield the same masses and temperatures. Our primary mass agrees with other recent analyses; however, our secondary mass, while still in the planetary regime, is 2-3 times larger than claimed previously. This discrepancy can be traced to the luminosities: while the absolute photometry and M-bol of the primary agree with theoretical predictions, the secondary is similar to 2.5 +/- 0.5 mag fainter than expected in all bands from I to L' and in M-bol. This accounts for the much lower secondary mass (and temperature) derived earlier. We argue that this effect is highly unlikely to result from a variety of model-related problems and is instead real. This conclusion is bolstered by the absence of any luminosity problems in either the primary or AB Pic B, which we also analyze. We therefore suggest gray extinction in 2M1207B, due to occlusion by an edge-on circum-secondary disk. This is consistent with the observed properties of edge-on disks around T Tauri stars and with the known presence of a high-inclination evolved disk around the primary. Finally, the system's implied mass ratio of similar to 0.3 suggests a binary-like formation scenario. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. European So Observ, Very Large Telescope, La Silla, Chile. 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; nhuelamo@eso.org; emamajek@cfa.harvard.edu RI Huelamo, Nuria/C-3042-2017 OI Huelamo, Nuria/0000-0002-2711-8143 NR 103 TC 100 Z9 100 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 10 PY 2007 VL 657 IS 2 BP 1064 EP 1091 DI 10.1086/510877 PN 1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IU UT WOS:000244928500033 ER PT J AU Winn, JN Holman, MJ Roussanova, A AF Winn, Joshua N. Holman, Matthew J. Roussanova, Anna TI The transit light curve project. III. TrES transits of TrES-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : individual (TrES-1); techniques : photometric ID HIGH-RESOLUTION SPECTROSCOPY; SPIN-ORBIT ALIGNMENT; EXTRASOLAR PLANET; ATMOSPHERE; STARS; SURFACE; RADIUS; MASS; SCINTILLATION; CONFIRMATION AB We present z-band photometry of three consecutive transits of the exoplanet TrES-1, with an accuracy of 0.15% and a cadence of 40 s. We improve on estimates of the system parameters, finding in particular that the planetary radius is 1.081 +/- 0.029 R-Jup and the stellar radius is 0.811 +/- 0.020 R.. The uncertainties include both the statistical error and the systematic error arising from the uncertainty in the stellar mass. The transit times are determined to within about 15 s and allow us to refine the estimate of the mean orbital period: P = 3.0300737 +/- 0.0000026 days. We find no evidence for starspots or other irregularities that have been previously reported. C1 MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Winn, JN (reprint author), MIT, Kavli Inst Astrophys & Space Res, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 52 TC 62 Z9 63 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 MAR 10 PY 2007 VL 657 IS 2 BP 1098 EP 1106 DI 10.1086/510834 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 146IU UT WOS:000244928500035 ER PT J AU Breedy, O Guzman, HM AF Breedy, Odalisca Guzman, Hector M. TI A revision of the genus Leptogorgia Milne Edwards & Haime, 1857 (Coelenterata : Octocorallia : Gorgoniidae) in the eastern Pacific SO ZOOTAXA LA English DT Article DE Cnidaria; Coelenterata; Costa Rica; eastern Pacific; gorgonian; octocoral; Leptogorgia; sea fans; Panama; soft corals; taxonomy AB The species of the widespread gorgoniid genus Leptogorgia, which occur along the eastern Pacific, are taxonomically revised based on original type material of all species described until now and reference specimens from recent surveys and expeditions along the Pacific coast of Panama, and Costa Rica. As a result, 21 species are recognized as valid and one as dubious. Lectotypes are assigned for eight species in order to establish their taxonomic status. All the species are described and illustrated. The fauna herein reported does not represent overall diversity or geographical range of each species but adds new reports. The present count is 16 species for Panama, 11 for Costa Rica, 7 for Mexico, 6 for El Salvador, 4 for Peru, 4 for Ecuador, 3 for Colombia, 2 for California, 2 for Nicaragua, and 2 for Chile. C1 Univ Costa Rica, Ctr Invest Ciencias Mar Limnol, San Jose, Costa Rica. Univ Costa Rica, Museo Zool, Escuela Biol, San Jose, Costa Rica. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar Limnol, San Jose, Costa Rica. EM odalisca@racsa.co.cr; guzmanh@naos.si.edu NR 59 TC 28 Z9 30 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 8 PY 2007 IS 1419 BP 1 EP 90 PG 88 WC Zoology SC Zoology GA 144EA UT WOS:000244777300001 ER PT J AU Hoke, KL Ryan, MJ Wilczynski, W AF Hoke, Kim L. Ryan, Michael J. Wilczynski, Walter TI Integration of sensory and motor processing underlying social behaviour in tungara frogs SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE immediate-early gene; tungara frog; social decisions; functional connectivity; effective connectivity; sensorimotor integration ID TREEFROG HYLA-CINEREA; BASAL GANGLIA ORGANIZATION; AXONAL PROJECTION PATTERN; TOAD BOMBINA-ORIENTALIS; MATING CALL PHONOTAXIS; RANA-P-PIPIENS; LEOPARD FROG; HODOLOGICAL CHARACTERIZATION; EFFERENT CONNECTIONS; AUDITORY MIDBRAIN AB Social decision making involves the perception and processing of social stimuli, the subsequent evaluation of that information in the context of the individual's internal and external milieus to produce a decision, and then culminates in behavioural output informed by that decision. We examined brain networks in an anuran communication system that relies on acoustic signals to guide simple, stereotyped motor output. We used egr-1 mRNA expression to measure neural activation in male tungara frogs, Physalaemus pustulosus, following exposure to conspecific and heterospecific calls that evoke competitive or aggressive behaviour. We found that acoustically driven activation in auditory brainstem nuclei is transformed into activation related to sensory-motor interactions in the diencephalon, followed by motor-related activation in the telencephalon. Furthermore, under baseline conditions, brain nuclei typically have correlated egr-1 mRNA levels within brain divisions. Hearing conspecific advertisement calls increases correlations between anatomically distant brain divisions; no such effect was observed in response to calls that elicit aggressive behaviour. Neural correlates of social decision making thus take multiple forms: (i) a progressive shift from sensory to motor encoding from lower to higher stages of neural processing and (ii) the emergence of correlated activation patterns among sensory and motor regions in response to behaviourally relevant social cues. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Georgia State Univ, Dept Psychol, Atlanta, GA 30302 USA. Georgia State Univ, Ctr Behav Neurosci, Atlanta, GA 30302 USA. RP Hoke, KL (reprint author), Univ Texas, Sect Integrat Biol, 1 Univ Stn C0930, Austin, TX 78712 USA. EM khoke@psych.stanford.edu FU NIMH NIH HHS [MH 057066, T32 MH65728, R01 MH057066, T32 MH065728] NR 58 TC 31 Z9 31 U1 0 U2 15 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD MAR 7 PY 2007 VL 274 IS 1610 BP 641 EP 649 DI 10.1098/rspb.2006.0038 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 125KB UT WOS:000243439700006 PM 17254988 ER PT J AU Hall, JPW AF Hall, Jason P. W. TI Two new genera in the Nymphidiina (Lepidoptera : Riodinidae : Nymphidiini) SO ZOOTAXA LA English DT Article DE Adelotypa; Amazon; morphology; Nymphidiini; taxonomy ID PHYLOGENY AB Two new riodinid genera in the subtribe Nymphidiina ( tribe Nymphidiini) are described from the lowlands of the Amazon basin. Livendula Hall, n. gen., is described with huebneri Butler as its type species, and the following eleven species are transferred to Livendula ( n. combs.) from Adelotypa Warren: amasis Hewitson, aminias Hewitson, aristus Stoll, balista Hewitson, epixanthe Stichel, huebneri Butler, jasonhalli Brevignon & Gallard, leucocyana Geyer, leucophaea Hubner, pauxilla Stichel, and violacea Butler. Minotauros Hall, n. gen., is described with lampros Bates as its type species, and the following two species are transferred to Minotauros ( n. combs.) from Adelotypa: lampros Bates, and charessa Stichel. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 5 PY 2007 IS 1415 BP 35 EP 42 PG 8 WC Zoology SC Zoology GA 143IA UT WOS:000244712700003 ER PT J AU Wasserman, A Moiseyev, N AF Wasserman, Adam Moiseyev, Nimrod TI Hohenberg-Kohn theorem for the lowest-energy resonance of unbound systems SO PHYSICAL REVIEW LETTERS LA English DT Article ID DENSITY-FUNCTIONAL THEORY; EXCITED-STATES; EIGENVALUES AB We show that under well-defined conditions the Hohenberg-Kohn theorem (HKT) that provides the foundation of ground-state density functional theory (DFT) can be extended to the lowest-energy resonance of unbound electronic systems. The extended version of the HKT provides an adequate framework to carry out DFT calculations of negative electron affinities. C1 Harvard Univ, Dept Chem & Biol Chem, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 01238 USA. Technion Israel Inst Technol, Schulich Fac Chem, IL-32000 Haifa, Israel. Technion Israel Inst Technol, Minerva Ctr Non Linear Phys, IL-32000 Haifa, Israel. RP Wasserman, A (reprint author), Harvard Univ, Dept Chem & Biol Chem, 12 Oxford St, Cambridge, MA 02138 USA. NR 23 TC 12 Z9 12 U1 0 U2 4 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 2 PY 2007 VL 98 IS 9 AR 093003 DI 10.1103/PhysRevLett.98.093003 PG 4 WC Physics, Multidisciplinary SC Physics GA 141PV UT WOS:000244592100016 PM 17359155 ER PT J AU Arbolino, RD AF Arbolino, Risa Diemond TI Southwest archaeology in the twentieth century. SO AMERICAN ANTHROPOLOGIST LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Arbolino, RD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 2200 WILSON BLVD, STE 600, ARLINGTON, VA 22201 USA SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD MAR PY 2007 VL 109 IS 1 BP 208 EP 209 DI 10.1525/aa.2007.109.1.208 PG 2 WC Anthropology SC Anthropology GA 152FM UT WOS:000245346600025 ER PT J AU Keita, SO Payne, P PascaleV, AK Roya, C AF Keita, S. O. Payne, P., Jr. Pascale, A. K., V Roya, C. TI Fetal programming and early childhood growth insult: Neglected in discussions of the causation of US adult health disparities. SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. Howard Univ, Natl Human Genome Ctr, GenEth Unit, Washington, DC 20059 USA. Howard Univ, Dept Philosophy, Washington, DC 20059 USA. NR 0 TC 1 Z9 1 U1 1 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAR-APR PY 2007 VL 19 IS 2 BP 261 EP 262 PG 2 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 141AB UT WOS:000244547100044 ER PT J AU Ricklefs, RE Bermingham, E AF Ricklefs, Robert E. Bermingham, Eldredge TI The causes of evolutionary radiations in archipelagoes: Passerine birds in the Lesser Antilles SO AMERICAN NATURALIST LA English DT Review DE adaptive radiation; allopatry; colonization; Lesser Antilles; speciation; sympatry ID DARWINS FINCHES; APPARENT COMPETITION; ADAPTIVE RADIATION; WEST-INDIES; CHARACTER DISPLACEMENT; CARIBBEAN REGION; SEXUAL SELECTION; HEBRIDEAN BIRDS; AVIAN MALARIA; ISLAND BIRDS AB To investigate why some lineages undergo evolutionary radiation, we compare the passerine avifaunas of the Hawaiian and Galapagos archipelagoes, which have supported well-known radiations of birds, with those of the Lesser Antilles, which have not. We focus on four steps required for the buildup of diversity through allopatric speciation and secondary sympatry: genetic divergence in isolation, persistence of island populations, recolonization of source islands, and ecological compatibility in secondary sympatry. Analysis of genetic divergence among island populations in the Lesser Antilles reveals evidence of both prolonged independent evolution and re-expansion of differentiated island populations through the archipelago but little evidence of secondary sympatry of divergent genetic lineages. Archipelagoes with high rates of colonization from continental or nearby large- island sources might fail to promote evolutionary radiations because colonists fill ecological space and constrain diversification through competition. However, morphological analysis demonstrated similar divergence between allopatric populations in species in Hawaii, Galapagos, and the Lesser Antilles, although the rate of divergence between secondarily sympatric species evidently is more rapid in Hawaii and the Galapagos. Alternatively, endemic buildup of diversity might be facilitated by the relative absence of pathogens in Hawaii and Galapagos that otherwise could prevent the secondary sympatry of populations owing to disease-mediated competition. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Ricklefs, RE (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. EM ricklefs@umsl.edu; bermingham@si.edu NR 135 TC 65 Z9 67 U1 5 U2 34 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 MAR PY 2007 VL 169 IS 3 BP 285 EP 297 DI 10.1086/510730 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 133SK UT WOS:000244033300001 PM 17230401 ER PT J AU Bernal, XE Page, RA Rand, AS Ryan, MJ AF Bernal, Ximena E. Page, Rachel A. Rand, A. Stanley Ryan, Michael J. TI Natural history miscellany - Cues for eavesdroppers: Do frog calls indicate prey density and quality? SO AMERICAN NATURALIST LA English DT Article DE audience; call preferences; communication network; prey preferences ID PHYSALAEMUS-PUSTULOSUS LEPTODACTYLIDAE; TUNGARA FROG; PARASITOID FLIES; WARNING SIGNALS; BAT PREDATION; PREFERENCES; EVOLUTION; ADVERTISEMENT; ECHOLOCATION; SELECTION AB Predators and parasites that eavesdrop on the mating signals of their prey often preferentially select individuals within a prey/host species that produce specific cues. Mechanisms driving such signal preferences are poorly understood. In the tungara frog Physalaemus pustulosus, conspecific females, frog-eating bats, and blood-sucking flies all prefer complex to simple mating calls. In this study we assess the natural signal variation in choruses in the wild and test two hypotheses for why eavesdroppers prefer complex calls: ( 1) prey quality: complex calls indicate better quality of prey/host, and ( 2) prey density: complex calls indicate higher prey/host density. Call complexity is not correlated with frog length, mass, or body condition, but it does signal higher abundance of prey/host. Thus, increased effectiveness of attack may have played a role favoring the preference for complex calls in eavesdropping heterospecifics. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Bernal, XE (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. EM xbernal@mail.utexas.edu; rachelpage@mail.utexas.edu; mryan@mail.utexas.edu NR 44 TC 35 Z9 35 U1 0 U2 23 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 2007 VL 169 IS 3 BP 409 EP 415 DI 10.1086/510729 PG 7 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 133SK UT WOS:000244033300011 PM 17230403 ER PT J AU Santiago-Blay, JA Lambert, JB AF Santiago-Blay, Jorge A. Lambert, Joseph B. TI Amber's botanical origins revealed SO AMERICAN SCIENTIST LA English DT Article ID TERPENOIDS AB With its fiery hue, amber has been valued for millennia for ornaments. Amber pieces, often hundreds of millions of years old, are even more treasured when they entomb plants, insects or other invertebrates or, more rarely, vertebrates such as amphibians and reptiles. Occasionally, the globules contain evidence of birds or mammals, such as a feather or fur. These inclusions were trapped in ancient sticky tree resin that then hardened and polymerized over the eons to become amber. But whenever an object fetches a high price, fakes are soon to follow. Precious family heirloom jewelry from the early 1900s often turns out to be celluloid or Bakelite plastics. In Sir Arthur Conan Doyle's books, Sherlock Holmes investigated the fake amber industry in England in the 1800s. Even Chinese writers in the fifth century A.D. warned against forgeries made of eggs and fish oil. More recent counterfeits-made of resins, plastics or both-can imitate amber's refractive index, specific gravity and ability to generate a static charge when rubbed. Fortunately, there does not yet seem to be one material that can duplicate all of amber's natural properties. Melted resin from contemporary trees, usually poured over some unfortunate creature, possesses amber's scent and its ability to retain warmth, but not its hardness. Modern polymers mimic amber's property of floating in salt water, but have not yet managed to give off the same piney scent when touched with. a hot needle. Determining a sample's botanical provenance is of interest to the scientist as well as the gemstone dealer and purchaser. Every day on the Internet commerce site eBay, unscrupulous sellers list numerous "amber" pieces that are obviously a sham to even a casual observer, yet unwary buyers still pay hundreds of dollars for these items. But if more skillful simulations were able to fool scientists, the consequences would be greater than just financial loss. Amber is renowned as a preserver of ancient organisms, so paleobiologists study amber samples in an effort to learn more about Earth's past history. Amber specialists, ourselves included, are often asked to evaluate samples. If we were somehow erroneously to give our stamp of approval to a false piece of amber, any inclusion it contained might skew the direction of scientific investigation into that species' lineage. With such a serious outcome on the line, we began to wonder, could we be fooled? Scientists can use more-modem tools and tests than a simple smell check to aid in their verification of a sample. Nuclear magnetic resonance (NMR) spectroscopy uses the magnetic properties of nuclei such as hydrogen or carbon to characterize different substances. The chemical environment of the nuclei influences their interaction with a magnetic field, as registered by what is called the chemical shift. The result is a spectrum of frequencies, reflecting the array of chemical species present in the material. This creates a sort of fingerprint for each compound in the sample. But not all amber is the same. Deposits are found in several regions around the world and likely from more plant families than currently known from the fossil record. Therefore it's necessary to create NMR catalogs of many different kinds of amber. Besides helping to discern true from spurious samples, such a library has the added advantage of possibly indicating what kind of tree the amber may have come from, which could give us a better idea of the prehistoric landscape. But to tell what tree amber came from, we may need to have something to compare it with as a starting point. Our approach has been to start with the exudates that modern plants ooze. There is no comprehensive library that relates NMR signatures to the taxonomy of modern plants that produce exudates. For the past 10 years, one of us (Santiago-Blay) has been amassing samples from all kinds of plants. We have now begun to outline the chemical picture of these gathered specimens of plant exudates. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Gallaudet Univ, Washington, DC 20002 USA. Northwestern Univ, Evanston, IL 60208 USA. RP Santiago-Blay, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121,10th & Constitut Ave,POB 37012, Washington, DC 20013 USA. EM blayj@si.edu NR 17 TC 8 Z9 10 U1 0 U2 17 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 2007 VL 95 IS 2 BP 150 EP 157 DI 10.1511/2007.64.1020 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 136AS UT WOS:000244195600023 ER PT J AU Songsasen, N Wildt, DE AF Songsasen, N. Wildt, D. E. TI Oocyte biology and challenges in developing in vitro maturation systems in the domestic dog SO ANIMAL REPRODUCTION SCIENCE LA English DT Review DE dog oocyte; folliculogenesis; oogenesis; in vitro maturation ID FOLLICLE-STIMULATING-HORMONE; EPIDERMAL-GROWTH-FACTOR; MEIOSIS-ACTIVATING SUBSTANCE; BITCH CANIS-FAMILIARIS; EARLY ANTRAL FOLLICLES; NUCLEAR MATURATION; DEVELOPMENTAL COMPETENCE; MEIOTIC COMPETENCE; CUMULUS CELLS; ZONA-PELLUCIDA AB The oocyte of the domestic dog, is unique from that of other mammalian species studied to date. Ovulation occurs either once or twice per year, with the oocyte released at the germinal vesicle stage, and then completing nuclear and cytoplasmic maturation within the oviduct under the influence of rising circulating progesterone. In vivo meiotic maturation of the bitch oocyte is completed within 48-72 h after ovulation, which is longer than 12-36 h required for oocytes from most other mammalian species. Due to these inherently novel traits, in vitro culture systems developed for maturing oocytes of other species have been found inadequate for maturation of dog oocytes. On average, only 15-20% of ovarian oocytes achieve the metaphase II stage after 48-72 h of in vitro culture. Thus far, no offspring have been produced in the dog (or other canids) by transferring embryos derived from in vitro matured oocytes. This review addresses current knowledge about dog reproductive physiology, specifically those factors influencing in vitro developmental competence of the oocyte. This summary lays a foundation for identifying the next steps to understanding the mechanisms regulating meiotic maturation and developmental competence of the dog oocyte. Published by Elsevier B.V. C1 Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. RP Songsasen, N (reprint author), Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. EM songsasenn@si.edu FU NCRR NIH HHS [K01 RR020564-01, K01 RR020564, K01 RR020565] NR 135 TC 51 Z9 56 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 EI 1873-2232 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD MAR PY 2007 VL 98 IS 1-2 BP 2 EP 22 DI 10.1016/j.anireprosci.2006.10.004 PG 21 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 144NS UT WOS:000244803700002 PM 17097840 ER PT J AU Littler, MM Littler, DS AF Littler, Mark M. Littler, Diane S. TI Assessment of coral reefs using herbivory/nutrient assays and indicator groups of benthic primary producers: a critical synthesis, proposed protocols, and critique of management strategies SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS LA English DT Review DE coral reefs; eutrophication; management; relative-dominance model; monitoring; indicator groups; herbivory; nutrients ID GREAT-BARRIER-REEF; FUNCTIONAL-FORM GROUPS; NUTRIENT ENRICHMENT; COMMUNITY STRUCTURE; FLORIDA-KEYS; MACROALGAL BLOOMS; SOUTHEAST FLORIDA; ALGAL COMMUNITY; RED-SEA; HERBIVORE EXCLUSION AB 1. Rapid assessment protocols for determining and monitoring the status of any given coral reef are provided and include measuring: (a) standing stocks of functional indicator groups, (b) herbivore populations, (c) water-column nutrient levels, (d) tissue C:N:P ratios, (e) algal physiological-response assays, and (f) herbivory assays. These measurements can reveal quantitative tipping-point levels beyond which resilience to undesirable phase shifts begins to become critically reduced. Universal tipping-point approximations are reviewed for inorganic nutrients, and posited for the first time for herbivory. 2. The relative roles of top-down and bottom-up controls in determining benthic community structure and the health of coral reefs are especially important management concerns. This paper specifically addresses the top-down effects of herbivory and bottom-up effects of nutrient enrichment on critical indicator groups, i.e. reef-building corals, crustose coralline algae, dense turf algae and frondose macroalgae. 3. A predominance of (a) massive corals and calcareous coralline algae relative to frondose macroalgae and algal turfs indicates a healthy spatially heterogeneous condition reflecting low nutrients and high herbivory. An abundance of (b) frondose macroalgae illustrates the least desirable condition of elevated nutrient levels and reduced herbivory, possibly reflecting pollution in concert with destructive herbivore fishing practices. High coverage of (c) coralline algae suggests healthy high herbivory levels, but problems with elevated nutrients that are inhibitory to some corals. Domination by (d) dense turf algae indicates desirably low nutrient levels, but an inadequate herbivory component. 4. The fast growth and turnover rates of fleshy algae compared to other reef organisms highlight their value as early warning indicators of reef degradation. 5. From a management perspective, levels of herbivory and nutrients rank among the most useful quantitative indicators of coral reef resilience; whereas, the degree of degradation and mortality are inferred from the above functional indicator groups of benthic primary producers. Published in 2006 by John Wiley & Sons, Ltd. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Littler, MM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC166,POB 37012, Washington, DC 20013 USA. EM littlerm@si.edu NR 170 TC 34 Z9 36 U1 4 U2 47 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1052-7613 J9 AQUAT CONSERV JI Aquat. Conserv.-Mar. Freshw. Ecosyst. PD MAR-APR PY 2007 VL 17 IS 2 BP 195 EP 215 DI 10.1002/aqc.790 PG 21 WC Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 149KJ UT WOS:000245145500005 ER PT J AU Loring, S Spiess, A AF Loring, Stephen Spiess, Arthur TI Further documentation supporting the former existence of grizzly bears (Ursus arctos) in northern Quebec-Labrador SO ARCTIC LA English DT Article DE Labrador; barren-ground grizzly bear; Ursus arctos; Innu; William Brooks Cabot; Lucien Turner; William Duncan Strong ID SKULL; SIZE AB The discovery in 1976 of a grizzly bear (Ursus arctos) skull in an 18th-century Labrador Inuit midden effectively ended speculation about the former existence of the species in the barrenlands of northern Quebec and Labrador. We analyzed a photograph of a bear skull taken in 1910 at an Innu camp in the Labrador interior (east of the George River), which appears to be that of a grizzly bear. Coupled with previously unpublished historical accounts by Lucien Turner (Smithsonian naturalist in northern Quebec, 1881-83) and William Duncan Strong (anthropologist in Labrador, 1928-29), Innu oral history accounts, and archaeological evidence, this photograph further substantiates the theory that a small number of grizzly bears were present in the Quebec-Labrador peninsula and survived into the 20th century. C1 Smithsonian Inst, Arctic Studies Ctr, Washington, DC 20013 USA. Maine Hist Preservat Commiss, Augusta, ME 04333 USA. RP Loring, S (reprint author), Smithsonian Inst, Arctic Studies Ctr, POB 37012,NMNH MRC 112, Washington, DC 20013 USA. EM lorings@si.edu; Arthur.Spiess@maine.gov NR 42 TC 4 Z9 4 U1 0 U2 2 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 2007 VL 60 IS 1 BP 7 EP 16 PG 10 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 152PG UT WOS:000245373400003 ER PT J AU Kewley, LJ Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ AF Kewley, Lisa J. Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. Kurtz, Michael J. TI SDSS 0809+1729: Connections between extremely metal-poor galaxies and gamma-ray burst hosts SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : dwarf; galaxies : fundamental parameters; galaxies : starburst; gamma rays : bursts ID BLUE COMPACT GALAXIES; DIGITAL SKY SURVEY; STAR-FORMATION RATES; LUMINOSITY-METALLICITY RELATION; PRIMORDIAL HELIUM ABUNDANCE; DWARF IRREGULAR GALAXIES; HEAVY-ELEMENT ABUNDANCES; EMISSION-LINE GALAXIES; H-II REGIONS; SPIRAL GALAXIES AB We discuss the serendipitous discovery of an extremely metal-poor galaxy, SDSS 0809+1729, classified as a star in the Sloan Digital Sky Survey (SDSS). The galaxy has a redshift z = 0.0441 and a B-band absolute magnitude M-B = 17.1. With a metallicity of log (O/H) + 12 similar to 7.44 or similar to 1/20 solar, this galaxy is among the 10 most metal-poor emission-line galaxies known. SDSS 0809+1729 is a blue compact galaxy (BCG) with a stellar age of similar to 4.5 Myr, a star formation rate of 0.18 M-circle dot yr(-1), and a large gas-phase electron density (similar to 367 cm(-3)). Similar values of these parameters are common among other extremely metal-poor galaxies, including I Zw 18. SDSS 0809+1729 is, however, unusual among BCGs because it lies in the same region of the luminosity-metallicity diagram as the two lowest metallicity long-duration gamma-ray burst (GRB) hosts. For a given B-band luminosity, both nearby GRB hosts and SDSS 0809+1729 have systematically lower metallicities than dwarf irregulars, the majority of BCGs, and normal star-forming galaxies. Because the star formation properties of SDSS 0809+1729 are similar to nearby long-duration GRB hosts, SDSS 0809+1729 may be a potential GRB host. Identification of larger samples of similar extremely metal-poor objects may provide important insights into the conditions required to produce long-duration GRBs. C1 Univ Hawaii, Honolulu, HI 96822 USA. Smithsonian Astrophys Observ, Cambridge, MA USA. RP Kewley, LJ (reprint author), Univ Hawaii, Honolulu, HI 96822 USA. EM kewley@ifa.hawaii.edu RI KURTZ, Michael /B-3890-2009; OI Kenyon, Scott/0000-0003-0214-609X; Kurtz, Michael/0000-0002-6949-0090 NR 100 TC 47 Z9 47 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2007 VL 133 IS 3 BP 882 EP 888 DI 10.1086/509135 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142GE UT WOS:000244636600007 ER PT J AU Krips, M Eckart, A Neri, R Bertram, T Straubmeier, C Fischer, S Staguhn, JG Vogel, SN AF Krips, M. Eckart, A. Neri, R. Bertram, T. Straubmeier, C. Fischer, S. Staguhn, J. G. Vogel, S. N. TI Barred CO emission in HE 1029-1831 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : kinematics and dynamics; galaxies : individual : HE 1029-1831; radio lines : galaxies; galaxies : Seyfert ID MOLECULAR GAS; GALAXIES NUGA; INFRARED GALAXIES; NUCLEI; AGN AB We present CO(1-0) and CO(2-1) line emission maps of the barred spiral active galaxy HE 1029-1831 (z = 0.0403) obtained with the IRAM Plateau de Bure Interferometer (PdBI) and in part by the Berkeley-Illinois-Maryland Association (BIMA) observatory. The CO emission is well associated with the optical bar and extended along it. The FWHM of the CO emission is estimated to be similar to(6 +/- 2) kpc. The CO emission shows a strong velocity gradient along the minor axis of the bar (PA = 90 degrees). The molecular gas mass is estimated to be similar to 1.2 x 10(10) M-circle dot which indicates a very gas rich host galaxy. Most of the molecular gas appears to be subthermally excited and cold but we also find weak evidence for a warmer and/or denser gas component at the southern part of the bar emission, about similar to 4 kpc from the galactic nucleus. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Harvard Smithsonian Ctr Astrophys, SMA Project, Hilo, HI 96720 USA. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. RP Krips, M (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM mkrips@cfa.harvard.edu NR 17 TC 8 Z9 8 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2007 VL 464 IS 1 BP 187 EP 191 DI 10.1051/0004-6361:20065832 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139BV UT WOS:000244407900019 ER PT J AU Krips, M Eckart, A Krichbaum, TP Pott, JU Leon, S Neri, R Garcia-Burillo, S Combes, F Boone, F Baker, AJ Tacconi, LJ Schinnerer, E Hunt, LK AF Krips, M. Eckart, A. Krichbaum, T. P. Pott, J. -U. Leon, S. Neri, R. Garcia-Burillo, S. Combes, F. Boone, F. Baker, A. J. Tacconi, L. J. Schinnerer, E. Hunt, L. K. TI NUclei of GAlaxies V. Radio emission in 7 NUGA sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : Seyfert; galaxies : nuclei; galaxies : jets; radio continuum : galaxies ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; DOMINATED ACCRETION FLOWS; SGR-A-ASTERISK; 1.49 GHZ ATLAS; MOLECULAR GAS; VELOCITY DISPERSION; SEYFERT-GALAXIES; SPIRAL GALAXIES; LIMITED SAMPLE AB We present high angular resolution radio snap-shot observations of seven nearby low-luminosity active galaxies (LLAGN) from the NUclei of GAlaxies (NUGA) survey. The observations were conducted with MERLIN and EVN/VLBI at 18 cm and 6 cm. At all observed angular resolutions and frequencies, we find indications for extended emission in about similar to 40% of the sources, consistent with the decrease of flux with increasing angular resolution. The extended components resemble jet emission in a majority of cases, consistent with the optically thin synchrotron emission implied by their steep spectra. We consider the compact 6 cm EVN/VLBI radio emission of our sources in the context of the "fundamental plane" that previous LLAGN studies identified within the three-dimensional parameter space of radio luminosity, X-ray luminosity, and black hole mass. We demonstrate, using NGC 7217 and NGC 1068 as particular examples, that high-resolution, multi-epoch radio observations offer useful information about the origin of offsets from the fundamental plane. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Harvard Smithsonian Ctr Astrophys, SMA Project, Hilo, HI 96720 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. European So Observ, D-85748 Garching, Germany. Inst Astrofis Andalucia, CSIC, E-18080 Granada, Spain. IRAM, E-18012 Granada, Spain. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. Observ Madrid, OAN, E-28014 Madrid, Spain. Observ Paris, LERMA, F-75014 Paris, France. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Ist Radioastron, Sez Firenze, INAF, I-50125 Florence, Italy. RP Krips, M (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM krips@ph1.uni-koeln.de; eckart@ph1.uni-koeln.de; tkrichbaum@mpifr-bonn.mpg.de; jpott@eso.org; leon@iram.es; neri@iram.fr; s.gburillo@oan.es; francoise.combes@obspm.fr; fboone@mpifr-bonn.mpg.de; ajbaker@physics.rutgers.edu; linda@mpe.mpg.de; schinner@mpia.de; hunt@arcetri.astro.it OI Garcia-Burillo, Santiago/0000-0003-0444-6897; Schinnerer, Eva/0000-0002-3933-7677; Combes, Francoise/0000-0003-2658-7893 NR 70 TC 29 Z9 29 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2007 VL 464 IS 2 BP 553 EP 563 DI 10.1051/0004-6361:20065037 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142VU UT WOS:000244679500020 ER PT J AU Zhang, Y Ercolano, B Liu, XW AF Zhang, Y. Ercolano, B. Liu, X. -W. TI Temperature fluctuations in HII regions: t(2) for the two-phase model SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : general; ISM : HII regions ID ELECTRON-TEMPERATURE; PLANETARY-NEBULAE AB Aims. We investigate temperature fluctuations in H II regions in terms of a two-phase model, which assumes that the nebular gas consists of a hot and a cold phase. Methods. We derive general formulae for T([O III]), the [O III] forbidden line temperature, and T(H I), the hydrogen Balmer jump temperature, in terms of the temperatures of the hot and cold phases, T-h and T-c. Results. For large temperature differences, the values of t(2) required to account for the observed difference between T([O III]) and T(H I) are much lower than those deduced using the classical formulae that assume random and small amplitude temperature fluctuations. One should therefore be cautious when using a two-phase model to account for empirically derived t(2) values. We present a correction of a recent work by Giammanco & Beckman, who use a two-phase model to estimate the ionization rate of H II regions by cosmic rays. We show that a very small amount of cold gas is sufficient to account for t(2) values typically inferred for H II regions. C1 Peking Univ, Dept Astron, Beijing 100871, Peoples R China. Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, Y (reprint author), Peking Univ, Dept Astron, Beijing 100871, Peoples R China. EM zhangy96@hkucc.hku.hk NR 10 TC 4 Z9 4 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2007 VL 464 IS 2 BP 631 EP 634 DI 10.1051/0004-6361:20066564 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142VU UT WOS:000244679500028 ER PT J AU Leipski, C Haas, M Meusinger, H Siebenmorgen, R Chini, R Drass, H Albrecht, M Wilkes, BJ Huchra, JP Ott, S Cesarsky, C Cutri, R AF Leipski, C. Haas, M. Meusinger, H. Siebenmorgen, R. Chini, R. Drass, H. Albrecht, M. Wilkes, B. J. Huchra, J. P. Ott, S. Cesarsky, C. Cutri, R. TI Narrow-line AGN in the ISO-2MASS survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : quasars : general; infrared : galaxies ID ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; DIGITAL SKY SURVEY; ULTRALUMINOUS INFRARED GALAXIES; II RADIO GALAXIES; OPTICAL SPECTROSCOPY; SPECTROGRAPH IRS; UNIFIED MODELS; QUASARS; SPECTRA AB Context. A long- standing challenge of observational AGN research is to find type 2 quasars, the luminous analogues of Seyfert- 2 galaxies. Aims. We search for luminous narrow- line type 2 AGN, characterise their properties, and compare them with broad- line type 1 AGN. Methods. Combining the ISOCAM parallel survey at 6.7 mu m with 2MASS, we have selected AGN via near- mid- infrared colours caused by the hot nuclear dust emission. We performed spectroscopy in the optical and, for a subset of the sample, also in the mid-infrared with Spitzer. Results. We find nine type 2 AGN at redshift 0.1 < z < 0.5, three of them have even quasar- like [ OIII] luminosities. At the given redshift and luminosity range the number of type 2 AGN is at least as high as that of type 1s. At z > 0.5 we did not find type 2 AGN, probably because the hottest dust emission, still covered by the NIR filters, is obscured. The optical spectra of the type 2 host galaxies show young and old stellar populations. Only one object is an ultraluminous infrared galaxy with starburst. The 5 - 38 mu m spectra of the two type 2 sources observed show a strong continuum with PAH emission in one case and silicate absorption in the other case. Conclusions. The near- mid- infrared selection is a successful strategy to find luminous type 2 AGN at low z. The objects exhibit a large range of properties so that it is di. cult to infer details by means of popular SED fitting with simple average templates. C1 Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. Thuringer Landessternwarte Tautenburg, Tautenburg, Germany. ESO, D-85748 Garching, Germany. UCN, Inst Astron, Antofagasta, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. ESA, HERSCHEL Sci Ctr, NL-2200 AG Noordwijk, Netherlands. CALTECH, IPAC, Pasadena, CA 91125 USA. RP Leipski, C (reprint author), Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany. EM leipski@physics.ucsb.edu OI Wilkes, Belinda/0000-0003-1809-2364 NR 39 TC 9 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2007 VL 464 IS 3 BP 895 EP 901 DI 10.1051/0004-6361:20066168 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 143WJ UT WOS:000244756800022 ER PT J AU Brunken, S Gottlieb, CA Gupta, H McCarthy, MC Thaddeus, P AF Brunken, S. Gottlieb, C. A. Gupta, H. McCarthy, M. C. Thaddeus, P. TI Laboratory detection of the negative molecular ion CCH- SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line : identification; molecular data; astrochemistry; methods : laboratory; ISM : molecules; radio lines : ISM ID SPECTRAL-LINE SURVEY; WAVE SPECTRUM; ORION-KL; GHZ; CHEMISTRY; C2H; MILLIMETER; IRC+10216; CLOUDS; CNH AB Aims. This paper reports the laboratory detection of the rotational spectrum of the acetylide anion, CCH-. Methods. Five successive rotational transitions have been measured to high accuracy in a dc discharge with a free space millimeterwave spectrometer in the frequency range 83 - 417 GHz. Results. Precise spectroscopic constants have been obtained for CCH- and transition rest frequencies can now be calculated to better than 1 km s(-1) in equivalent radial velocity far into the terahertz region, allowing for deep astronomical searches for this anion in space. The highly stable and fairly polar CCH- anion is a likely candidate for radio astronomical detection, its neutral analogue CCH being among one of the most abundant molecules in a wide variety of astrophysical sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Texas, Inst Theoret Chem, Dept Chem & Biochem, Austin, TX 78712 USA. RP Brunken, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sbruenken@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; McCarthy, Michael/0000-0001-9142-0008 NR 31 TC 25 Z9 25 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2007 VL 464 IS 3 BP L33 EP L36 DI 10.1051/0004-6361:20066964 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 143WJ UT WOS:000244756800003 ER PT J AU Klochkov, D Horns, D Santangelo, A Staubert, R Segreto, A Ferrigno, C Kretschmar, P Kreykenbohm, I La Barbera, A Masetti, N McCollough, M Pottschmidt, K Schonherr, G Wilms, J AF Klochkov, D. Horns, D. Santangelo, A. Staubert, R. Segreto, A. Ferrigno, C. Kretschmar, P. Kreykenbohm, I. La Barbera, A. Masetti, N. McCollough, M. Pottschmidt, K. Schoenherr, G. Wilms, J. TI INTEGRAL and Swift observations of EXO 2030+375 during a giant outburst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-ray binaries; stars : neutron; accretion, accretion disks ID X-RAY SOURCES; EXO-2030+375; PULSAR; DISCOVERY; TELESCOPE; ACCRETION; MISSION AB Aims. We investigate the X- ray spectral and timing properties of the high mass X- ray binary EXO 2030+ 375 observed during its June - September 2006 giant ( type II) outburst. Methods. The data analyzed in this work are from partly simultaneous observations with INTEGRAL and Swift. The pulse period P and its temporal derivative. P are measured. X- ray pulse profiles in different energy ranges and time intervals are constructed. Pulse averaged X- ray spectra for different time intervals are studied. Results. We report a strong spin-up of the source during the outburst, comparable to that observed in 1985 during the previous giant outburst when the source was discovered. The value of. P is found to be linearly related to the X- ray luminosity of the source during the outburst. For the first time the hard X- ray (> 25 keV) characteristics of the source during a type II outburst are studied. The X- ray pulse profiles apparently change with luminosity. The X- ray spectral continuum in the 3 - 120 keV energy range is modeled with an absorbed power law with an exponential cutoff around E similar to 26 keV. An iron emission line at similar to 6 - 7 keV is observed. The spectrum reveals some features between 10 and 20 keV which can be modeled either by a broad emission line at similar to 13 - 15 keV ( a " bump") or by two absorption lines at similar to 10 and similar to 20 keV. C1 Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. INAF IFC Pa, I-90146 Palermo, Italy. Integral SOC ESA, Madrid, Spain. INTEGRAL Sci Data Ctr, Versoix, Switzerland. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Univ Erlangen Nurnberg, Inst Astron, D-96049 Bamberg, Germany. INAF IASF Bo, I-40129 Bologna, Italy. RP Klochkov, D (reprint author), Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM klochkov@astro.uni-tuebingen.de RI Horns, Dieter/C-9727-2011; Ferrigno, Carlo/H-4139-2012; Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803; Segreto, Alberto/0000-0001-7341-6603; LA BARBERA, ANTONINO/0000-0002-5880-8913; Kretschmar, Peter/0000-0001-9840-2048; Masetti, Nicola/0000-0001-9487-7740 NR 20 TC 15 Z9 16 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2007 VL 464 IS 3 BP L45 EP L48 DI 10.1051/0004-6361:20066801 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 143WJ UT WOS:000244756800006 ER PT J AU Kelly, BC Bechtold, J Siemiginowska, A Aldcroft, T Sobolewska, M AF Kelly, Brandon C. Bechtold, Jill Siemiginowska, Aneta Aldcroft, Tom Sobolewska, Malgorzata TI Evolution of the X-ray emission of radio-quiet quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; quasars : general; ultraviolet : galaxies; X-rays : galaxies ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QUASARS; ABSORPTION-LINE QUASARS; XMM-NEWTON OBSERVATIONS; DRIVEN ACCRETION FLOWS; ASTRONOMICAL DATA; CHANDRA SURVEY; BLACK-HOLE; ULTRAVIOLET LUMINOSITY AB We report new Chandra observations of seven optically faint, z similar to 4 radio-quiet quasars (RQQs). We have combined these new observations with previous Chandra observations of RQQs to create a sample of 174 sources. These sources have 0.1 < z < 4.7, and 10(44) ergs s(-1) < nu L-nu (2500 angstrom) < 10(48) ergs s(-1). The X- ray detection fraction is 90%. We find that the X- ray loudness of RQQs decreases with UV luminosity and increases with redshift. The model that is best supported by the data has a linear dependence of optical to X-ray ratio alpha(ox) on cosmic time and a quadratic dependence of alpha(ox) on log L-UV, where alpha(ox) becomes X-ray quiet more rapidly at higher log L-UV. We find no significant evidence for a relationship between the X-ray photon index Gamma(x) and the UV luminosity, and we findmarginally significant evidence that the X-ray continuum flattens with increasing z (2 sigma). The Gamma(x)-z anticorrelation may be the result of X-ray spectral curvature, redshifting of a Compton reflection component into the observed Chandra band, and/or redshifting of a soft excess out of the observed Chandra band. Using the results for Gamma(x), we show that the alpha(ox)-z relationship is unlikely to be a spurious result caused by redshifting of the observable X-ray spectral region. A correlation between alpha(ox) and z implies evolution of the accretion process. We present a qualitative comparison of these new results with models for accretion disk emission. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Durham, Dept Phys, Durham, England. RP Kelly, BC (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM bkelly@as.arizona.edu; jbechtold@as.arizona.edu; asiemiginowska@cfa.harvard.edu; taldcroft@cfa.harvard.edu; m.a.sobolewska@durham.ac.uk NR 96 TC 40 Z9 40 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 2007 VL 657 IS 1 BP 116 EP 134 DI 10.1086/510876 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142FR UT WOS:000244635300011 ER PT J AU Siemiginowska, A Stawarz, L Cheung, CC Harris, DE Sikora, M Aldcroft, TL Bechtold, J AF Siemiginowska, Aneta Stawarz, Lukasz Cheung, C. C. Harris, D. E. Sikora, Marek Aldcroft, Thomas L. Bechtold, Jill TI The 300 kpc long X-ray jet in PKS 1127-145, z=1.18 quasar: Constraining X-ray emission models SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : individual (PKS 1127-145); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; SPECTRUM RADIO-SOURCES; LARGE-SCALE JETS; RELATIVISTIC JETS; EXTRAGALACTIC JETS; CHANDRA DISCOVERY; DEEP CHANDRA; 3C-273; GALAXIES AB We present a similar to 100 ks Chandra X-ray observation and new VLA radio data of the large-scale, 300 kpc long X-ray jet in PKS 1127-145, a radio-loud quasar at redshift z = 1.18. With this deep X-ray observation we now clearly discern the complex X-ray jet morphology and see substructure within the knots. The X-ray and radio jet intensity profiles are seen to be strikingly different, with the radio emission peaking strongly at the two outer knots while the X-ray emission is strongest in the inner jet region. The jet X-ray surface brightness gradually decreases by an order of magnitude going out from the core. The new X-ray data contain sufficient counts for spectral analysis of the key jet features. The X-ray energy index of the inner jet is relatively flat with alpha(X) = 0.66 +/- 0.15 and steep in the outer jet with alpha(X) = 1.0 +/- 0.2. We discuss the constraints implied by the new data on the X-ray emission models and conclude that "one-zone'' models fail and that at least a two-component model is needed to explain the jet's broadband emission. We propose that the X-ray emission originates in the jet proper while the bulk of the radio emission comes from a surrounding jet sheath. We also consider intermittent jet activity as a possible cause of the observed jet morphology. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Landessternwarte Heidelberg, Konigstuhl, Germany. Jagiellonian Univ, Obserwatorium Astron, Krakow, Poland. Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. Copernicus Astron Ctr, Warsaw, Poland. Univ Arizona, Steward Observ, Tucson, AZ USA. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 62 TC 36 Z9 36 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 MAR 1 PY 2007 VL 657 IS 1 BP 145 EP 158 DI 10.1086/510898 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142FR UT WOS:000244635300013 ER PT J AU Rines, K Diaferio, A Natarajan, P AF Rines, Kenneth Diaferio, Antonaldo Natarajan, Priyamvada TI The virial mass function of nearby SDSS galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : observations; galaxies : clusters : general; galaxies : kinematics and dynamics ID DIGITAL SKY SURVEY; COLD DARK-MATTER; RAY LUMINOSITY FUNCTION; TO-LIGHT RATIO; X-RAY; INFALL REGION; REDSHIFT SURVEY; COSMOLOGICAL CONSTRAINTS; VELOCITY DISPERSIONS; RICH CLUSTERS AB We present a new determination of the cluster mass function and velocity dispersion function in a volume similar to 10(7) h(3) Mpc(-3) using data from the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to determine virial masses. We use the caustic technique to remove foreground and background galaxies. The cluster virial mass function agrees well with recent estimates from both X-ray observations and cluster richnesses. Our determination of the mass function lies between those predicted by the 1 and 3 year WMAP data. We constrain the cosmological parameters Omega(m) and sigma(8) and find good agreement with WMAP and constraints from other techniques. With the CIRS mass function alone, we estimate Omega(m) = 0.24(-0.09)(+0.14) and sigma(8) = 0.92(-0.19)(+0.24), or sigma(8) 0.84 +/- 0.03 when holding Omega(m) = 0.3 fixed. We also use the WMAP parameters as priors and constrain velocity segregation in clusters. Using the 1 and 3 year results, we infer velocity segregation of sigma(gxy)/sigma(DM) approximate to 0.94 +/- 0.05 or 1.28 +/- 0.06, respectively. The good agreement of various estimates of the cluster mass function shows that it is a useful independent constraint on estimates of cosmological parameters. We compare the velocity dispersion function of clusters to that of early-type galaxies and conclude that clusters comprise the high-velocity end of the velocity dispersion function of dark matter halos. Future studies of galaxy groups are needed to study the transition between dark matter halos containing individual galaxies and those containing systems of galaxies. The evolution of cluster abundances provides constraints on dark energy models; the mass function presented here offers an important low-redshift calibration benchmark. C1 Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT USA. Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Turin, Italy. Yale Univ, Dept Astron, New Haven, CT 06511 USA. RP Rines, K (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA. EM krines@astro.yale.edu; diaferio@ph.unito.it; priya@astro.yale.edu NR 137 TC 38 Z9 38 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 MAR 1 PY 2007 VL 657 IS 1 BP 183 EP 196 DI 10.1086/510829 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142FR UT WOS:000244635300017 ER PT J AU Sun, M Jones, C Forman, W Vikhlinin, A Donahue, M Voit, M AF Sun, M. Jones, C. Forman, W. Vikhlinin, A. Donahue, M. Voit, M. TI X-ray thermal coronae of galaxies in hot clusters: Ubiquity of embedded mini-cooling cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE conduction; cooling flows; galaxies : clusters : general; magnetic fields; radio continuum : galaxies; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; DYNAMICALLY YOUNG CLUSTER; FUNDAMENTAL-PLANE-SURVEY; ELLIPTIC GALAXIES; COMA-CLUSTER; XMM-NEWTON; CHANDRA OBSERVATIONS; INTERSTELLAR-MEDIUM; INTRACLUSTER MEDIUM; SPECTROSCOPIC DATA AB We present a systematic investigation of X-ray thermal coronae in 157 early-type and 22 late-type galaxies from a survey of 25 hot (kT > 3 keV), nearby (z < 0.05) clusters, based on Chandra archival data. Cool galactic coronae (kT = 0.5-1.1 keV generally) have been found to be common, > 60% in L-Ks > 2L(*) galaxies. These embedded coronae in hot clusters are generally smaller, less luminous, and less massive than coronae in poor environments, demonstrating the negative effects of hot cluster environments on galactic coronae. Nevertheless, these coronae still manage to survive ICM stripping, evaporation, rapid cooling, and powerful AGN outflows, making them a rich source of information about gas stripping, microscopic transport, and feedback processes in the cluster environment. Heat conduction across the boundary of the coronae has to be suppressed by a factor of greater than or similar to 100, which implies that the X-ray gas in early-type galaxies is magnetized and the magnetic field plays an important role in energy transfer. The luminous, embedded coronae, with high central density (0.1-0.4 cm(-3)), are miniversions of group and cluster cooling cores. As the prevalence of coronae of massive galaxies implies a long lifetime (greater than or similar to several Gyr), there must be a heat source inside coronae to offset cooling. While we argue that AGN heating may not generally be the heat source, we conclude that SN heating can be enough as long as the kinetic energy of SNe can be efficiently dissipated. Diffuse thermal coronae have also been detected in at least 8 of 22 late-type galaxies in our sample. The fraction of luminous X-ray AGNs (> 10(41) ergs s(-1)) is not small (similar to 5%) in our sample. C1 Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Inst, Moscow, Russia. RP Sun, M (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM sunm@pa.msu.edu RI Donahue, Megan/B-5361-2012; OI Forman, William/0000-0002-9478-1682; Voit, Gerard/0000-0002-3514-0383 NR 95 TC 98 Z9 98 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 2007 VL 657 IS 1 BP 197 EP 231 DI 10.1086/510895 PN 1 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142FR UT WOS:000244635300018 ER PT J AU Lugger, PM Cohn, HN Heinke, CO Grindlay, JE Edmonds, PD AF Lugger, Phyllis M. Cohn, Haldan N. Heinke, Craig O. Grindlay, Jonathan E. Edmonds, Peter D. TI Chandra X-ray sources in the collapsed-core globular cluster M30 (NGC 7099) SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters : individual (M30, NGC 7099); novae, cataclysmic variables; stars : neutron; X-rays : binaries ID HUBBLE-SPACE-TELESCOPE; SUBDWARF-B-STARS; NEUTRON-STARS; CCD PHOTOMETRY; 47 TUCANAE; GLOBULAR-CLUSTER-47 TUCANAE; LUMINOSITY FUNCTIONS; MILLISECOND PULSARS; MODEL ATMOSPHERES; MASS SEGREGATION AB We report the detection of six discrete, low-luminosity (L-X < 10(33) ergs s(-1)) X- ray sources, located within 12" of the center of the collapsed-core globular cluster M30 (NGC 7099), and a total of 13 sources within the half-mass radius, from a 50 ks Chandra ACIS-S exposure. Three sources lie within the very small upper limit of 1.9" on the core radius. The brightest of the three core sources has a luminosity of L-X(0.5-6 keV) approximate to 6 x 10(32) ergs s(-1) and a blackbody-like soft X-ray spectrum, which are both consistent with it being a quiescent low-mass X-ray binary (qLMXB). We have identified optical counterparts to four of the six central sources and a number of the outlying sources, using deep Hubble Space Telescope and ground-based imaging. While the two proposed counterparts that lie within the core may represent chance superpositions, the two identified central sources that lie outside of the core have X- ray and optical properties consistent with being cataclysmic variables (CVs). Two additional sources outside of the core have possible active binary counterparts. We discuss the X-ray source population of M30 in light of its collapsed-core status. C1 Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lugger, PM (reprint author), Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. OI Heinke, Craig/0000-0003-3944-6109 NR 62 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2007 VL 657 IS 1 BP 286 EP 301 DI 10.1086/507572 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142FR UT WOS:000244635300023 ER PT J AU Cooper, RL Narayan, R AF Cooper, Randall L. Narayan, Ramesh TI The latitude of type I X-ray burst ignition on rapidly rotating neutron stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : neutron; X-rays : binaries; X-rays : bursts ID PHOTOSPHERIC RADIUS EXPANSION; THERMONUCLEAR RUNAWAYS; FREQUENCY EVOLUTION; SHELL FLASHES; RISING PHASE; OSCILLATIONS; PROPAGATION; DISCOVERY; MODEL; SUPERBURSTS AB We investigate the latitude at which type I X-ray bursts are ignited on rapidly rotating accreting neutron stars. We find that, for a wide range of accretion rates M, ignition occurs preferentially at the equator, in accord with the work of Spitkovsky et al. However, for a range of M below the critical M above which bursts cease, ignition occurs preferentially at higher latitudes. The range of M over which nonequatorial ignition occurs is an increasing function of the neutron star spin frequency. These findings have significant implications for thermonuclear flame propagation, and they may explain why oscillations during the burst rise are detected predominantly when the accretion rate is high. They also support the suggestion of Bhattacharyya & Strohmayer that non-photospheric radius expansion double-peaked bursts and the unusual harmonic content of oscillations during the rise of some bursts result from ignition at or near a rotational pole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cooper, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rcooper@cfa.harvard.edu; rnarayan@cfa.harvard.edu NR 47 TC 15 Z9 15 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2007 VL 657 IS 1 BP L29 EP L32 DI 10.1086/513077 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 142FU UT WOS:000244635600008 ER PT J AU Ribeiro, PD Christy, JH Rissanen, RJ Kim, TW AF Ribeiro, Pablo D. Christy, John H. Rissanen, Rebecca J. Kim, Tae Won TI Males are attracted by their own courtship signals (vol 61, pg 81, 2006) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Correction C1 Univ Mar del Plata, Dept Biol, RA-7600 Mar Del Plata, Argentina. Consejo Nacl Invest Cient & Tecn, Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina. Smithsonian Trop Res Inst, Naos Lab, Balboa, Ancon, Panama. Seoul Natl Univ, Sch Biol Sci, Lab Behav & Ecol, Seoul 151742, South Korea. RP Ribeiro, PD (reprint author), Univ Mar del Plata, Dept Biol, CC 573 Correo Cent, RA-7600 Mar Del Plata, Argentina. EM pdribeir@mdp.edu.ar NR 1 TC 0 Z9 0 U1 0 U2 1 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 MAR PY 2007 VL 61 IS 5 BP 823 EP 823 DI 10.1007/s00265-006-0318-6 PG 1 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 142XL UT WOS:000244684500018 ER PT J AU Logue, DM Droessler, EE Roscoe, DW Vokey, JR Rendall, D Kunimoto, RM AF Logue, David M. Droessler, Erika E. Roscoe, David W. Vokey, John R. Rendall, Drew Kunimoto, Robyn M. TI Sexually antithetical song structure in a duet singing wren SO BEHAVIOUR LA English DT Article DE Darwin's Principle of Antithesis; bird song; female song; acoustic adaptation hypothesis; sex differences; animal communication; signal evolution; Pheugopedius fasciatoventris ID BLACK-BELLIED WREN; MAGPIE-LARKS; WHITE WRENS; BEHAVIOR; BIRD; STRATEGIES; PLAYBACK; FEMALES; SIGNALS; SOUNDS AB Black-bellied wrens (Thryothorus fasciatoventris) use loud songs to communicate sex over long distances. We compared male and female songs recorded from a central Panamanian population of black-bellied wrens. All nine measured features differed significantly between the sexes. Males sang lower fundamental frequencies than females, but this difference cannot be explained by simple body size-frequency scaling. A discriminant function analysis correctly discriminated the singer's sex for all songs in the analysis. When viewed as sonograms, the terminal syllables of male and female songs exhibited opposite structure - all male songs ended in V-shaped syllables, and all female songs ended in arc-shaped syllables. The degree and character of dimorphism lead us to describe song structure in this population as 'sexually antithetical'. Variation in song dimorphism throughout this species' range provides an excellent opportunity to test the hypothesis that signal degradation during transmission selects for divergent signal structure. C1 Univ Lethbridge, Dept Biol Sci, Lethbridge, AB T1K 3M4, Canada. Smithsonian Trop Res Inst, Balboa, Panama. Univ Lethbridge, Dept Psychol, Lethbridge, AB T1K 3M4, Canada. RP Logue, DM (reprint author), Univ Lethbridge, Dept Biol Sci, 4401 Univ Dr W, Lethbridge, AB T1K 3M4, Canada. EM david.logue@uleth.ca NR 41 TC 11 Z9 11 U1 2 U2 6 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0005-7959 J9 BEHAVIOUR JI Behaviour PD MAR PY 2007 VL 144 BP 331 EP 350 DI 10.1163/156853907780425749 PN 3 PG 20 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 176PK UT WOS:000247097200005 ER PT J AU Buij, R McShea, WJ Campbell, P Lee, ME Dallmeier, F Guimondou, S Mackaga, L Guisseougou, N Mboumba, S Hines, JE Nichols, JD Alonso, A AF Buij, Ralph McShea, William J. Campbell, Patrick Lee, Michelle E. Dallmeier, Francisco Guimondou, Sylvain Mackaga, Loic Guisseougou, Nicaise Mboumba, Serge Hines, James E. Nichols, James D. Alonso, Alfonso TI Patch-occupancy models indicate human activity as major determinant of forest elephant Loxodonta cyclotis seasonal distribution in an industrial corridor in Gabon SO BIOLOGICAL CONSERVATION LA English DT Article DE elephants; Loxodonta cyclotis; Gabon; rainforest; oil industry; patch-occupancy ID ESTIMATING SITE OCCUPANCY; ESTIMATING DECAY-RATES; NATIONAL-PARK; AFRICAN ELEPHANTS; RAIN-FOREST; POPULATION; ABUNDANCE; MAMMALS; DUNG; CALLS AB The importance of human activity and ecological features in influencing African forest elephant ranging behaviour was investigated in the Rabi-Ndogo corridor of the Gamba Complex of Protected Areas in southwest Gabon. Locations in a wide geographical area with a range of environmental variables were selected for patch-occupancy surveys using elephant dung to assess seasonal presence and absence of elephants. Patch-occupancy procedures allowed for covariate modelling evaluating hypotheses for both occupancy in relation to human activity and ecological features, and detection probability in relation to vegetation density. The best fitting models for old and fresh dung data sets indicate that (1) detection probability for elephant dung is negatively related to the relative density of the vegetation, and (2) human activity, such as presence and infrastructure, are more closely associated with elephant distribution patterns than are ecological features, such as the presence of wetlands and preferred fresh fruit. Our findings emphasize the sensitivity of elephants to human disturbance, in this case infrastructure development associated with gas and oil production. Patch-occupancy methodology offers a viable alternative to current transect protocols for monitoring programs with multiple covariates. (c) 2006 Elsevier Ltd. All rights reserved. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Smithsonian Inst, Natl Zool Pk, Monitoring & Assessment Biodivers Program, Washington, DC 20560 USA. Gabon Biodivers Program, Gamba, Gabon. Minist Waters & Forestry, Wildlife & Hunting Dept, Libreville, Gabon. SCD Operat Loango, Iguela, Gabon. US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. RP Buij, R (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM rbuij@yahoo.com; mcsheaw@si.edu RI Buij, Ralph/M-4669-2013 NR 37 TC 21 Z9 23 U1 3 U2 25 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD MAR PY 2007 VL 135 IS 2 BP 189 EP 201 DI 10.1016/j.biocon.2006.10.028 PG 13 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 154FP UT WOS:000245492600004 ER PT J AU Eberhard, WG AF Eberhard, William G. TI Stabilimenta of Philoponella vicina (Araneae : Uloboridae) and Gasteracantha cancriformis (Araneae : Araneidae): Evidence against a prey attractant function SO BIOTROPICA LA English DT Article DE camouflage; non-orb webs; spider; stabilimentum function; uloborid; web advertisement ID FORAGING SUCCESS; SPIDERS ARANEAE; WEBS; DECORATIONS AB Both the uloborid Philoponella vicina and the araneid Gasteracantha cancriformis spiders sometimes placed silk stabilimenta on non-orb "resting webs" that consisted of only one or a few lines. These webs completely lacked sticky silk, so their stabilimenta could not function to attract prey. Some non-orbs were built by spiders when their orb webs are damaged. These observations contradict the prey attraction camouflage hypothesis for stabilimentum function, but are compatible with the spider camouflage and web advertisement to avoid web destruction hypotheses. 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 23 TC 9 Z9 9 U1 1 U2 8 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2007 VL 39 IS 2 BP 216 EP 220 DI 10.1111/j.1744-7429.2006.00254.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 134QI UT WOS:000244098300009 ER PT J AU Dietsch, TV Perfecto, I Greenberg, R AF Dietsch, Thomas V. Perfecto, Ivette Greenberg, Russell TI Avian foraging behavior in two different types of coffee agroecosystem in Chiapas, Mexico SO BIOTROPICA LA English DT Article DE floristic diversity; frugivory; insectivory; nectivory; Neotropics; seasonal variation; tropical agriculture ID FOLIAGE-GLEANING BIRDS; SHADE COFFEE; PLANTATIONS; BIODIVERSITY; POPULATIONS AB This study describes the foraging ecology of birds during summer and winter in two different types of coffee agroecosystems in Chiapas, Mexico. Avian foraging behavior is documented in two agroecosystems of differing management intensity, structurally similar but with different levels of floristic diversity, during summer and winter seasons. The distribution of tree species used by birds was more even, and birds used a greater diversity of tree species, in the more diverse coffee shade system. Much of the variation in resource use derived from shifts in the use of flowers and fruit, highlighting the importance in resource phenology for birds. Insectivory was more frequent in winter than summer for the coffee layer, and in summer for the shade layer. Given the vegetative structural similarity of the two coffee agroecosystems included in this study, floristic differences probably accounted for much of the difference in the bird communities between the management systems, especially given the strong seasonal response to flowering and fruiting. This work suggests that plentiful and diverse food resources associated with the high diversity of plant species may facilitate coexistence of the high number of bird species found in shade-grown coffee agroecosystems. C1 Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Dietsch, TV (reprint author), Univ Calif Los Angeles, Ctr Trop Res, Inst Environm, Box 951496, Los Angeles, CA 90095 USA. EM wilderth@ucla.edu NR 26 TC 18 Z9 18 U1 2 U2 19 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2007 VL 39 IS 2 BP 232 EP 240 DI 10.1111/j.1744-7429.2006.00248.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 134QI UT WOS:000244098300012 ER PT J AU Croes, BM Laurance, WF Lahm, SA Tchignoumba, L Alonso, A Lee, ME Campbell, P Buij, R AF Croes, Barbara M. Laurance, William F. Lahm, Sally A. Tchignoumba, Landry Alonso, Alfonso Lee, Michelle E. Campbell, Patrick Buij, Ralph TI The influence of hunting on antipredator behavior in central African monkeys and duikers SO BIOTROPICA LA English DT Article DE conservation; Gabon; hunting; rain forest ID TAI-NATIONAL-PARK; RED COLOBUS MONKEYS; GROUP-SIZE; ECOLOGICAL-CONSTRAINTS; POLYSPECIFIC ASSOCIATIONS; POPULATION-DENSITY; LEOPARD PREDATION; CROWNED EAGLES; SOCIAL-SYSTEMS; PRIMATE GROUPS AB Many animals can adjust their behavioral strategies to reduce predation risk. We investigated whether rain forest monkeys and duikers alter their antipredatory behavior in response to hunting by humans in southwestern Gabon. We compared monkey and duiker responses to human observers in an area where hunting is prohibited, to those in a nearby area where hunting pressure is moderate but spatially variable. The results of our study indicate that monkeys become more secretive when hunted, commencing alarm calls only when at a certain distance (typically > 50 m) from humans. We found no difference in monkey group size between hunted and no-hunting areas. In no-hunting areas, duikers often freeze in response to approaching observers, but in hunted areas they abandon this strategy and rapidly flee from humans. Duikers also whistle more often in areas where they are hunted frequently. Our findings have at least two important implications. First, behavioral observations of monkeys and duikers may be useful in gauging local hunting intensity in African rain forests. Second, duiker densities are likely to be overestimated in hunted areas, where they more readily flee and whistle, and underestimated in no-hunting areas, where they rely on freezing behavior to avoid detection. Because behavioral adaptations to hunting vary both among species and localities, these differences should be considered when attempting to derive population-density estimates for forest wildlife. C1 Leiden Univ, Inst Environm Sci CML, NL-2300 RA Leiden, Netherlands. Smithsonian Inst, Monitoring & Assessment Biodivers Program, Washington, DC 20013 USA. Smithsonian Trop Res Inst, Balboa, Panama. Inst Rech Ecol Trop, Makokou, Gabon. RP Croes, BM (reprint author), Leiden Univ, Inst Environm Sci CML, POB 9518, NL-2300 RA Leiden, Netherlands. EM croes_barbara@yahoo.com RI Laurance, William/B-2709-2012; Buij, Ralph/M-4669-2013 NR 70 TC 15 Z9 15 U1 2 U2 16 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2007 VL 39 IS 2 BP 257 EP 263 DI 10.1111/j.1744-7429.2006.00247.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 134QI UT WOS:000244098300015 ER PT J AU Griscom, HP Kalko, EKV Ashton, MS AF Griscom, Heather P. Kalko, Elisabeth K. V. Ashton, Mark S. TI Frugivory by small vertebrates within a deforested, dry tropical region of Central America SO BIOTROPICA LA English DT Article DE dry forest; fragmented; frugivores; live fences; Panama; pastures; reforestation; riparian forest; seed dispersal ID FRUIT-EATING BIRDS; SEED DISPERSAL; LOS-TUXTLAS; RAIN-FOREST; FRAGMENTED LANDSCAPE; SPECIES RICHNESS; ISOLATED TREES; PASTURES; MEXICO; BATS AB Small vertebrates were inventoried within three habitat types in a degraded dry forest region of Panama. Animals were classified as frugivorous if they were observed foraging on fruit or if fecal samples contained mostly or exclusively seeds. Overall, we found that eight bat species and 21 bird species consumed fruit. The greatest numbers of birds were observed within live fences and bird species richness was greatest within riparian forests. Bat assemblages were not significantly different between habitats. The implication is that ecosystem services such as seed dispersal may still be functional in this landscape. C1 Yale Univ, Sch Forestry & Environm Studies, PRORENA Program, New Haven, CT 06511 USA. Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Griscom, HP (reprint author), Yale Univ, Sch Forestry & Environm Studies, PRORENA Program, New Haven, CT 06511 USA. EM hgriscom@aya.yale.edu NR 45 TC 16 Z9 18 U1 2 U2 18 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2007 VL 39 IS 2 BP 278 EP 282 DI 10.1111/j.1744-729.2006.00242.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 134QI UT WOS:000244098300019 ER PT J AU McCann, LD Hitchcock, NG Winston, JE Ruiz, GM AF McCann, Linda D. Hitchcock, Natasha Gray Winston, Judith E. Ruiz, Gregory M. TI Non-native bryozoans in coastal embayments of the Southern United States: New records for the western Atlantic SO BULLETIN OF MARINE SCIENCE LA English DT Review ID GULF-OF-MEXICO; INDIAN RIVER LAGOON; BOMBAY WATERS; CHEILOSTOME BRYOZOANS; BIOLOGICAL INVASIONS; NORTH-AMERICA; PERNA-VIRIDIS; GREEN MUSSEL; NEW-ZEALAND; FLORIDA AB Bryozoans are among the most common fouling organisms in coastal marine environments around the world, yet their distribution in many coastal areas is not well known. We surveyed the bryozoans in shallow coastal estuaries in the southern United States, focusing on Texas and Florida. We deployed settlement plates across six different estuaries at 61 sites. Thirty-five species of bryozoans were identified, including four non-native species described here for the first time from the United States: Hippoporina indica (Pillai, 1978), Electra bengalensis (Stoliczka, 1869), Sinoflustra annae (Osburn, 1953), and Celleporaria pilaefera (Canu and Bassler, 1929). At all six estuaries, non-native species were among the most common bryozoans. Hippoporina indica was the most abundant bryozoan, occurring in all estuaries sampled. In Jacksonville, Florida, E. bengalensis and S. annae dominated both the numbers and biomass of bryozoans. All four species have probable Indo-West Pacific origins. A literature-based analysis identified 39 additional non-native species of marine invertebrates and algae already established in the region, and over half are considered to have an Indo-West Pacific origin. Ships from Asia are regular visitors to Florida and the Gulf of Mexico, providing a possible mechanism of introduction for the non-native bryozoans. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Virginia Museum Nat Hist, Martinsville, VA 24112 USA. RP McCann, LD (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM mc-cannl@si.edu OI Ruiz, Gregory/0000-0003-2499-441X NR 110 TC 11 Z9 12 U1 0 U2 9 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD MAR PY 2007 VL 80 IS 2 BP 319 EP 342 PG 24 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 161WE UT WOS:000246046400003 ER PT J AU Venzke, E AF Venzke, Edward TI Smithsonian Institution's Global Volcanism Network SO BULLETIN OF VOLCANOLOGY LA English DT Article AB Information included in this summary is based on more detailed reports published in the Bulletin of the Global Volcanism Network, vol. 31, no. 6, June 2006 (on the Internet at http://www.volcano.si.edu/). Edited by scientists at the Smithsonian, this bulletin includes reports provided by a worldwide network of correspondents. The reports contain the names and contact information for all sources. Please note that these reports are preliminary and subject to change as events are studied in more detail. The Global Volcanism Program welcomes further reports of current volcanism, seismic unrest, monitoring data, and field observations. C1 Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Program, Washington, DC 20013 USA. RP Venzke, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Program, MRC 119,POB 37012, Washington, DC 20013 USA. EM gvp@si.edu NR 0 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0258-8900 J9 B VOLCANOL JI Bull. Volcanol. PD MAR PY 2007 VL 69 IS 5 BP 577 EP 579 DI 10.1007/s00445-006-0095-0 PG 3 WC Geosciences, Multidisciplinary SC Geology GA 137OZ UT WOS:000244303200007 ER PT J AU Herre, EA Mejia, LC Kyllo, DA Rojas, E Maynard, Z Butler, A Van Bael, SA AF Herre, Edward Allen Mejia, Luis C. Kyllo, Damond A. Rojas, Enith Maynard, Zuleyka Butler, Andre Van Bael, Sunshine A. TI Ecological implications of anti-pathogen effects of tropical fungal endophytes and mycorrhizae SO ECOLOGY LA English DT Article DE arbuscular mycorrhizal fungi; endophytic fungi; mutualism; pathogens; plant defense; Theobroma cacao; tropical plant ecology ID ARBUSCULAR MYCORRHIZAE; RAIN-FOREST; PUERTO-RICO; DIVERSITY; LEAVES; COMMUNITIES; GROWTH; TREE; PLANTS; COLONIZATION AB We discuss studies of foliar endophytic fungi (FEF) and arbuscular mycorrhizal fungi (AMF) associated with Theobroma cacao in Panama. Direct, experimentally controlled comparisons of endophyte free (E-) and endophyte containing (E+) plant tissues in T. cacao show that foliar endophytes ( FEF) that commonly occur in healthy host leaves enhance host defenses against foliar damage due to the pathogen ( Phytophthora palmivora). Similarly, root inoculations with commonly occurring AMF also reduce foliar damage due to the same pathogen. These results suggest that endophytic fungi can play a potentially important mutualistic role by augmenting host defensive responses against pathogens. There are two broad classes of potential mechanisms by which endophytes could contribute to host protection: (1) inducing or increasing the expression of intrinsic host defense mechanisms and (2) providing additional sources of defense, extrinsic to those of the host ( e. g., endophyte-based chemical antibiosis). The degree to which either of these mechanisms predominates holds distinct consequences for the evolutionary ecology of host-endophyte-pathogen relationships. More generally, the growing recognition that plants are composed of a mosaic of plant and fungal tissues holds a series of implications for the study of plant defense, physiology, and genetics. C1 Smithsonian Trop Res Inst, Miami, FL 34002 USA. Rutgers State Univ, Dept Plant Biol & Pathol, New Brunswick, NJ 08901 USA. RP Herre, EA (reprint author), Smithsonian Trop Res Inst, APO AA,Unit 0948, Miami, FL 34002 USA. EM HERREA@si.edu NR 85 TC 101 Z9 122 U1 8 U2 73 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 MAR PY 2007 VL 88 IS 3 BP 550 EP 558 DI 10.1890/05-1606 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 156SB UT WOS:000245668500003 PM 17503581 ER PT J AU Gilbert, GS Reynolds, DR Bethancourt, A AF Gilbert, Gregory S. Reynolds, Don R. Bethancourt, Ariadna TI The patchiness of epifoliar fungi in tropical forests: Host range, host abundance, and environment SO ECOLOGY LA English DT Article DE canopy access cranes; Cleistanthus myrianthus; epiphyll; phyloecology; plant-fungus symbiosis; Queensland Australia; San Lorenzo Panama; tropical rainforest canopy ID RAIN-FOREST; EVOLUTIONARY ECOLOGY; TREE; COLONIZATION; ENDOPHYTES; DIVERSITY; DISEASE; PLANTS; LIGHT; CLASSIFICATION AB Fungal symbioses affect the diversity, dynamics, and spatial patterns of trees in tropical forests. Their ecological importance is partly driven by their inherent patchiness. We used epifoliar fungi, a guild of common, benign, obligate, fungal symbionts of plants, as a model system to evaluate the relative importance of host phylogeny, host relative abundance, and microclimate on the three-dimensional distribution of plant-fungus symbioses. In parallel studies in rainforests in Panama and Australia, most epifoliar fungi were able to colonize several plant lineages but showed significant host preferences within the local plant community. More closely related plant species were not more likely to share fungal symbionts. Instead, fungal species were more likely to be shared by more abundant hosts, which supported a greater number and diversity of fungi. Environmental conditions strongly affected spatial distributions, with sites in the dark understory 2.5- to fourfold more likely to have epifoliar fungi than in the exposed forest canopy. In the understory, fungal incidence increased with canopy openness. Canopy trees supported only a subset of the fungal symbionts found in the understory, suggesting that adult trees are not reservoirs of these fungal symbionts for understory juveniles. C1 Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Panama. Museum Nat Hist, Los Angeles, CA 90007 USA. Univ Panama, Dept Microbiol, Panama City, Panama. RP Gilbert, GS (reprint author), Univ Calif Santa Cruz, 1156 High St, Santa Cruz, CA 95064 USA. EM ggilbert@ucsc.edu RI Gilbert, Gregory/C-2595-2008 NR 42 TC 28 Z9 30 U1 0 U2 16 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 MAR PY 2007 VL 88 IS 3 BP 575 EP 581 DI 10.1890/05-1170 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 156SB UT WOS:000245668500006 PM 17503584 ER PT J AU Gallery, RE Dalling, JW Arnold, AE AF Gallery, Rachel E. Dalling, James W. Arnold, A. Elizabeth TI Diversity, host affinity, and distribution of seed-infecting fungi: A case study with Cecropia SO ECOLOGY LA English DT Article DE Ascomycota; Cecropia; diversity; fungi; ITS; pioneer species; tropical forest; recruitment limitation; richness ID RAIN-FOREST; RECRUITMENT LIMITATION; TROPICAL FOREST; SOIL FUNGI; TREE; DISPERSAL; PATHOGENS; SURVIVAL; DISTANCE; PLANTS AB Recruitment limitation has been proposed as an important mechanism contributing to the maintenance of tropical tree diversity. For pioneer species, infection by fungi significantly reduces seed survival in soil, potentially influencing both recruitment success and adult distributions. We examined fresh seeds of four sympatric Cecropia species for evidence of fungal infection, buried seeds for five months in common gardens below four C. insignis crowns in central Panama, and measured seed survival and fungal infection of inviable seeds. Seed survival varied significantly among species and burial sites, and with regard to local ( Panama) vs. foreign ( Costa Rica) maternal seed sources. Fresh seeds contained few cultivable fungi, but > 80% of soil-incubated seeds were infected by diverse Ascomycota, including putative pathogens, saprophytes, and endophytes. From 220 isolates sequenced for the nuclear internal transcribed spacer region ( ITS), 26 of 73 unique genotypes were encountered more than once. Based on the most common genotypes, fungal communities demonstrate host affinity and are structured at the scale of individual crowns. Similarity among fungal communities beneath a given crown was significantly greater than similarity among isolates found under different crowns. However, the frequency of rare species suggests high fungal diversity and fine-scale spatial heterogeneity. These results reveal complex plant fungal interactions in soil and provide a first indication of how seed survival in tropical forests may be affected by fungal community composition. C1 Univ Illinois, Program Ecol & Evolut Biol, Urbana, IL 61801 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Arizona, Dept Plant Sci, Div Plant Pathol & Microbiol, Tucson, AZ 85721 USA. RP Gallery, RE (reprint author), Univ Illinois, Program Ecol & Evolut Biol, Urbana, IL 61801 USA. EM rachel.gallery@gmail.com NR 34 TC 47 Z9 52 U1 0 U2 38 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 MAR PY 2007 VL 88 IS 3 BP 582 EP 588 DI 10.1890/05-1207 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 156SB UT WOS:000245668500007 PM 17503585 ER PT J AU Tzortziou, M Subramaniam, A Herman, JR Gallegos, CL Neale, PJ Harding, LW AF Tzortziou, Maria Subramaniam, Ajit Herman, Jay R. Gallegos, Charles L. Neale, Patrick J. Harding, Lawrence W., Jr. TI Remote sensing reflectance and inherent optical properties in the mid Chesapeake Bay SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE bio-optics; satellite retrievals; Case 2; estuaries; coastal waters ID DISSOLVED ORGANIC-MATTER; BULK REFRACTIVE-INDEX; CASE 2 WATERS; CHLOROPHYLL-A; OCEAN COLOR; COASTAL WATERS; BIDIRECTIONAL REFLECTANCE; ABSORPTION-COEFFICIENTS; NATURAL PHYTOPLANKTON; DIFFUSE-REFLECTANCE AB We used an extensive set of bio-optical data to examine the relationships between inherent optical properties and remotely sensed quantities in an optically complex and biologically productive region of the Chesapeake Bay. Field observations showed that the chlorophyll algorithms used by the MODIS (MODerate resolution Imaging Spectroradiometer) ocean color sensor (i.e. Chlor_a, chlor_MODIS, chlor_a_3 products) do not perform accurately in these Case 2 waters. This is because, at high concentrations of chlorophyll, all MODIS algorithms are based on empirical relationships between chlorophyll concentration and blue:green wavelength remote sensing reflectance (R(rs)) ratios that do not account for the typically strong blue-wavelength absorption by non-covarying, dissolved and non-algal particulate components. We found stronger correlation between chlorophyll concentration and red:green R(rs) ratios (i.e. R(rs)(677)/R(rs)(554)). Regionally-specific algorithms that are based on the phytoplankton optical properties in the red wavelength region provide a better basis for satellite monitoring of phytoplankton blooms in these Case 2 waters. Our estimates of f/Q (proportionality factor in the relationship between R(rs) and the ratio of water backscattering, b(b), and absorption, a, coefficients, b(b)/(a + b(b))) were not considerably different from f/Q previously estimated for same measurement geometry but Case 1 waters. Variation in surface bb significantly affected R(rs) magnitude across the visible spectrum and was most strongly correlated (R(2) = 0.88) with observed variability in R(rs) at 670 nm. Surface values of particulate backscattering were strongly correlated with non-algal particulate absorption, a(nap) (R(2) = 0.83). These results, along with the measured backscattering fraction and non-algal particulate absorption spectral slope, indicate that suspended non-algal particles with high inorganic content are the major water constituents regulating b(b) variability in the studied region of the Chesapeake Bay. Remote retrieval of surface a(nap) from R(rs)(670) could be used in conjunction with inversion of UV-blue wavelengths to separate contribution by non-algal particles and colored dissolved organic matter to total light absorption, and monitor non-algal suspended particle concentration and distribution in these Case 2 waters. (c) 2006 Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Ctr Environm Sci, Horn Point Lab, Cambridge, MD 21613 USA. RP Tzortziou, M (reprint author), NASA, Goddard Space Flight Ctr, Code 613-3,Bldg 33, Greenbelt, MD 20771 USA. EM martz@code613-3.gsfc.nasa.gov RI Neale, Patrick/A-3683-2012; OI Subramaniam, Ajit/0000-0003-1316-5827; Gallegos, Charles/0000-0001-5112-0166; Herman, Jay/0000-0002-9146-1632 NR 83 TC 63 Z9 68 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 MAR PY 2007 VL 72 IS 1-2 BP 16 EP 32 DI 10.1016/j.ecss.2006.09.018 PG 17 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 145JZ UT WOS:000244862400002 ER PT J AU Hilton, EJ Johnson, GD AF Hilton, Eric J. Johnson, G. David TI When two equals three: developmental osteology and homology of the caudal skeleton in carangid fishes (Perciformes : Carangidae) SO EVOLUTION & DEVELOPMENT LA English DT Article ID SYSTEMATICS; PISCES; FINS; MORPHOLOGY; SCOMBRIDAE; ONTOGENY; LARVAE; BONE AB Ontogeny often provides the most compelling evidence for primary homology in evolutionary developmental studies and is critical to interpreting complex structures in a phylogenetic context. As an example of this, we document the ontogenetic development of the caudal skeleton of Caranx crysos by examining a series of cleared and stained larval and postlarval specimens. By studying ontogeny, we are able to more accurately identify some elements of the adult caudal skeleton than is possible when studying the adult stage alone. The presence of two epurals has been used as a synapomorphy of Caranginae (homoplastically present in the scomberoidine genera Scomberoides and Oligoplites). Here we find that three epurals (ep) are present in larvae and small postlarval juveniles (i.e.,< 25 mm standard length [SL]) of C. crysos and other carangines, but ep2 never ossifies and does not develop beyond its initial presence. Ep2 was last observed in a 33.6 mm SL specimen as a small nodule of very lightly stained cartilage cells and eventually disappears completely. Therefore, the two epurals present in the adult are ep1 and ep3. In other carangines examined (e.g., Selene, Selar), the rudimentary ep2 ossifies and appears to fuse to the proximal tip of ep1. In these taxa, therefore, the two epurals of the adult appear to be ep1+2 and ep3. We found no indication of three epurals at any stage in the development of Oligoplites (developmental material of Scomberoides was unavailable). We discuss the osteology of the caudal skeleton of carangoid fishes generally and emphasize the power and importance of ontogeny in the identification of primary homology. C1 Smithsonian Inst, Div Fishes, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Hilton, EJ (reprint author), Field Museum Nat Hist, Dept Geol, 1400 S Lake Dr, Chicago, IL 60605 USA. EM ehilton@fieldmuseum.org NR 51 TC 16 Z9 20 U1 0 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1520-541X J9 EVOL DEV JI Evol. Dev. PD MAR-APR PY 2007 VL 9 IS 2 BP 178 EP 189 PG 12 WC Evolutionary Biology; Developmental Biology; Genetics & Heredity SC Evolutionary Biology; Developmental Biology; Genetics & Heredity GA 146OA UT WOS:000244942700007 PM 17371400 ER PT J AU Constantino, P Wood, B AF Constantino, Paul Wood, Bernard TI The evolution of Zinjanthropus boisei SO EVOLUTIONARY ANTHROPOLOGY LA English DT Article DE Paranthropus; Australopithecus; Olduvai Gorge; Koobi Fora; cranial morphology ID PLIO-PLEISTOCENE HOMINIDS; AUSTRALOPITHECUS-BOISEI; FOSSIL HOMINIDS; SOUTH-AFRICA; PARANTHROPUS-BOISEI; SEXUAL-DIMORPHISM; OLDUVAI-GORGE; LAKE TURKANA; BODY-MASS; NORTHERN KENYA AB Many people assume that OH 5, the type specimen of Paranthropus boisei, collected in 1959, was the first evidence of that taxon to be found, but OH 3, recovered in 1955, predated the discovery of OH 5 by four years. Thus, Paranthropus boisei recently celebrated the equivalent of its fiftieth birthday. This review marks that milestone by examining the way our understanding of this taxon has changed during its fifty, or so, year history. C1 George Washington Univ, Dept Anthropol, Hominid Paleobiol Program, Washington, DC 20052 USA. Smithsonian Inst, Museum Natl Hist Nat, Human Origins Program, Washington, DC 20560 USA. RP Constantino, P (reprint author), George Washington Univ, Dept Anthropol, Hominid Paleobiol Program, 2110 G St NW, Washington, DC 20052 USA. EM pcma@gwu.edu; bernardawood@gmail.com OI Constantino, Paul/0000-0003-3397-7961 NR 99 TC 17 Z9 18 U1 2 U2 17 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1060-1538 J9 EVOL ANTHROPOL JI Evol. Anthropol. PD MAR-APR PY 2007 VL 16 IS 2 BP 49 EP 62 DI 10.1002/evan.20130 PG 14 WC Anthropology SC Anthropology GA 164DO UT WOS:000246213500003 ER PT J AU Briceno, D Eberhard, W Shelly, T AF Briceno, Daniel Eberhard, William Shelly, Todd TI Male courtship behavior in Ceratitis capitata (Diptera : Tephritidae) that have received aromatherapy with ginger root oil SO FLORIDA ENTOMOLOGIST LA English DT Article DE aromatherapy; Ceratitis capitata; close range pheromones; mating behavior; Mediterranean fruit fly; sexual selection ID MEDITERRANEAN FRUIT-FLIES; ENHANCES MATING SUCCESS; MASS-REARED MALES; MEDFLIES DIPTERA; FLY DIPTERA; WILD; TRIMEDLURE; EXPOSURE; CRITERIA AB The results of previous studies that showed that exposing mass-reared male Mediterranean fruit flies Ceratitis capitata (Wiedemann) to ginger root oil ("aromatherapy") increases the likelihood of mating with wild females were confirmed. The increased male success could be due to female responses to changes in male behavior or male pheromones. There were no significant differences in the types of courtship movements executed by males with and without aromatherapy. The durations of movements also did not differ when mass-reared males were paired with mass-reared females; however, when they were paired with wild females, there were a few, small differences. Previous studies indicated that the effectiveness of the male long-distance attractant pheromone is not affected by aromatherapy, but these studies did not consider pheromones released at close range during courtship, which behavioral analyses suggest may be different. We propose the following possible explanation for the different effects of aromatherapy with different females. Selection on males under mass rearing may have altered their close-range pheromones in ways that can be remedied by aromatherapy; and only wild females respond because the pheromonal responsiveness of mass-reared females has also changed. We propose observations that could test these ideas. C1 Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Smithsonian Trop Res Inst, Balboa, Panama. USDA, APHIS, CPHST, Waimanalo, HI 96795 USA. RP Briceno, D (reprint author), Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. NR 17 TC 6 Z9 6 U1 1 U2 3 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD MAR PY 2007 VL 90 IS 1 BP 175 EP 179 DI 10.1653/0015-4040(2007)90[175:MCBICC]2.0.CO;2 PG 5 WC Entomology SC Entomology GA 155RK UT WOS:000245595400024 ER PT J AU Hershler, R Liu, HP Lang, BK AF Hershler, Robert Liu, Hsiu-Ping Lang, B. K. TI Genetic and morphologic variation of the Pecos assiminea, an endangered mollusk of the Rio Grande region, United States and Mexico (Caenogastropoda : Rissooidea : Assimineidae) SO HYDROBIOLOGIA LA English DT Article DE assiminea; gastropoda; North America; systematics; biogeography; conservation ID MITOCHONDRIAL-DNA; RECENT SPECIATION; GASTROPODA; HYDROBIIDAE; DIVERGENCE; HISTORY; ORIOLE; BASIN; TAXA AB Assiminea pecos is an endangered species of amphibious gastropod that occupies four widely separated portions of the Rio Grande region in the southwestern United States (Pecos River basin) and northeastern Mexico (Cuatro Cienegas basin). Our statistical and discriminant function analyses of shell variation among the disjunct populations of this species indicate that Mexican specimens differ in their morphometry from those of the United States and can be diagnosed by several characters. We also analyzed variation in the mitochondrial genome by sequencing 658 bp of mitochondrial COI from populations of A. pecos, representatives of the other three North American species of Assiminea, and several outgroups. Our results indicated substantial divergence of the Mexican population of A. pecos, which was consistently depicted as a monophyletic unit nested within or sister to the shallowly structured group comprised of American members of this species. Consistent with our findings, we describe the Mexican population as a new species, which is provisionally placed in the large, worldwide genus Assiminea pending further study of the phylogentic relationships of the North American assimineids. Our molecular data suggest that the Rio Grande region assimineids, which are among the few inland members of the otherwise estuarine subfamily Assimineinae, diverged from coastal progenitors in the late Miocene, with subsequent Pleistocene vicariance of Mexican and American species perhaps associated with development of the modern, lower course of the Rio Grande. C1 Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. New Mexico Dept Game & Fish, Santa Fe, NM 87507 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, NHB W-305,MRC 163,POB 37012, Washington, DC 20013 USA. EM hershlerr@si.edu NR 42 TC 8 Z9 9 U1 3 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD MAR PY 2007 VL 579 BP 317 EP 335 DI 10.1007/s10750-006-0473-9 PG 19 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 135XM UT WOS:000244187200026 ER PT J AU Crouch, TD AF Crouch, Tom D. TI Testing the limits: Aviation medicine and the origins of manned space flight. SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Crouch, TD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD MAR PY 2007 VL 93 IS 4 BP 1301 EP 1301 PG 1 WC History SC History GA 193AL UT WOS:000248245400132 ER PT J AU Liu, HP Hershler, R AF Liu, Hsiu-Ping Hershler, Robert TI A test of the vicariance hypothesis of western North American freshwater biogeography SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE conservation biogeography; dispersal; Gastropoda; Great Basin; mtDNA; phylogeography; springsnails; vicariance; western North America ID MACROBRACHIUM-AUSTRALIENSE DECAPODA; MITOCHONDRIAL-DNA SEQUENCES; POPULATION-STRUCTURE; NYMPHOPHILINE GASTROPODS; PHENOTYPIC ASSOCIATIONS; CLADISTIC-ANALYSIS; RIVER-BASIN; QUEENSLAND; CALIFORNIA; PATTERNS AB Aim The biogeography of western North American freshwater molluscs has traditionally been attributed to vicariance associated with late Tertiary rearrangement of landscape based on distributional evidence and the putatively limited dispersal ability of these organisms. We examined the phylogeography of a widely ranging western springsnail (Pyrgulopsis wongi Hershler, 1989) to test this hypothesis and evaluate the relative importance of vicariance and dispersal in structuring the distribution of this species. Location Southwestern Great Basin (California and Nevada), United States of America. Methods Two mitochondrial genes (COI, NDI) were sequenced for 28 populations of P. wongi spanning its entire geographic range, which consists of 10 topographically closed drainage basins. We also sequenced eight closely related congeners, as well as the type species of the closely related eastern North American genus Floridobia Hershler & Thompson, 2002, which was used as the outgroup. Phylogenies based on the combined data set were obtained using several methods, and networks for each gene were generated as an additional means of examining relationships among haplotypes. Partitioning of haplotype variation was studied using AMOVA, migration between populations was estimated using a coalescent-based method (MDIV), and divergence times were inferred using a locally calibrated molecular clock and MDIV. Results Pyrgulopsis wongi is subdivided into narrowly localized and widely distributed lineages that diverged in the Pleistocene, well after the inception of the contemporary regional landscape. While large Phi(ST) values and the localized geographic distributions of most haplotypes imply absence or negligible contemporary dispersal of this spring-dwelling snail, the pattern of phylogeographic structuring, presence of a few widespread haplotypes, and results of the MDIV analyses suggest geologically recent dispersal across drainage divides. Main Conclusions Phylogeography of P. wongi conflicts with the traditional vicariance model as it is not structured by the contemporary landscape and is instead indicative of geologically recent dispersal. In the absence of evidence that dispersal of this species occurred through surface water connections during the relevant (Quaternary) time frame, we conjecture that spread may have instead been mediated by transport on waterfowl or via upland stream capture. The non-concordance between phylogeography and landscape reported in this and other recent studies of Pyrgulopsis suggests that members of this diverse and imperiled genus should not be managed using an a priori, 'watershed as conservation unit' approach. 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 hershlerr@si.edu NR 65 TC 20 Z9 20 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD MAR PY 2007 VL 34 IS 3 BP 534 EP 548 DI 10.1111/j.1365-2699.2006.01611.x PG 15 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 134WA UT WOS:000244113900015 ER PT J AU Martrille, L Ubelaker, DH Cattaneo, C Seguret, F Tremblay, M Baccino, E AF Martrille, Laurent Ubelaker, Douglas H. Cattaneo, Cristina Seguret, Fabienne Tremblay, Marie Baccino, Eric TI Comparison of four skeletal methods for the estimation of age at death on white and black adults SO JOURNAL OF FORENSIC SCIENCES LA English DT Article; Proceedings Paper CT 57th Annual Meeting of the American-Academy-of-Forensic-Sciences CY FEB 21-26, 2005 CL New Orleans, LA SP Amer Acad Forens Sci DE forensic science; aging; ribs; pubic symphysis; teeth; auricular surface ID AURICULAR SURFACE; PHASE-ANALYSIS; STERNAL RIB; AT-DEATH; OS PUBIS; FEMALES; SAMPLE; MALES; ILIUM; END AB When analyzing human adult skeletal remains, it is often difficult to decide whether a single aging method will give a more reliable age estimation than a combination of methods. This study evaluates four macroscopic indicators for age estimation on 218 American White and Black individuals, ranging in age from 25 to 90 years of age, from the Terry collection. Individuals in the sample were selected to have a balanced race, sex, and age distribution. The following aging methods were applied to each skeleton by one experienced observer: the Suchey-Brooks (SB) pubic symphysis method, the Lovejoy auricular surface method, the monoradicular teeth Lamendin (LM) method, and the Iscan (IC) method for fourth ribs. The statistical study involved the evaluation of inaccuracy and bias (based on median age) for each age indicator and the combination of methods using Principal component analysis (PCA). Analysis was performed on the entire sample, then by race, then sex, and then age group (25-40 years, 41-60 years, and > 60 years). PCA was the most accurate method for both racial groups when all age groups are analyzed together. When the sample was divided into age groups, SB was the most accurate for young adults (25-40 years) and LM was the most accurate for middle adults (41-60 years). After the age of 60, all methods are highly inaccurate, although IC gives the lowest inaccuracy. As regards bias, the study highlights the tendency of all methods to overestimate the age of young individuals and to underestimate in the older age group. No single skeletal indicator of age at death is ever likely to reflect accurately the many factors that accumulate with chronological age. In fact, one must use as many dental and skeletal indicators as possible. However, in order to maximize the potential of each method, in the final evaluation one should consider mainly the method or methods that have a higher accuracy for a particular age range. C1 Univ Montpellier, Ctr Hosp, Hop Lapeyronie, Serv Med Legale, F-34295 Montpellier 5, France. Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. Univ Milan, Ist Med Legale, I-20133 Milan, Italy. Ctr Hosp Univ, DIM, Montpellier, France. RP Martrille, L (reprint author), Univ Montpellier, Ctr Hosp, Hop Lapeyronie, Serv Med Legale, 191 Ave Doyen Gaston Giraud, F-34295 Montpellier 5, France. EM l-martrille@chu-montpellier.fr RI Cattaneo, Cristina/M-2671-2016 OI Cattaneo, Cristina/0000-0003-0086-029X NR 28 TC 56 Z9 59 U1 3 U2 28 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD MAR PY 2007 VL 52 IS 2 BP 302 EP 307 DI 10.1111/j.1556-4029.2006.00367.x PG 6 WC Medicine, Legal SC Legal Medicine GA 138DJ UT WOS:000244343000007 PM 17316225 ER PT J AU Lidberg, M Johansson, JM Scherneck, HG Davis, JL AF Lidberg, Martin Johansson, Jan M. Scherneck, Hans-Georg Davis, James L. TI An improved and extended GPS-derived 3D velocity field of the glacial isostatic adjustment (GIA) in Fennoscandia SO JOURNAL OF GEODESY LA English DT Article DE glacial isostatic adjustment (GIA); postglacial rebound (PGR); Global Positioning System (GPS); terrestrial reference frame (TRF); ITRF2000; GAMIT; GLOBK software; Fennoscandia ID COORDINATE TIME-SERIES; SEA-LEVEL CHANGE; EARTH; CONSTRAINTS; ITRF2000; MODELS; IMPACT; UPLIFT; NOISE AB We present a new GPS-derived 3D velocity field for the Fennoscandia glacial isostatic adjustment (GIA) area. This new solution is based upon similar to 3,000 days of continuous GPS observations obtained from the permanent networks in Fennoscandia. The period encompasses a prolongated phase of stable observation conditions after the northern autumn of 1996. Several significant improvements have led to smaller uncertainties and lower systematic errors in the new solutions compared to our previous results. The GPS satellite elevation cut-off angle was lowered to 10 degrees, we fixed ambiguities to integers where possible, and only a few hardware changes occurred over the entire network. The GAMIT/GLOBK software package was used for the GPS analysis and reference frame realization. Our new results confirmed earlier findings of maximum discrepancies between GIA models and observations in northern Finland. The reason may be related to overestimated ice-sheet thickness and glaciation period in the north. In general, the new solutions are more coherent in the velocity field, as some of the perturbations are now avoided. We compared GPS-derived GIA rates with sea-level rates from tide-gauge observations, repeated precise leveling, and with GIA model computations, which showed consistency. C1 Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lidberg, M (reprint author), Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. EM lidberg@oso.chalmers.se RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 42 TC 68 Z9 69 U1 3 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD MAR PY 2007 VL 81 IS 3 BP 213 EP 230 DI 10.1007/s00190-006-0102-4 PG 18 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 154GY UT WOS:000245496100004 ER PT J AU Patenaude, NJ Portway, VA Schaeff, CM Bannister, JL Best, PB Payne, RS Rowntree, VJ Rivarola, M Baker, CS AF Patenaude, Nathalie J. Portway, Vicky A. Schaeff, Cathy M. Bannister, John L. Best, Peter B. Payne, Roger S. Rowntree, Vicky J. Rivarola, Mariana Baker, C. Scott TI Mitochondrial DNA diversity and population structure among southern right whales (Eubalaena australis) SO JOURNAL OF HEREDITY LA English DT Article ID ATLANTIC RIGHT WHALES; STATISTICAL TESTS; DIFFERENTIATION; POLYMORPHISM; CETACEANS; GENETICS; NORTH AB The population structure and mitochondrial (mt) DNA diversity of southern right whales (Eubalaena australis) are described from 146 individuals sampled on 4 winter calving grounds (Argentina, South Africa, Western Australia, and the New Zealand sub-Antarctic) and 2 summer feeding grounds (South Georgia and south of Western Australia). Based on a consensus region of 275 base pairs of the mtDNA control region, 37 variable sites defined 37 unique haplotypes, of which only one was shared between regional samples of the Indo-Pacific and South Atlantic Oceans. Phylogenetic reconstruction of the southern right whale haplotypes revealed 2 distinct clades that differed significantly in frequencies between oceans. An analysis of molecular variance confirmed significant overall differentiation among the 4 calving grounds at both the haplotype and the nucleotype levels (F-ST = 0.159; Phi(ST) = 0.238; P < 0.001). Haplotype diversity was significantly lower in the Indo-Pacific (h = 0.701 +/- 0.037) compared with the South Atlantic (h = 0.948 +/- 0.013), despite a longer history of exploitation and larger catches in the South Atlantic. In fact, the haplotype diversity in the Indo-Pacific basin was similar to that of the North Atlantic right whale that currently numbers about 300 animals. Multidimensional scaling of genetic differentiation suggests that gene flow occurred primarily between adjacent calving grounds within an ocean basin, with mixing of lineages from different calving grounds occurring on feeding grounds. C1 Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand. Smithsonian Inst, Mol Genet Lab, Washington, DC 20560 USA. American Univ, Dept Biol, Washington, DC 20006 USA. Western Australian Museum, Perth, WA 6000, Australia. Univ Pretoria, Mammal Res Inst, ZA-0002 Pretoria, South Africa. Whale Conservat Inst, Lincoln, MA 01733 USA. Fundac Patagonia Natl, RA-9120 Madryn, Argentina. Oregon State Univ, Hatfield Marine Sci Ctr, Marine Mammal Program, Newport, OR 97365 USA. RP Baker, CS (reprint author), Univ Auckland, Sch Biol Sci, Private Bag 92019, Auckland 1, New Zealand. EM scott.baker@oregonstate.edu OI Schaeff, Catherine/0000-0003-3728-9402 NR 57 TC 33 Z9 36 U1 2 U2 25 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-1503 J9 J HERED JI J. Hered. PD MAR PY 2007 VL 98 IS 2 BP 147 EP 157 DI 10.1093/jhered/esm005 PG 11 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 162XO UT WOS:000246123000008 PM 17416933 ER PT J AU Harrington, GJ Jaramillo, CA AF Harrington, Guy J. Jaramillo, Carlos A. TI Paratropical floral extinction in the Late Palaeocene-Early Eocene SO JOURNAL OF THE GEOLOGICAL SOCIETY LA English DT Article ID NORTHERN SOUTH-AMERICA; US GULF-COAST; THERMAL MAXIMUM; TROPICAL FORESTS; BIGHORN BASIN; TAXONOMIC DIVERSITY; VEGETATION DYNAMICS; SPECIES RICHNESS; CLIMATE CHANGES; OXYGEN-ISOTOPE AB The Palaeocene-Eocene Thermal Maximum (PETM) at c. 55.8 Ma marks a transient (c. 100 ka duration) interval of rapid greenhouse warming that had profound effects on marine and terrestrial biota. Plant communities responded rapidly with major compositional turnover. The long-term effects on tropical vegetation communities that stein from the brief period of global warming are unclear. We present pollen data from the paratropical US Gulf Coast (eastern Mississippi, western Alabama and Georgia), which had background Palacogene mean annual temperatures of 26-27 degrees C. Sporomorph data (pollen and spores) demonstrate that taxonomic diversity increases over c. 1 Ma in the Late Palaeocene but this trend is replaced, with the first occurrences of taxa that mark the Early Eocene, by a pronounced extinction into the Early Eocene (c. 20% of the palynoflora). Taxonomic diversity also decreases by up to 38% in the Early Eocene. The timing of the extinction is not clearly resolved but may be restricted to the earliest part of the Early Eocene. Two richness estimators (Chao 2 and Jackknife 2) both demonstrate that Late Palaeocene samples contain significantly more taxa than those in the Early Eocene. Extinction on the US Gulf Coast proves that ancient tropical ecosystems were highly susceptible to changes in diversity mediated directly or indirectly by environmental change even during equable greenhouse climates in the early Palaeogene. C1 Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Unit 0948, APO, AA 34002 USA. RP Harrington, GJ (reprint author), Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. EM g.j.harrington@bham.ac.uk NR 83 TC 37 Z9 39 U1 1 U2 18 PU GEOLOGICAL SOC PUBL HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CENTRE, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0016-7649 J9 J GEOL SOC LONDON JI J. Geol. Soc. PD MAR PY 2007 VL 164 BP 323 EP 332 DI 10.1144/0016-76492006-027 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 149JN UT WOS:000245143300006 ER PT J AU Santos-Granero, F AF Santos-Granero, Fernando TI Of fear and friendship: Amazonian sociality beyond kinship and affinity SO JOURNAL OF THE ROYAL ANTHROPOLOGICAL INSTITUTE LA English DT Article AB The article explores the nature of sociality and alterity in indigenous Amazonia. If native Amazonian sociality is all about predatory affinity or, alternatively, convivial consanguinity, why do native Amazonians constantly strive to establish social relationships with people with whom they are related neither as kin nor as affines? The comparative analysis of intertribal trading partnerships, shamanic networks, and mystical associations allows the author to examine the mechanisms by which hostile or potentially hostile relations between strangers - non-relatives - are transformed into relations of amicability. Special emphasis is placed on the role played by 'trust' and 'spaces of trust' in the creation of non-kin-based social networks. In brief the article analyses the little-studied issue of 'friendship', viewing it as an alternative to kinship and affinity in the construction of Amerindian societies and multi-ethnic polities. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. EM santosf@si.edu NR 66 TC 19 Z9 20 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1359-0987 EI 1467-9655 J9 J ROY ANTHROPOL INST JI J. R. Anthropol. Inst. PD MAR PY 2007 VL 13 IS 1 BP 1 EP 18 DI 10.1111/j.1467-9655.2007.00410.x PG 18 WC Anthropology SC Anthropology GA 134KU UT WOS:000244082700001 ER PT J AU Richards, LA Windsor, DM AF Richards, Lora A. Windsor, Donald M. TI Seasonal variation of arthropod abundance in gaps and the understorey of a lowland moist forest in Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Coleoptera; communities; Hymenoptera; Malaise traps; Panama; seasonality; treefall gaps; tropical forest ID TROPICAL RAIN-FOREST; COMPARATIVE FORAGING BEHAVIOR; TREEFALL GAPS; NEOTROPICAL FOREST; SPECIES-DIVERSITY; INSECT COMMUNITIES; WET FOREST; HERBIVORY; AVAILABILITY; BIRDS AB Treefalls gaps contribute to the habitat heterogeneity of tropical forest floors. Previous studies have shown that these gaps play an important role in plant and bird communities, however less is known about their role in arthropod communities. Using eight Malaise traps we investigated the difference in arthropod abundance of 19 taxonomic groups between gaps and understorey for 21 wk during the rainy season and 8 wk in the dry season on Barro Colorado Island, Panama. More (33.8%) arthropods were collected in gaps during the rainy season and 32.2%, more in the understorey during the dry season. To assess the possible factors contributing to these differences we measured light, plant densities and young leaf densities, as indicators of abiotic factors and food resources for insect herbivores. Arthropod abundance was negatively correlated with light in the dry season. Thus, abiotic stress may explain the pattern of abundance in the dry season. While there was no correlation with light in the rainy season, predator abundance was positively correlated with herbivore abundance. The plant and young leaf density data suggest that there is significantly higher food availability for herbivores in gaps. Thus, less stressful abiotic conditions and more food resources may contribute to more herbivores followed by more predators in gaps during the rainy season. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Macquarie Univ, Dept Biol Sci, Ancon 84112, Panama. Smithsonian Trop Res Inst, Ancon, Panama. RP Richards, LA (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. EM lrichards@bio.mq.edu.au NR 38 TC 41 Z9 42 U1 4 U2 24 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2007 VL 23 BP 169 EP 176 DI 10.1017/S0266467406003907 PN 2 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 149SV UT WOS:000245167800005 ER PT J AU Feeley, KJ Davies, SJ Noor, MNS Kassim, AR Tan, S AF Feeley, Kenneth J. Davies, Stuart J. Noor, Md. Nur Supardi Kassim, Abdul Rahman Tan, Sylvester TI Do current stem size distributions predict future population changes? An empirical test of intraspecific patterns in tropical trees at two spatial scales SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE coefficient of skewness; forest dynamics; Malaysia; population dynamics; Weibull distribution ID DISTURBANCE HISTORY; AMAZONIAN FORESTS; WESTERN THAILAND; TURNOVER; GROWTH; RATES; AGE; MONODOMINANT; COMMUNITIES; RECRUITMENT AB It is critical to understand the responses of tropical tree species to ongoing anthropogenic disturbances. Given the longevity of large trees and the scarcity of appropriately long-term demographic data, standing size distributions are a potential tool for predicting species' responses to disturbances and resultant changes in population structure. Here we test the utility of several different measures of size distribution for predicting subsequent population changes at the intraspecific level using demographic records from two subsampled 50-ha tree plots in Malaysia (Pasoh and Lambir). Most measures of size distribution failed to successfully predict population change better than random; however, the 'coefficient of skewness' (a measure of the relative proportion of small vs. large stems in a population) was able to correctly predict the direction of population change for approximately three-quarters of species at both sites. At Pasoh, the magnitude of this relationship decreased with adult stature and rate of turnover, but was unrelated to sapling growth rates at either site. Finally, using data for species common at both forests, we found that size distributions were generally uninformative of subsequent differences in population change between sites (only median dbh correctly predicted the direction of change for more species than random). Based on these results we conclude that some measures of intraspecific differences in size distribution are potentially informative of population trends within forests but have limited utility across broader spatial scales. C1 Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum Asia Program, Cambridge, MA 02138 USA. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Miami, FL 34002 USA. Forest Res Inst Malaysia, Forest Environm Div, Kuala Lumpur 52109, Malaysia. Sarawak Forest Corp, Forest Res Ctr, Kuching 93250, Sarawak, Malaysia. RP Feeley, KJ (reprint author), Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum Asia Program, 22 Divin Ave, Cambridge, MA 02138 USA. EM kfeeley@oeb.harvard.edu RI Feeley, Kenneth/A-7631-2009 NR 33 TC 27 Z9 30 U1 0 U2 19 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2007 VL 23 BP 191 EP 198 DI 10.1017/S0266467406003919 PN 2 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 149SV UT WOS:000245167800007 ER PT J AU Zimmerman, JK Wright, SJ Calderon, O Pagan, MA Paton, S AF Zimmerman, Jess K. Wright, S. Joseph Calderon, O. Pagan, M. Aponte Paton, S. TI Flowering and fruiting phenologies of seasonal and aseasonal neotropical forests: the role of annual changes in irradiance SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Barro Colorado Island; Panama; Luquillo Forest Dynamics Plot; phenology; Puerto Rico; rainfall; reproduction; seasonality; solar irradiance ID DRY TROPICAL FOREST; RAIN-FOREST; PUERTO-RICO; SEED PREDATION; LEAF PHENOLOGY; WATER STORAGE; CANOPY TREES; COSTA-RICA; WET FOREST; PATTERNS AB The seasonality of both rainfall and solar irradiance might influence the evolution of flowering and fruiting in tropical forests. In seasonally dry forests, to the degree that soil moisture limits plant productivity, community-wide peaks in reproduction are expected during the rainy season, with seedfall and germination timed to allow seedlings to become well established while soil moisture is available. Where soil moisture is never seasonally limiting, seasonal changes in light availability caused by periods of cloudiness or seasonally low zenithal sun angles should favour reproduction during seasons when irradiance levels are high. To evaluate these predictions, we documented the timing of flower and fruit fall for 10 and 15 y at El Verde, Puerto Rico, and Barro Colorado Island (BCI), Panama. At El Verde, rainfall is abundant year-round and solar declination largely determines seasonal variation in irradiance. At BCL rainfall is abundant throughout the 8-mo wet season while drought develops and average solar irradiance increases by 40-50% over the 4-mo dry season. Seasonal variation in the number of species flowering and fruiting at both sites was generally consistent with the hypothesis that seasonal variation in irradiance limits the evolution of reproductive phenologies. Community-level metrics provided no evidence for a similar role for moisture availability at BCL Seasonal variation in irradiance also strongly influenced seed development times at both sites. Thus, community-wide phenologics reveal a strong signature of seasonal changes in irradiance, even in those forests that exhibit some degree of seasonality in rainfall. C1 Univ Puerto Rico, Inst Trop Ecosyst Studies, Rio Piedras, PR 00931 USA. Smithsonian Trop Res Inst, Balboa 084303092, Panama. RP Zimmerman, JK (reprint author), Univ Puerto Rico, Inst Trop Ecosyst Studies, POB 2910, Rio Piedras, PR 00931 USA. EM jkzimmerman@uprrp.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 43 TC 69 Z9 72 U1 4 U2 40 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2007 VL 23 BP 231 EP 251 DI 10.1017/S0266467406003890 PN 2 PG 21 WC Ecology SC Environmental Sciences & Ecology GA 149SV UT WOS:000245167800011 ER PT J AU Qin, Q Wei, FW Li, M Dubovi, EJ Loeffler, IK AF Qin, Qin Wei, Fuwen Li, Ming Dubovi, Edward J. Loeffler, I. Kati TI Serosurvey of infectious disease agents of carnivores in captive red pandas (Ailurus fulgens) in China SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE red panda; Ailiurus fulgens; serosurvey; infectious diseases; China ID CANINE-DISTEMPER; SEROLOGIC SURVEY; SEROPREVALENCE; NEOSPORA; ANTIBODIES; PARVOVIRUS; VIRUSES; DOGS AB The future of the endangered red panda (Ailurus fulgens) depends in part on the development of protective measures against infectious diseases. The present study is a first step toward improved understanding of infectious diseases in the species' home regions. Serum samples obtained from 73 red pandas in 10 captive facilities in southwest, east, and northeast China from October to December 2004 were tested for antibodies against nine common infectious pathogens of carnivores. Antibody titers against canine distemper virus (CDV), canine parvovirus (CPV), and canine adenovirus (CAV) in the three facilities in which red pandas were vaccinated were highly variable. The CAV titer in one vaccinated red panda was high enough to suggest infection with the field virus following vaccination. Together with anecdotal reports of vaccine-associated morbidity and mortality, our results suggest that the Chinese vaccine is not suitable for this species. In the seven unvaccinated groups, CDV titers were low and occurred in 20-100% of the animals; antibody titers against CPV were found in seven of eight areas. Only one of 61 and two of 61 unvaccinated red pandas had CAV and canine coronavirus titers, respectively, and these titers were all low. Positive titers to Toxoplasma gondii were found in four locations (33-94% seropositive); the titers in 52% of seropositive individuals were of a magnitude consistent with active disease in other species (1: 1,024 to >= 1:4,096). One red panda in each of three locations was seropositive for Neospora caninum. Antibodies against canine herpesvirus and Brucella canis were not detected in any of the samples. Only one of the 73 red pandas had a weak positive influenza A titer. The results of this study emphasize the need for research on and protection against infectious diseases of red pandas and other endangered species in China. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Chinese Acad Sci, Inst Zool, Beijing 100080, Peoples R China. Cornell Univ, Anim Hlth Diagnost Ctr, Ithaca, NY 14853 USA. RP Loeffler, IK (reprint author), 2828 Regent St, Madison, WI 53705 USA. NR 26 TC 9 Z9 10 U1 2 U2 14 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2007 VL 38 IS 1 BP 42 EP 50 DI 10.1638/06-048.1 PG 9 WC Veterinary Sciences SC Veterinary Sciences GA 149IV UT WOS:000245141500007 PM 17469274 ER PT J AU Harris, MC Sleeman, JM AF Harris, M. Camille Sleeman, Jonathan M. TI Morbidity and mortality of bald eagles (Haliaeetus leucocephalus) and peregrine falcons (Falco peregrinus) admitted to the Wildlife Center of Virginia, 1993-2003 SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE bald eagles; Falco peregrinus; Haliaeetus leucocephalus; morbidity; mortality; peregrine falcons ID WEST-NILE-VIRUS; RAPTORS; BIRDS AB Medical records from 111 threatened bald eagles (86%, Haliaeetus leucocephalus) and peregrine falcons (14%, Falco peregrinus) admitted to the Wildlife Center of Virginia from 1993 to 2003 were reviewed to identify submitters, causes of morbidity and mortality, and final disposition. Half of all patients admitted were submitted by the Virginia Department of Game and Inland Fisheries personnel. Trauma was the most common reason for presentation in bald eagles (70%) and peregrine falcons (81%). Additional causes of morbidity and mortality in bald eagles included toxicoses (10%), infectious diseases (8%), and orphaned young (1%). Neoplasia was confirmed in two trauma cases, suggesting underlying disease might have increased susceptibility to acute traumatic injuries. Peregrine falcons were also admitted for infectious disease (19%). The most frequent infectious disease for both species was West Nile virus. Thirty-nine percent of patients were released back into the wild, 28% were euthanized, 20% died, and 13% were placed in captivity. Postrelease monitoring that would determine whether rehabilitated animals survived to contribute to threatened populations was not performed in this study. C1 Wildlife Ctr Virginia, Waynesboro, VA 22980 USA. Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. RP Harris, MC (reprint author), Wildlife Ctr Virginia, POB 1557, Waynesboro, VA 22980 USA. RI Harris, M. Camille/E-2465-2013 NR 27 TC 14 Z9 14 U1 1 U2 23 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2007 VL 38 IS 1 BP 62 EP 66 DI 10.1638/05-099.1 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA 149IV UT WOS:000245141500010 PM 17469277 ER PT J AU Rodriguez, W August, PV Wang, YQ Paul, JF Gold, A Rubinstein, N AF Rodriguez, Wilfrid August, Peter V. Wang, Yeqiao Paul, John F. Gold, Arthur Rubinstein, Norman TI Empirical relationships between land use/cover and estuarine condition in the Northeastern United States SO LANDSCAPE ECOLOGY LA English DT Article DE landscape analysis; estuarine condition; water quality; GIS ID COASTAL WATER-QUALITY; WAQUOIT BAY; SEDIMENT CONTAMINATION; MID-ATLANTIC; NITROGEN; EUTROPHICATION; MASSACHUSETTS; CONSEQUENCES; MARINE; ENRICHMENT AB Land-water interactions were examined in three regions in the Virginian Biogeographic Province; the southern shore of Cape Cod, Massachusetts; the Hudson/Raritan region of New York; and the eastern shore of the Delmarva (Delaware/Maryland/Virginia) Peninsula. Cumulative distribution functions were used to evaluate similarity in environmental condition among estuaries. Spatial-setting variables (location in a river, coastal lagoon, or in open waters) were associated with variation for some measures of estuarine condition. Patterns of coastal urban and agriculture gradients were measured and their relationship with indicators of estuarine condition was modeled statistically. When estuaries were pooled, the highest variation explained by spatial-setting variables was found for dissolved oxygen (DO, R-2 = 0.44) and salinity (R-2 = 0.58), with DO decreasing in river locations and salinity decreasing with rainfall and sampling locations near rivers. The explanatory power for the other indicator variables was low and varied from 6% to 27%. Rainfall explained some of the variation (R-2 = 0.23) in total suspended solids. Moderate (0.4 < vertical bar r vertical bar < 0.7) to strong (vertical bar r vertical bar 0.7) linear associations were found between total urban area and measures of estuarine condition. Within regions, total urban area was positively associated with Silver (r = 0.59), Cadmium (r = 0.65), and Mercury (r = 0.47) in Cape Cod, and inversely related to DO (r = -0.65) in the Hudson/Raritan region. No associations were found in the Delmarva Peninsula study area. Total area of agriculture showed a moderate association with Arsenic in Cape Cod, but no other associations were found in the other two regions. Our analyses show a measurable impact of urban land use on coastal ecosystem condition over large areas of the northeastern United States. This pattern was most evident when many different landscapes were considered simultaneously. The relationship between urban development and estuarine condition were weaker within the individual regions studied. The use of land use/cover models for predicting estuarine condition is a challenging task that warrants enhancements in the type, quantity, and quality of data to improve our ability to discern relationships between anthropogenic activities on land and the condition of coastal environments. C1 Univ Rhode Isl, Dept Civil & Environm Engn, Kingston, RI 02881 USA. Univ Rhode Isl, Dept Nat Resources Sci, Kingston, RI 02881 USA. US Environm Protect Agcy, ORD, NHEERL, Res Triangle Pk, NC 27711 USA. US Environm Protect Agcy, Atlantic Ecol Div, Narragansett, RI 02882 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Rodriguez, W (reprint author), Univ Rhode Isl, Dept Civil & Environm Engn, 1 Lippit Rd,Bliss Hall Room 308C, Kingston, RI 02881 USA. EM wrg@etal.uri.edu NR 77 TC 16 Z9 18 U1 2 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD MAR PY 2007 VL 22 IS 3 BP 403 EP 417 DI 10.1007/s10980-006-9036-8 PG 15 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 139TJ UT WOS:000244455200006 ER PT J AU Arnold, DE Neff, H Glascock, MD Speakman, RJ AF Arnold, Dean E. Neff, Hector Glascock, Michael D. Speakman, Robert J. TI Sourcing the palygorskite used in Maya Blue: A pilot study comparing the results of INAA and LA-ICP-MS SO LATIN AMERICAN ANTIQUITY LA English DT Article ID PIGMENTS; YUCATAN; MEXICO; SIMULATIONS; ATTAPULGITE; POTTERY; INDIGO; PAINT AB Maya Blue is an unusual blue pigment consisting of a clay-organic complex of indigo and the unusual clay mineral palygorskite (also called attapulgite). Used on pottery, sculpture, and murals from the Preclassic to Late Colonial periods largely in Mesoamerica, blue was the color of sacrifice and ritual. Did the palygorskite used to make Maya Blue come from a restricted source in Yucatan like Shepard, Arnold, Arnold and Bohor believed, or from widespread sources like Littmann argued? This report presents the results of a pilot study comparing INAA and LA-ICP-MS analysis of 33 palygorskite samples collected from different parts of the Maya area. These data reveal that it is possible to discriminate mineral source locations, and that it should be possible to determine whether the palygorskite used to make Maya Blue came from widespread sources or was traded widely from one or a few sources. Consideration of contextual information such as agency, landscape and language suggest that the Shepard/Arnold/Bohor hypothesis is more plausible than that of Littmann. No matter which hypothesis is supported, however, each has significant implications for the relationship of the diffusion of Maya Blue (or the knowledge of its production) to Maya social organization. C1 Wheaton Coll, Dept Sociol Anthropol, Wheaton, IL 60187 USA. Calif State Univ Long Beach, Dept Anthropol, Long Beach, CA 90840 USA. Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. Smithsonian Inst Museum Conservat Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Arnold, DE (reprint author), Wheaton Coll, Dept Sociol Anthropol, Wheaton, IL 60187 USA. EM Dean.E.Arnold@wheaton.edu; hneff@csulb.edu; glascockm@missouri.edu; speakmanj@si.edu OI Glascock, Michael D./0000-0003-0686-7556; Speakman, Robert/0000-0003-2063-154X NR 52 TC 19 Z9 19 U1 2 U2 6 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD MAR PY 2007 VL 18 IS 1 BP 44 EP 58 PG 15 WC Archaeology SC Archaeology GA 150EJ UT WOS:000245198100003 ER PT J AU Stark, BL Speakman, RJ Glascock, MD AF Stark, Barbara L. Speakman, Robert J. Glascock, Michael D. TI Inter-regional and intra-regional scale compositional variability in pottery from south-central Veracruz, Mexico SO LATIN AMERICAN ANTIQUITY LA English DT Article ID PROVENANCE; CERAMICS; BASIN AB Both long-distance and localized chemical relationships in pottery and their implications for studies of Gulf lowland exchange can be examined with instrumental neutron activation. New pottery samples from Classic period (A.D. 300-900) contexts in the western lower Papaloapan basin were subjected to chemical compositional analysis. The sample represents three groups, coarse utility jars, common orange slipped serving bowls, and fine paste, higher-value white slipped serving bowls. At an intraregional scale, four localities in the western basin were sampled, but not all proved to be compositionally distinct. A mangrove zone pottery group contrasts compositionally with groups from riverine farmlands to the west. At a larger interregional scale, pottery from neighboring geomorphological areas as well as distant alluvial systems up and down the Gulf lowlands yielded chemically distinct groups. Considerable intraregional trade is suggested, but little is evident at the interregional scale. The interregional analysis is the first integrated overview of Gulf lowland ceramic chemical compositions, and the intraregional analysis begins assessment of Classic period pottery production and exchange within the western lower Papaloapan basin. Methodologically, we use sand sources in the region to determine if differences in tempering of pastes are likely to account for differences in compositional groups. C1 Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. Smithsonian Inst Museum Conservat Inst, Museum Support Ctr, Suitland, MD 20746 USA. Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. RP Stark, BL (reprint author), Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. EM blstark@asu.edu; speakmanj@si.edu; glascockm@missouri.edu OI Glascock, Michael D./0000-0003-0686-7556; Speakman, Robert/0000-0003-2063-154X NR 43 TC 2 Z9 2 U1 0 U2 0 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD MAR PY 2007 VL 18 IS 1 BP 59 EP 84 PG 26 WC Archaeology SC Archaeology GA 150EJ UT WOS:000245198100004 ER PT J AU Riley, S AF Riley, Sheila TI Mergers and acquisitions. 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 REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 1 PY 2007 VL 132 IS 4 BP 79 EP 79 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 141WE UT WOS:000244608900094 ER PT J AU Derivera, CE Hitchcock, NG Teck, SJ Steves, BP Hines, AH Ruiz, GM AF deRivera, Catherine E. Hitchcock, Natasha Gray Teck, Sarah J. Steves, Brian P. Hines, Anson H. Ruiz, Gregory M. TI Larval development rate predicts range expansion of an introduced crab SO MARINE BIOLOGY LA English DT Article ID CARCINUS-MAENAS L; PORTUNIDAE LARVAE; SHORE CRAB; L DECAPODA; NONINDIGENOUS CRAB; TEMPERATURE; INVASIONS; GROWTH; ABUNDANCE; IMPACTS AB Introduced populations can cause ecological and economic damage and are difficult to eradicate once they have established. It is therefore important to be able to predict both where species may become established and their capacity to spread within recipient regions. Here, we use a new method to assess potential for intraregional spread of a marine crab introduced to North America, Carcinus maenas. We determined survivorship and development rates throughout a range of temperatures in the laboratory for C. maenas larvae from non-native populations on the Atlantic and Pacific coasts of North America. The larvae exhibited narrower physiological tolerances than adults, and no lab-cultured larvae completed larval development below 10.0 degrees C or above 22.5 degrees C. Survivorship peaked at intermediate water temperatures of 12.5-20.0 degrees C, and development time decreased with increasing temperatures within this range. Based upon these laboratory development rates, we used nearshore sea-surface temperature data from both coasts of North America to predict development times required for larvae at different months and sites. Taken together, survivorship and development data indicate that C. maenas has the capacity to continue its northward spread and establish populations at numerous additional sites in North America. Moreover, decadal temperature data at two Alaskan sites predicted little variability in development duration across years, suggesting that development duration predictions are robust to interannual water temperature differences. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Portland State Univ, Aquat Invas Res & Policy Inst, Portland, OR 97207 USA. RP Derivera, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM derivera@pdx.edu RI Teck, Sarah/C-5179-2009; OI Ruiz, Gregory/0000-0003-2499-441X NR 45 TC 38 Z9 39 U1 2 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAR PY 2007 VL 150 IS 6 BP 1275 EP 1288 DI 10.1007/s00227-006-0451-9 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 139TG UT WOS:000244454900023 ER PT J AU Cuignet, M Hance, T Windsor, DM AF Cuignet, M. Hance, T. Windsor, D. M. TI Phylogenetic relationships of egg parasitoids (Hymenoptera : Eulophidae) and correlated life history characteristics of their neotropical Cassidinae hosts (Coleoptera, Chrysomelidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Eulophidae; Cassidinae; parasitoid; supertree; total evidence; matrix representation parsimony ID COMBINING DATA SETS; MATRIX REPRESENTATION; SPECIES PHYLOGENIES; BAYESIAN-INFERENCE; SEQUENCE DATA; TREES; CHALCIDOIDEA; ACCURACY; CLASSIFICATION; PTEROMALIDAE AB Egg parasitoids in the family Eulophidae (Hymenoptera) are an important part of the community of insects attacking neotropical leaf beetles in the subfamily Cassidinae. We present a phylogeny of 24 species of oophagous Eulophidae, using the 28S rDNA, the ITS2 rDNA and the cytochrome b genes, applying the NJ, MP, ML and Bayesian tree reconstruction methods on each data set. We ask whether the phylogenetic relationships of the parasitoids are linked with the life history characteristics of their beetle hosts. We show that cladogenesis in the oophagous Eulophidae does correlate with ovipositional behaviour and, to a lesser extent, diet and tribal affinities of their hosts. Additionally using two methods of simultaneous analysis of several gene sets: the Total Evidence method, and the construction of a "supertree" by Matrix Representation Parsimony (MRP), we substantiate the same major phylogenetic relationships within the Eulophidae. (c) 2006 Elsevier Inc. All rights reserved. C1 Ctr Rech Biodivers, Unite Ecol & Biogeog, B-1348 Louvain, Belgium. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Hance, T (reprint author), Ctr Rech Biodivers, Unite Ecol & Biogeog, Pl Croix Sud 4-5, B-1348 Louvain, Belgium. EM cuignet@ecol.ucl.ac.be; Hance@ecol.ucl.ac.be; windsord@si.edu NR 57 TC 6 Z9 7 U1 1 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2007 VL 42 IS 3 BP 573 EP 584 DI 10.1016/j.ympev.2006.09.005 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 157KB UT WOS:000245717300001 PM 17118675 ER PT J AU Ercolano, B Barlow, MJ Sugerman, BEK AF Ercolano, B. Barlow, M. J. Sugerman, B. E. K. TI Dust yields in clumpy supernova shells: SN 1987A revisited SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae : individual : SN 1987A ID BOLOMETRIC LIGHT-CURVE; RADIATIVE-TRANSFER; REMNANT CASSIOPEIA; PLATEAU SUPERNOVA; II SUPERNOVAE; SN-1987A; GRAINS; EXTINCTION; PHOTOMETRY; SPECTROPHOTOMETRY AB We present a study of the effects of clumping on the emergent spectral energy distribution (SED) from dusty supernova (SN) shells illuminated by a diffuse radiation source distributed throughout the medium. These models are appropriate for Type II SNe older than a few hundred days, when the energy input is dominated by gamma-rays from (56)Co decay. The fully 3D radiation transport problem is solved using a Monte Carlo code, MOCASSIN, and we present a set of models aimed at investigating the sensitivity of the SEDs to various clumping parameters. We find that, contrary to the predictions of analytical prescriptions, the combination of an optical and infrared (IR) observational data set is sufficient to constrain dust masses even in the case where optically thick clumps are present. Using both smoothly varying and clumped grain density distributions, we obtain new estimates for the mass of dust condensed by the Type II SN 1987A by fitting the optical and IR spectrophotometric data of Wooden et al. at two epochs (day 615 and day 775). When using amorphous carbon grains, our best fits to the observational data imply that about 2.0 x 10(-4) M(circle dot) of dust had condensed in the envelope of SN 1987A by day 615 and between 2.0 x 10(-4) and 4.2 x 10(-3) M(circle dot) by day 775. We find that the absence of a silicate emission or absorption feature in the observed mid-IR spectra implies that no more than 15 per cent of the dust formed around SN 1987A can have been in the form of silicate particles. Our models require larger dust masses for the case of graphite grains, namely between 4.2 x 10(-4) and 6.6 x 10(-4) M(circle dot) at day 615 and between 4.5 x 10(-4) and 7.5 x 10(-4) M(circle dot) at day 775. From our numerical models, we derive dust masses for SN 1987A that are comparable to previous analytic clumped graphite grain mass estimates, and at least two orders of magnitude below the 0.1-0.3 M(circle dot) that have been predicted to condense as dust grains in primordial core-collapse SN ejecta. This low condensation efficiency for SN 1987A is in contrast to the case of SN 2003gd, for which a dust condensation efficiency as large as 0.12 has recently been estimated. C1 UCL, Dept Phys & Astron, London WC1E 6BT, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Goucher Coll, Baltimore, MD 21204 USA. RP Ercolano, B (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM bercolano@head.cfa.harvard.edu RI Barlow, Michael/A-5638-2009 OI Barlow, Michael/0000-0002-3875-1171 NR 57 TC 73 Z9 73 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2007 VL 375 IS 3 BP 753 EP 763 DI 10.1111/j.1365-2966.2006.11336.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134WT UT WOS:000244115800001 ER PT J AU Diego, JM Tegmark, M Protopapas, P Sandvik, HB AF Diego, J. M. Tegmark, M. Protopapas, P. Sandvik, H. B. TI Combined reconstruction of weak and strong lensing data with WSLAP SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; galaxies : clusters : general; dark matter ID CLUSTER MASS-DISTRIBUTION; HUBBLE-SPACE-TELESCOPE; NONPARAMETRIC RECONSTRUCTION; DARK-MATTER; GALAXIES; INVERSION; LENSES; ABELL-2218; QUASARS; A1689 AB We describe a method to estimate the mass distribution of a gravitational lens and the position of the sources from combined strong and weak lensing data. The algorithm combines weak and strong lensing data in a unified way producing a solution which is valid in both the weak and the strong lensing regimes. The method is non-parametric, allowing the mass to be located anywhere in the field of view. We study how the solution depends on the choice of basis used to represent the mass distribution. We find that combining weak and strong lensing information has two major advantages: it alleviates the need for priors and/or regularization schemes for the intrinsic size of the background galaxies (this assumption was needed in previous strong lensing algorithms) and it reduces (although does not remove) biases in the recovered mass in the outer regions where the strong lensing data are less sensitive. The code is implemented into a software package called Weak & Strong Lensing Analysis Package (WSLAP) which is publicly available at http://darwin.cfa.harvard.edu/SLAP/. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. IFCA, Inst Fis Cantabria, Santander 39005, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85748 Garching, Germany. RP Diego, JM (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jdiego@ifca.unican.es NR 35 TC 39 Z9 39 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 MAR 1 PY 2007 VL 375 IS 3 BP 958 EP 970 DI 10.1116/j.1365-2966.2007.11380.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134WT UT WOS:000244115800017 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, J. Stuart B. Loeb, Abraham TI The correlation between the distribution of galaxies and 21-cm emission at high redshifts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : high-redshift; intergalactic medium; diffuse radiation; large-scale structure of Universe; cosmology : theory ID DARK-MATTER HALOES; LOW-MASS GALAXIES; REIONIZATION; EPOCH; PHOTOIONIZATION; FLUCTUATIONS; EVOLUTION; QUASARS; MODEL AB Deep surveys have recently discovered galaxies at the tail end of the epoch of reionization. In the near future, these discoveries will be complemented by a new generation of low-frequency radio observatories that will map the distribution of neutral hydrogen in the intergalactic medium through its redshifted 21-cm emission. In this paper we calculate the expected cross-correlation between the distribution of galaxies and intergalactic 21-cm emission at high redshifts. We demonstrate using a simple model that overdense regions are expected to be ionized early as a result of their biased galaxy formation. This early phase leads to an anticorrelation between the 21-cm emission and the overdensities in galaxies, matter and neutral hydrogen. Existing Ly alpha surveys probe galaxies that are highly clustered in overdense regions. By comparing 21-cm emission from regions near observed galaxies to those away from observed galaxies, future observations will be able to test this generic prediction and calibrate the ionizing luminosity of high-redshift galaxies. C1 Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyithe, JSB (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. EM swyithe@physics.unimelb.edu.au; loeb@cfa.harvard.edu OI Wyithe, Stuart/0000-0001-7956-9758 NR 22 TC 32 Z9 32 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2007 VL 375 IS 3 BP 1034 EP 1042 DI 10.1111/j.1365-2966.2007.11366.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134WT UT WOS:000244115800025 ER PT J AU Kreamer, CM AF Mullen Kreamer, Christine TI "Crossroads of people, crossroads of trade" - The shared heritage and contested terrain of Ghana's Cape Coast Castle Museum SO MUSEUM NEWS LA English DT Article C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. RP Kreamer, CM (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 2007 VL 86 IS 2 BP 52 EP 59 PG 8 WC Art SC Art GA 178QB UT WOS:000247234100028 ER PT J AU Soon, W AF Soon, Willie TI Implications of the secondary role of carbon dioxide and methane forcing in climate change: Past, present, and future SO PHYSICAL GEOGRAPHY LA English DT Review DE glacial-interglacial cycles; water vapor, cloud-and-ice insulator, and albedo feedback; Milankovic orbital insulation forcing; atmospheric Co-2 and CH4 forcing ID LAST GLACIAL MAXIMUM; SEA-SURFACE TEMPERATURES; DEUTERIUM-EXCESS CORRECTION; EURASIAN ICE SHEETS; PACIFIC WARM POOL; HOLOCENE CLIMATE; ATMOSPHERIC CO2; VOSTOK ICE; SOUTHERN-HEMISPHERE; LATE PLEISTOCENE AB A review of the recent refereed literature fails to confirm quantitatively that carbon dioxide (CO2) radiative forcing was the prime mover in the changes in temperature, ice-sheet volume, and related climatic variables in the glacial and interglacial episodes of the past 650,000 years, even under the "fast-response" framework where the convenient if artificial distinction between forcing and feedback is assumed. Atmospheric CO2 variations generally follow changes in temperature and other climatic variables rather than preceding them. Likewise, there is no confirmation of the often-posited significant supporting role of methane (CH4) forcing, which-despite its faster atmospheric response time-is simply too small, amounting to less than 0.2 W/m(2) from a change of 400 ppb. We cannot quantitatively validate the numerous qualitative suggestions that the CO2 and CH4 forcings that occurred in response to Milankovic orbital cycles accounted for more than half of the amplitude of the changes in the glacial/interglacial cycles of global temperature, sea level, and ice volume. Consequently, we infer that natural climatic variability-notably the persistence of insolation forcing at key seasons and geographical locations, taken with closely related thermal, hydrological, and cryospheric changes (such as the water vapor, cloud, and ice albedo feedbacks)-suffices in se to explain the proxy-derived, global and regional climatic and environmental phase-transitions in the paleoclimate. If so, it may be appropriate to place anthropogenic greenhouse gas emissions in context by separating their medium-term climatic impacts from those of a host of natural forcings and feedbacks that may, as in paleoclimatological times, prove equally significant. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 146 TC 14 Z9 18 U1 3 U2 32 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0272-3646 EI 1930-0557 J9 PHYS GEOGR JI Phys. Geogr. PD MAR-APR PY 2007 VL 28 IS 2 BP 97 EP 125 DI 10.2747/0272-3646.28.2.97 PG 29 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Physical Geography; Geology; Meteorology & Atmospheric Sciences GA 230RE UT WOS:000250892800001 ER PT J AU Chu, X Dalgarno, A Groenenboom, GC AF Chu, Xi Dalgarno, Alexander Groenenboom, Gerrit C. TI Dynamic polarizabilities of rare-earth-metal atoms and dispersion coefficients for their interaction with helium atoms SO PHYSICAL REVIEW A LA English DT Article ID DER-WAALS COEFFICIENTS; TENSOR POLARIZABILITIES; STARK; STATES AB The dynamic scalar and tensor polarizabilities of the rare-earth-metal atoms are calculated with time-dependent density functional theory. The frequency-dependent polarizabilities at imaginary frequencies are used to determine the isotropic and orientation-dependent van der Waals coefficients for the interactions of the rare-earth-metal atoms with helium atoms. The static polarizabilities are compared with other theoretical values and with experimental results. The agreement is satisfactory in most cases but there are some exceptions where the discrepancy between theory and experiment is significant. The derived isotropic van der Waals coefficients range between 37 and 50 E(H)a(0)(6) and the orientation-dependent coefficients between 2 and -1 E(H)a(0)(6). Thus the ratio of elastic to inelastic scattering cross sections is expected to be substantial and any one of the rare-earth-metal atoms is an excellent candidate for trapping and cooling in a He gas. C1 Univ Montana, Dept Chem, Missoula, MT 59812 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Radboud Univ Nijmegen, Inst Mol & Mat, NL-6525 ED Nijmegen, Netherlands. RP Chu, X (reprint author), Univ Montana, Dept Chem, Missoula, MT 59812 USA. RI Groenenboom, Gerrit/F-9692-2015; OI Groenenboom, Gerrit/0000-0002-0920-3707 NR 28 TC 30 Z9 30 U1 0 U2 6 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 MAR PY 2007 VL 75 IS 3 AR 032723 DI 10.1103/PhysRevA.75.032723 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 151YE UT WOS:000245326300129 ER PT J AU Rossini, D Calarco, T Giovannetti, V Montangero, S Fazio, R AF Rossini, Davide Calarco, Tommaso Giovannetti, Vittorio Montangero, Simone Fazio, Rosario TI Decoherence induced by interacting quantum spin baths SO PHYSICAL REVIEW A LA English DT Article ID RENORMALIZATION-GROUPS; STATISTICAL-MECHANICS; CONTROLLED COLLISIONS; XY-MODEL; ENTANGLEMENT; CHAIN; TRANSITION; COMPUTERS; SYSTEMS; ATOMS AB We study decoherence induced on a two-level system coupled to a one-dimensional quantum spin chain. We consider the cases where the dynamics of the chain is determined by the Ising, XY, or Heisenberg exchange Hamiltonian. This model of quantum baths can be of fundamental importance for the understanding of decoherence in open quantum systems, since it can be experimentally engineered by using atoms in optical lattices. As an example, here we show how to implement a pure dephasing model for a qubit system coupled to an interacting spin bath. We provide results that go beyond the case of a central spin coupled uniformly to all the spins of the bath, in particular showing what happens when the bath enters different phases, or becomes critical; we also study the dependence of the coherence loss on the number of bath spins to which the system is coupled and we describe a coupling-independent regime in which decoherence exhibits universal features, irrespective of the system-environment coupling strength. Finally, we establish a relation between decoherence and entanglement inside the bath. For the Ising and the XY models we are able to give an exact expression for the decay of coherences, while for the Heisenberg bath we resort to the numerical time-dependent density matrix renormalization group. C1 CNR, INFM, NEST, I-56126 Pisa, Italy. Scuola Normale Super Pisa, I-56126 Pisa, Italy. Univ Trent, Dipartimento Fis, I-38050 Trento, Italy. INFM, CNR, BEC, I-38050 Trento, Italy. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. SISSA, Int Sch Adv Studies, I-34014 Trieste, Italy. RP Rossini, D (reprint author), CNR, INFM, NEST, Piazza Cavalieri 7, I-56126 Pisa, Italy. RI Rossini, Davide/A-8156-2012; Montangero, Simone/J-9393-2013; Fazio, rosario/M-1742-2013; OI Rossini, Davide/0000-0002-9222-1913; Fazio, rosario/0000-0002-7793-179X; GIOVANNETTI, VITTORIO/0000-0002-7636-9002 NR 53 TC 124 Z9 126 U1 2 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 2007 VL 75 IS 3 AR 032333 DI 10.1103/PhysRevA.75.032333 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 151YE UT WOS:000245326300065 ER PT J AU Wang, T Yelin, SF Cote, R Eyler, EE Farooqi, SM Gould, PL Kostrun, M Tong, D Vrinceanu, D AF Wang, T. Yelin, S. F. Cote, R. Eyler, E. E. Farooqi, S. M. Gould, P. L. Kostrun, M. Tong, D. Vrinceanu, D. TI Superradiance in ultracold Rydberg gases SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; SUPER-RADIANCE; ATOMS; OSCILLATIONS AB Experiments in dense, ultracold gases of rubidium Rydberg atoms show a considerable decrease of the radiative excited state lifetimes compared to dilute gases. This accelerated decay is explained by collective and cooperative effects, leading to superradiance. A formalism to calculate effective decay times in a dense Rydberg gas shows that for these atoms the decay into nearby levels increases by up to three orders of magnitude. Excellent agreement between theory and experiment follows from this treatment of Rydberg decay behavior. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. RP Wang, T (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. NR 28 TC 46 Z9 46 U1 2 U2 11 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 MAR PY 2007 VL 75 IS 3 AR 033802 DI 10.1103/PhysRevA.75.033802 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 151YE UT WOS:000245326300179 ER PT J AU Klaiman, S Moiseyev, N Sadeghpour, HR AF Klaiman, Shachar Moiseyev, Nimrod Sadeghpour, H. R. TI Interpretation of the Fano lineshape reversal in quantum waveguides SO PHYSICAL REVIEW B LA English DT Article ID ARTIFICIAL ATOMS; SPIN FILTERS; RESONANCES; DOTS; SPECTROSCOPY; SPECTRA; MATRIX; STATES AB Fano lineshape parameter (q) reversal is a proxy for interaction beyond the usual interference of indistinguishable quantum pathways. Reversal of the Fano parameter has been observed recently in quantum dots (QDs). We show that such a profile reversal may come about from the interaction of interloping over-the-top states (shape resonances) in the "nonresonant" channel with the QD bound states, interacting with the continuum channel (Feshbach resonances). Using this mechanism, we show that with minimal modifications of the QD parameters, we can affect the presence or absence of interloping resonances and hence lineshape profile reversal, as a way of coherence engineering. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Technion Israel Inst Technol, Dept Chem, IL-3200 Haifa, Israel. Technion Israel Inst Technol, Minerva Ctr Nonlinear Phys Complex Syst, IL-32000 Haifa, Israel. RP Klaiman, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. EM shachark@tx.technion.ac.il NR 32 TC 10 Z9 10 U1 0 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD MAR PY 2007 VL 75 IS 11 AR 113305 DI 10.1103/PhysRevB.75.113305 PG 4 WC Physics, Condensed Matter SC Physics GA 151ZK UT WOS:000245329600012 ER PT J AU Abazajian, KN Markevitch, M Koushiappas, SM Hickox, RC AF Abazajian, Kevork N. Markevitch, Maxim Koushiappas, Savvas M. Hickox, Ryan C. TI Limits on the radiative decay of sterile neutrino dark matter from the unresolved cosmic and soft X-ray backgrounds SO PHYSICAL REVIEW D LA English DT Article ID MILKY-WAY; CHANDRA; MODELS; HALO; OSCILLATIONS; CONSTRAINTS; PARTICLES; GALAXIES; CORE AB We present upper limits on line emission in the Cosmic X-ray background (CXB) that would be produced by decay of sterile neutrino dark matter. We employ the spectra of the unresolved component of the CXB in the Chandra Deep Fields North and South obtained with the Chandra CCD detector in the E=0.8-9 keV band. The expected decay flux comes from the dark matter on the lines of sight through the Milky Way galactic halo. Our constraints on the sterile neutrino decay rate are sensitive to the modeling of the Milky Way halo. The highest halo mass estimates provide a limit on the sterile neutrino mass of m(s)< 2.9 keV in the Dodelson-Widrow production model, while the lowest halo mass estimates provide the conservative limit of m(s)< 5.7 keV (2 sigma). We also discuss constraints from a short observation of the softer (E < 1 keV) X-ray background with a rocket-borne calorimeter by McCammon and collaborators. C1 Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. Los Alamos Natl Lab, ISR Div, Los Alamos, NM 87545 USA. RP Abazajian, KN (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. NR 66 TC 65 Z9 65 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAR PY 2007 VL 75 IS 6 AR 063511 DI 10.1103/PhysRevD.75.063511 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 152AW UT WOS:000245333600024 ER PT J AU Brown, ALP Day, FP Hungate, BA Drake, BG Hinkle, CR AF Brown, Alisha Lea Pagel Day, Frank P. Hungate, Bruce A. Drake, Bert G. Hinkle, C. Ross TI Root biomass and nutrient dynamics in a scrub-oak ecosystem under the influence of elevated atmospheric CO2 SO PLANT AND SOIL LA English DT Article DE root biomass; carbon dioxide; carbon; phosphorus; nitrogen; scrub-oak ID LONG-TERM DECOMPOSITION; CARBON-DIOXIDE; FINE ROOTS; SOIL CARBON; PLANT-RESPONSES; LEAF-LITTER; NITROGEN; FOREST; ENRICHMENT; GROWTH AB Elevated CO2 can increase fine root biomass but responses of fine roots to exposure to increased CO2 over many years are infrequently reported. We investigated the effect of elevated CO2 on root biomass and N and P pools of a scrub-oak ecosystem on Merritt Island in Florida, USA, after 7 years of CO2 treatment. Roots were removed from 1-m deep soil cores in 10-cm increments, sorted into different categories (< 0.25 mm, 0.25-1 mm, 1-2 mm, 2 mm to 1 cm, > 1 cm, dead roots, and organic matter), weighed, and analyzed for N, P and C concentrations. With the exception of surface roots < 0.25 mm diameter, there was no effect of elevated CO2 on root biomass. There was little effect on C, N, or P concentration or content with the exception of dead roots, and < 0.25 mm and 1-2 mm diameter live roots at the surface. Thus, fine root mass and element content appear to be relatively insensitive to elevated CO2. In the top 10 cm of soil, biomass of roots with a diameter of < 0.25 mm was depressed by elevated CO2. Elevated CO2 tended to decrease the mass and N content of dead roots compared to ambient CO2. A decreased N concentration of roots < 0.25 mm and 1-2 mm in diameter under elevated CO2 may indicate reduced N supply in the elevated CO2 treatment. Our study indicated that elevated CO2 does not increase fine root biomass or the pool of C in fine roots. In fact, elevated CO2 tends to reduce biomass and C content of the most responsive root fraction (< 0.25 mm roots), a finding that may have more general implications for understanding C input into the soil at higher atmospheric CO2 concentrations. C1 Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Dynamac Corp, Kennedy Space Ctr, FL 32899 USA. RP Day, FP (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. EM alpagel@yahoo.com; fday@odu.edu RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 45 TC 19 Z9 20 U1 0 U2 18 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X J9 PLANT SOIL JI Plant Soil PD MAR PY 2007 VL 292 IS 1-2 BP 219 EP 232 DI 10.1007/s11104-007-9218-4 PG 14 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 149BP UT WOS:000245121900017 ER PT J AU Rusch, DB Halpern, AL Sutton, G Heidelberg, KB Williamson, S Yooseph, S Wu, DY Eisen, JA Hoffman, JM Remington, K Beeson, K Tran, B Smith, H Baden-Tillson, H Stewart, C Thorpe, J Freeman, J Andrews-Pfannkoch, C Venter, JE Li, K Kravitz, S Heidelberg, JF Utterback, T Rogers, YH Falcon, LI Souza, V Bonilla-Rosso, G Eguiarte, LE Karl, DM Sathyendranath, S Platt, T Bermingham, E Gallardo, V Tamayo-Castillo, G Ferrari, MR Strausberg, RL Nealson, K Friedman, R Frazier, M Venter, JC AF Rusch, Douglas B. Halpern, Aaron L. Sutton, Granger Heidelberg, Karla B. Williamson, Shannon Yooseph, Shibu Wu, Dongying Eisen, Jonathan A. Hoffman, Jeff M. Remington, Karin Beeson, Karen Tran, Bao Smith, Hamilton Baden-Tillson, Holly Stewart, Clare Thorpe, Joyce Freeman, Jason Andrews-Pfannkoch, Cynthia Venter, Joseph E. Li, Kelvin Kravitz, Saul Heidelberg, John F. Utterback, Terry Rogers, Yu-Hui Falcon, Luisa I. Souza, Valeria Bonilla-Rosso, German Eguiarte, Luis E. Karl, David M. Sathyendranath, Shubha Platt, Trevor Bermingham, Eldredge Gallardo, Victor Tamayo-Castillo, Giselle Ferrari, Michael R. Strausberg, Robert L. Nealson, Kenneth Friedman, Robert Frazier, Marvin Venter, J. Craig TI The Sorcerer II Global Ocean Sampling expedition: Northwest Atlantic through Eastern Tropical Pacific SO PLOS BIOLOGY LA English DT Review ID INTERGENIC SPACER ANALYSIS; 16S RIBOSOMAL-RNA; MICROBIAL DIVERSITY; PROCHLOROCOCCUS ECOTYPES; BACTERIAL COMMUNITIES; ESCHERICHIA-COLI; GENOMIC ANALYSIS; SARGASSO SEA; DEEP-SEA; RED-SEA AB The world's oceans contain a complex mixture of micro-organisms that are for the most part, uncharacterized both genetically and biochemically. We report here a metagenomic study of the marine planktonic microbiota in which surface (mostly marine) water samples were analyzed as part of the Sorcerer 11 Global Ocean Sampling expedition. These samples, collected across a several-thousand km transect from the North Atlantic through the Panama Canal and ending in the South Pacific yielded an extensive dataset consisting of 7.7 million sequencing reads (6.3 billion bp). Though a few major microbial clades dominate the planktonic marine niche, the dataset contains great diversity with 85% of the assembled sequence and 57% of the unassembled data being unique at a 98% sequence identity cutoff. Using the metadata associated with each sample and sequencing library, we developed new comparative genomic and assembly methods. One comparative genomic method, termed "fragment recruitment," addressed questions of genome structure, evolution, and taxonomic or phylogenetic diversity, as well as the biochemical diversity of genes and gene families. A second method, termed "extreme assembly," made possible the assembly and reconstruction of large segments of abundant but clearly nonclonal organisms. Within all abundant populations analyzed, we found extensive intra-ribotype diversity in several forms: (1) extensive sequence variation within orthologous regions throughout a given genome; despite coverage of individual ribotypes approaching 500-fold, most individual sequencing reads are unique; (2) numerous changes in gene content some with direct adaptive implications; and (3) hypervariable genomic islands that are too variable to assemble. The intra-ribotype diversity is organized into genetically isolated populations that have overlapping but independent distributions, implying distinct environmental preference. We present novel methods for measuring the genomic similarity between metagenomic samples and show how they may be grouped into several community types. Specific functional adaptations can be identified both within individual ribotypes and across the entire community, including proteorhoclopsin spectral tuning and the presence or absence of the phosphate-binding gene PstS. C1 J Craig Venter Inst, Rockville, MD USA. Univ So Calif, Dept Biol Sci, Avalon, CA USA. Univ Calif Davis, Genome Ctr, Davis, CA 95616 USA. Your World, World Genome, Rockville, MD USA. Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol Evolut, Mexico City 04510, DF, Mexico. Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. Bedford Inst Oceanog, Dartmouth, NS, Canada. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Concepcion, Dept Oceanog, Concepcion, Chile. Univ Costa Rica, Escuela Quim, San Pedro, Costa Rica. Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ USA. Univ So Calif, Dept Earth Sci, Los Angeles, CA USA. RP Rusch, DB (reprint author), J Craig Venter Inst, Rockville, MD USA. EM DRusch@venterinstitute.org RI Tamayo, Giselle/J-3609-2015; Bonilla-Rosso, German/F-6548-2010; Goodwin, Kelly/B-4985-2014; OI Tamayo, Giselle/0000-0002-4912-8895; Bonilla-Rosso, German/0000-0003-0929-2890; Goodwin, Kelly/0000-0001-9583-8073; Heidelberg, John/0000-0003-0673-3224; Eisen, Jonathan A./0000-0002-0159-2197 NR 104 TC 1111 Z9 1139 U1 29 U2 224 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1544-9173 J9 PLOS BIOL JI PLoS. Biol. PD MAR PY 2007 VL 5 IS 3 BP 398 EP 431 AR e77 DI 10.1371/journal.pbio.0050077 PG 34 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA 150TW UT WOS:000245243500006 PM 17355176 ER PT J AU Small, LM AF Small, Lawrence M. TI A man in full (James Smithson) - From the secretary SO SMITHSONIAN LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 2007 VL 37 IS 12 BP 34 EP 34 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 137XX UT WOS:000244327500014 ER PT J AU Baudin, F Ibarra, E Avrett, EH Vial, JC Bocchialini, K Costa, A Lemaire, P Rovira, M AF Baudin, F. Ibarra, E. Avrett, E. H. Vial, J. -C. Bocchialini, K. Costa, A. Lemaire, P. Rovira, M. TI A contribution to the understanding of chromospheric oscillations SO SOLAR PHYSICS LA English DT Article ID SOLAR ATMOSPHERE; INTERNETWORK OSCILLATIONS; K-LINE; WAVES; SUMER; VELOCITY AB We present SUMER/SOHO UV measurements of chromospheric oscillations of intensity, velocity, and linewidth observed in C I, S I, O I, and C II lines, which are formed in the altitude range from 1000 km to 2000 km above tau(500) = 1. Oscillations in lines originating at similar altitudes exhibit different behaviors which we discuss in terms of the formation of the lines. C1 CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. Univ Paris Sud 11, F-91405 Orsay, France. Consejo Nacl Invest Cient & Tecn, Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Baudin, F (reprint author), CNRS, Inst Astrophys Spatiale, UMR 8617, Bat 121, F-91405 Orsay, France. EM frederic.baudin@ias.u-psud.fr NR 18 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAR PY 2007 VL 241 IS 1 BP 39 EP 51 DI 10.1007/s11207-007-0006-3 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 154JM UT WOS:000245503000005 ER PT J AU Jehl, JR AF Jehl, Joseph R., Jr. TI Why do Eared Grebes leave hypersaline lakes in autumn? SO WATERBIRDS LA English DT Article DE Eared Grebe; Podiceps nigricollis; Mono Lake; California; Great Salt Lake; Utah; foraging; prey; migration ID PODICEPS-NIGRICOLLIS; MIGRATION; UTAH AB Jehl (1988) observed that the departure of Eared Grebes Podiceps nigricollis from Mono Lake, California, a major fall staging area, did not occur in relation to time of year or weather but was initiated after the density of brine shrimp (Artemia monica)-the major prey-fell below a predictable threshold. Although Caudell and Conover (2006) found no such relationship at Great Salt Lake, the other major staging area, reevaluation of their data indicates that the threshold concept applies there as well. Substantial differences in the staging ecology of Eared Grebes at the two lakes remain to be demonstrated. C1 Smithsonian Inst, US Natl Museum Nat Hist, Smithsonian Ornithol, Washington, DC 20560 USA. RP Jehl, JR (reprint author), Smithsonian Inst, US Natl Museum Nat Hist, Smithsonian Ornithol, Washington, DC 20560 USA. EM grebe5k@cs.com NR 15 TC 10 Z9 10 U1 0 U2 5 PU WATERBIRD SOC PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 1524-4695 J9 WATERBIRDS JI Waterbirds PD MAR PY 2007 VL 30 IS 1 BP 112 EP 115 DI 10.1675/1524-4695(2007)030[0112:WDEGLH]2.0.CO;2 PG 4 WC Ornithology SC Zoology GA 162MX UT WOS:000246093100015 ER PT J AU Isler, ML Isler, PR Whitney, BM Zimmer, KJ AF Isler, Morton L. Isler, Phyllis R. Whitney, Bret M. Zimmer, Kevin J. TI Species limits in the "Schistocichla" complex of Percnostola antbirds (Passeriformes : Thamnophilidae) SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article ID VOCALIZATIONS AB The species-group in the genus Percnostola that is sometimes placed in the genus "Schistocichla" is shown to consist of seven, mostly allopatric, species. All seven are distinct morphologically; when their vocalizations were compared, 19 of 21 pairwise comparisons resulted in differences as great as or greater than those of syntopic species-pairs in this family. Differences in the two remaining comparisons were limited to two vocal characters, but one involved a pair whose ranges appear to abut without apparent physical barriers; members of the second pair were separated geographically by similar to 2,400 km. Insights into speciation in the complex are relevant to conservation efforts and ultimately will be related to an ongoing genetic study to suggest a phylogery and contribute to an understanding of avian evolution in Amazonia. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool Birds, Washington, DC 20560 USA. Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. Los Angeles Museum Nat Hist, Los Angeles, CA 90007 USA. RP Isler, ML (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool Birds, Washington, DC 20560 USA. EM antbird@cox.net NR 32 TC 9 Z9 14 U1 0 U2 2 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2007 VL 119 IS 1 BP 53 EP 70 DI 10.1676/05-121.1 PG 18 WC Ornithology SC Zoology GA 148YQ UT WOS:000245113700007 ER PT J AU Auer, SK Logue, DM Bassar, RD Gammon, DE AF Auer, Sonya K. Logue, David M. Bassar, Ronald D. Gammon, David E. TI Nesting biology of the Black-bellied Wren (Thryothorus fasciatoventris) in central Panama SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article ID BIRDS AB We describe the nest and nest site, and provide the first description of the eggs and nesting behavior of the Black-bellied Wren (Thryothorus fasciatoventris) in central Panama. Nine nests were found near tree-fall gaps, swamps, and roads in moist tropical forests. Nests were dome-shaped with a circular side entrance. They were composed chiefly of strips of dead palm fronds, and were generally built in places where leaf litter and other debris had accumulated at the convergence of several vines near the forest floor. Both males and females participated in building the nest. Clutch size was three, and eggs were laid on consecutive days. Egg color varied from creamy to beige with faint to dark brown speckles that were more concentrated at the blunt end. Females were the sole incubators, but males fed the incubating females. Only the female brooded the nestlings once they hatched, but both parents fed the nestlings. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Auer, SK (reprint author), Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. EM myioborus@yahoo.com NR 12 TC 2 Z9 2 U1 1 U2 2 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2007 VL 119 IS 1 BP 71 EP 76 DI 10.1676/06-008.1 PG 6 WC Ornithology SC Zoology GA 148YQ UT WOS:000245113700008 ER PT J AU Marley, A AF Marley, Anna TI Thomas Moran's west: Chromolithotraphy, high art, and popular taste. SO WINTERTHUR PORTFOLIO-A JOURNAL OF AMERICAN MATERIAL CULTURE LA English DT Book Review C1 Univ Delaware, Smithsonian Inst, Newark, DE 19716 USA. RP Marley, A (reprint author), Univ Delaware, Smithsonian Inst, Newark, DE 19716 USA. NR 5 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 0084-0416 J9 WINTERTHUR PORTFOLIO JI Winterthur Portfol.-J. Amer. Mater. Cult. PD SPR PY 2007 VL 41 IS 1 BP 94 EP 96 DI 10.1086/518918 PG 3 WC Art SC Art GA 169DV UT WOS:000246573800011 ER PT J AU Hershler, R Liu, HP Frest, TJ Johannes, EJ AF Hershler, Robert Liu, Hsiu-Ping Frest, Terrence J. Johannes, Edward J. TI Extensive diversification of pebblesnails (Lithoglyphidae : Fluminicola) in the upper Sacramento River basin, northwestern USA SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE biogeography; freshwater; Gastropoda; mitochondrial DNA; phylogenetics; taxonomy ID HYDROBIID SNAILS GASTROPODA; WESTERN UNITED-STATES; PHYLOGENETIC-RELATIONSHIPS; NORTHEASTERN CALIFORNIA; MOLECULAR SYSTEMATICS; RANGE TRANSITION; SIERRA-NEVADA; GREAT-BASIN; RISSOOIDEA; GENUS AB Mitochondrial DNA sequences from the cytochrome c oxidase subunit I (COI) and cytochrome b (cytb) genes were obtained from the nine extant, previously described species of the northwestern North American freshwater gastropod genus Fluminicola (commonly known as pebblesnails) and from a large number of taxonomically undescribed populations of these animals from the upper Sacramento River basin, California and Oregon, which is composed of the Sacramento River headwaters, and the McCloud and Pit Rivers. Phylogenetic analyses of separate and combined molecular datasets yielded well-supported and largely congruent trees delineating 13 genetically divergent and morphologically distinctive upper Sacramento basin lineages, which we describe as new species. These include two groups of closely related and geographically proximal species that are further united by unique radular or shell features. Most of these novelties have narrow geographical distributions and are restricted to headspring areas, whereas several are more wide ranging and typically occupy larger, well-integrated habitats. The highly endemic fauna of upper Sacramento River pebblesnails is not a single species flock, but instead a polyphyletic assemblage spread among four separate clades. Our phylogeny, together with the application of a COI molecular clock for Fluminicola, suggests that upper Sacramento River clades originated as a result of late Neogene separation of this basin from neighbouring regions (northwestern Great Basin, Klamath River basin), which is consistent with previous biogeographical hypotheses based on the distributions of fishes. The upper Sacramento River pebblesnails evolved in association with the complex late Cenozoic history of regional landscape and drainage and diversification was also facilitated by the invasion of and adaptation to insular spring habitats. Our findings are consistent with the generally limited dispersal ability and geologically ancient (mid-Tertiary) age of this genus and imply that other portions of northwestern North America may also harbour a large number of undescribed pebblesnail species. Journal compilation (c) 2007 The Linnean Society of London. C1 Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. DEIXIS Consultants, Seattle, WA 98115 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu NR 60 TC 24 Z9 25 U1 0 U2 6 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAR PY 2007 VL 149 IS 3 BP 371 EP 422 PG 52 WC Zoology SC Zoology GA 141DB UT WOS:000244556000004 ER PT J AU Anker, A Marin, IN AF Anker, Arthur Marin, Ivan N. TI Athanas anatidactylus sp nov., a new alpheid shrimp (Crustacea : Decapoda) associated with crinoids in the tropical western Pacific SO ZOOLOGICAL STUDIES LA English DT Article DE Alpheidae; shrimp; Athanas; crinoid; symbiosis ID CARIDEA; MUDFLATS AB Athanas anatidactylus sp. nov. is described on the basis of a holotype specimen collected in Nhatrang Bay, Vietnam, and an additional specimen from the Bohol Sea, the Philippines. The specimen from Nhatrang Bay was collected from a crinoid host. The new species is unique within the genus Athanas in having non-enlarged, symmetrical chelipeds ending in a peculiar claw with duckbill-shaped fingers, and the 3rd maxilliped having a broadened ultimate segment, distally armed with a row of strong spines. It is closely related to A. ornithorhynchus Banner and Banner, 1973, known as a facultative symbiont of filter-feeding brittle stars. An earlier report of a crinoid-associated Athanas (Bruce 1987) suggests that A. anatidactylus sp. nov. may also occur on the Great Barrier Reef, Australia. C1 Inst Smithsonian Invest Trop, Balboa, Ancon, Panama. Smithsonian Trop Res Inst, Naos Unit 0948, APO, AA 34002 USA. Russian Acad Sci, AN Severtsov Inst Ecol & Evolut, Lab Ecol & Morphol Marine Invertebrates, Moscow 119071, Russia. RP Anker, A (reprint author), Inst Smithsonian Invest Trop, Apartado 0843-03092, Balboa, Ancon, Panama. EM ankera@si.edu; coralliodecapoda@mail.ru NR 14 TC 10 Z9 12 U1 0 U2 0 PU ACAD SINICA INST ZOOLOGY PI TAIPEI PA EDITORIAL OFFICE, TAIPEI 115, TAIWAN SN 1021-5506 J9 ZOOL STUD JI Zool. Stud. PD MAR PY 2007 VL 46 IS 2 BP 162 EP 167 PG 6 WC Zoology SC Zoology GA 159ZZ UT WOS:000245907900005 ER PT J AU Vari, RP Castro, RMC AF Vari, Richard P. Castro, Ricardo M. C. TI New species of Astyanax (Ostariophysi : Characiformes : Characidae) from the upper Rio Parana system, Brazil SO COPEIA LA English DT Article ID RIVER-BASIN; ARGENTINA CHARACIFORMES; NORTHWESTERN ARGENTINA; GENUS; FISH AB Astyanax bockmanni, a new species of characid, is widespread in streams in the upper Rio Parana system of central, southeastern, and southern Brazil. Samples of the species were identified by previous authors as A. eigenmanniorum, a species originally described from far southern Brazil. Astyanax bockmanni differs from A. eigenmanniorum and all congeners in the combination of morphometric, meristic, and pigmentary features and details of oral dentition. Uncertainties concerning the generic placement of Astyanax paranahybae are discussed, and it is proposed that the species is a member of a clade within the Characidae that does not include Astyanax. C1 Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. Univ Sao Paulo, Fac Filosofia Ciencias & Letras, Dept Biol, Lab Ictiol Ribeirao Preto, BR-14040901 Ribeirao Preto, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Div Fishes, POB 37012,WG-14,MRC 159, Washington, DC 20013 USA. EM varir@si.edu; rmcastro@ffclrp.usp.br NR 48 TC 14 Z9 15 U1 0 U2 5 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD FEB 28 PY 2007 IS 1 BP 150 EP 162 DI 10.1643/0045-8511(2007)7[150:NSOAOC]2.0.CO;2 PG 13 WC Zoology SC Zoology GA 141YK UT WOS:000244614900013 ER PT J AU Hilton, EJ Britz, R Johnson, GD Forey, PL AF Hilton, Eric J. Britz, Ralf Johnson, G. David Forey, Peter L. TI Clarification of the occipito-vertebral region of Arapaima gigas (Osteoglossomorpha : Osteoglossidae) through developmental osteology SO COPEIA LA English DT Article ID TELEOSTEI; FOSSIL AB The structure and composition of the ventral portion of the occipital region of the skull in Arapaima gigas (Osteoglossidae) is unique among teleostean fishes, and past comparative anatomical studies have variously interpreted it as containing only the basioccipital or the basioccipital fused to one or two vertebral centra. By studying an ontogenetic series, we show that the dominant element of the ventral occipital region of the skull in Arapaima is the first vertebral centrum and its greatly enlarged parapophyses. The parapophyses, which become fused to the centrum, extend anteriorly to suture to the lateral portions of the parasphenoid. In the adult, the anterior portion of the basioccipital is flattened, with a narrow ventrally directed keel of bone that is exposed ventrally only along the midline of the skull. Although a general enlargement of the anteriormost parapophyses appears to be a synapomorphy of the family Osteoglossidae, their arrangement in other osteoglossids does not closely resemble that described herein for Arapaima. C1 Field Museum Nat Hist, Dept Geol, Chicago, IL 60605 USA. Nat Hist Museum, Dept Zool, London SW7 5BD, England. Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. RP Hilton, EJ (reprint author), Field Museum Nat Hist, Dept Geol, 1400 S Lake Shore Dr, Chicago, IL 60605 USA. EM ehilton@fieldmuseum.org; R.Britz@nhm.ac.uk; johnsond@si.edu; plf@nhm.ac.uk NR 32 TC 4 Z9 4 U1 2 U2 2 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD FEB 28 PY 2007 IS 1 BP 218 EP 224 DI 10.1643/0045-8511(2007)7[218:COTORO]2.0.CO;2 PG 7 WC Zoology SC Zoology GA 141YK UT WOS:000244614900021 ER PT J AU Roberts, TR AF Roberts, Tyson R. TI The "celestial pearl danio", a new genus and species of colourful minute cyprinid fish from Myanmar (Pisces : Cypriniformes) SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article DE Hopong; principal caudal fin rays; danioin mandibular notch, knob, and pad; captive breeding ID PIGMENT PATTERN; DIVERSIFICATION; VERTEBRATES; TELEOSTEI AB Celestichthys margaritatus, a new genus and species of Danioinae, is described from a rapidly developing locality in the Salween basin about 70-80 kin northeast of Inle Lake in northern Myanmar. Males and females are strikingly colouful. It is apparently most closely related to two danioins endemic to Inle, Microrasbora rubescens and "Microrasbora" erythromicron. The latter species may be congeneric with the new species. The new genus is identified as a danioin by specializations on its lower jaw and its numerous anal fin rays. The colouration, while highly distinctive, seems also to be characteristically danioin. The danioin notch (Roberts, 1986; Fang, 2003) is reduced or absent, but the danioin mandibular flap and bony knob (defined herein) are present. The anal fin has iii81/2-101/2 rays. In addition to its distinctive body spots and barred fins the new fish is distinguished from other species of danioins by the following combination of characters: snout and mouth extremely short; premaxillary with an elongate and very slender ascending process; mandible foreshortened; body deep, with rounded dorsal and anal fins; modal vertebral count 15+16=31; caudal fin moderately rather than deeply forked; principal caudal fin rays 9/8; scales vertically ovoid; and pharyngeal teeth conical, in three rows. C1 Smithsonian Trop Res Inst, Res Associate, Balboa, Panama. RP Roberts, TR (reprint author), Smithsonian Trop Res Inst, Res Associate, Balboa, Panama. EM tysonregalecus@yahoo.com NR 17 TC 10 Z9 10 U1 3 U2 10 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 FEB 28 PY 2007 VL 55 IS 1 BP 131 EP 140 PG 10 WC Zoology SC Zoology GA 159PW UT WOS:000245879600012 ER PT J AU Giman, B Stuebing, R Megum, N Mcshea, WJ Stewart, CM AF Giman, Belden Stuebing, Robert Megum, Nyegang Mcshea, William J. Stewart, Chad M. TI A camera trapping inventory for mammals in a mixed use planted forest in Sarawak SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article DE camera trapping; scent lures; planted forest; Sarawak ID TIGER; POPULATIONS AB A series of camera trapping surveys was done in and around an Acacia plantation in central Sarawak to monitor wildlife populations within the planted forest. The study area was divided into I km(2) blocks with two cameras placed in each block for thirty days at each position, and placed in five study areas for a period of approximately six months. Camera sites were baited with a variety of commercially available scent lures. During 1,632 trap-nights, a total of 25 species of mammals were detected and photographed, comprising 15 families, and 23 genera, including local Bearded Pig (Sus barbatus), Sambar Deer (Cervus unicolor), Sun Bear (Helarctos malayanus), and an Otter Civet (Cynogale bennettii). Some lures failed to attract any mammals, while oily lures such as Fish Oil, seemed to better withstand rain, increasing the long-term chances for obtaining species photographs. Magna Glan, producing a very strong odor, attracted numerous terrestrial mammals and remained detectable even to humans for at least one month, even during the rainy season. The implications of the results of this study for successfully monitoring tropical forest wildlife is discussed. C1 Smithsonian Inst, Front Royal, VA 22630 USA. Wildlife Conservat Soc, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Giman, B (reprint author), Grand Perfect Sdn Bhd 144,Lot 3430,1a Floor,Pk Ci, Sarawak, Indonesia. EM beldengiman@yahoo.com NR 21 TC 18 Z9 22 U1 3 U2 34 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 FEB 28 PY 2007 VL 55 IS 1 BP 209 EP 215 PG 7 WC Zoology SC Zoology GA 159PW UT WOS:000245879600023 ER PT J AU Dickau, R Ranere, AJ Cooke, RG AF Dickau, Ruth Ranere, Anthony J. Cooke, Richard G. TI Starch grain evidence for the preceramic dispersals of maize and root crops into tropical dry and humid forests of Panama SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE agricultural origins; crop dispersals; Neotropics; starch grain analysis ID COASTAL ECUADOR; LAND-BRIDGE; DOMESTICATION; AGRICULTURE; RECORD; COLONIZATION; CULTIVATION; CUCURBITA; PHYTOLITH; HISTORY AB The Central American isthmus was a major dispersal route for plant taxa originally brought under cultivation in the domestication centers of southern Mexico and northern South America. Recently developed methodologies in the archaeological and biological sciences are providing increasing amounts of data regarding the timing and nature of these dispersals and the associated transition to food production in various regions. One of these methodologies, starch grain analysis, recovers identifiable microfossils of economic plants directly off the stone tools used to process them. We report on new starch grain evidence from Panama demonstrating the early spread of three important New World cultigens: maize (Zea mays), manioc (Manihot esculenta), and arrowroot (Maranta arundinacea). Maize starch recovered from stone tools at a site located in the Pacific lowlands of central Panama confirms previous archaeobotanical evidence for the use of maize there by 7800-7000 cal BP. Starch evidence from preceramic sites in the less seasonal, humid premontane forests of Chiriqui province, western Panama, shows that maize and root crops were present by 7400-5600 cal BP, several millennia earlier than previously documented. Several local starchy resources, including Zamia and Dioscorea spp., were also used. The data from both regions suggest that crop dispersals took place via diffusion or exchange of plant germplasm rather than movement of human populations practicing agriculture. C1 Univ Calgary, Dept Archaeol, Calgary, AB T2N 1N4, Canada. Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Dickau, R (reprint author), Univ Calgary, Dept Archaeol, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. EM redickau@ucalgary.ca NR 56 TC 76 Z9 80 U1 0 U2 15 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 27 PY 2007 VL 104 IS 9 BP 3651 EP 3656 DI 10.1073/pnas.0611605104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 142PG UT WOS:000244661400110 PM 17360697 ER PT J AU Mallet, J Beltran, M Neukirchen, W Linares, M AF Mallet, James Beltran, Margarita Neukirchen, Walter Linares, Mauricio TI Natural hybridization in heliconiine butterflies: the species boundary as a continuum SO BMC EVOLUTIONARY BIOLOGY LA English DT Review ID PASSION-VINE BUTTERFLIES; MITOCHONDRIAL-DNA; HYBRID ZONES; GENE FLOW; ADAPTIVE RADIATION; MULLERIAN MIMICRY; LEPIDOPTERA-NYMPHALIDAE; REPRODUCTIVE ISOLATION; SYMPATRIC SPECIATION; CLOSE RELATIVES AB Background: To understand speciation and the maintenance of taxa as separate entities, we need information about natural hybridization and gene flow among species. Results: Interspecific hybrids occur regularly in Heliconius and Eueides (Lepidoptera: Nymphalidae) in the wild: 26-29% of the species of Heliconiina are involved, depending on species concept employed. Hybridization is, however, rare on a per-individual basis. For one well-studied case of species hybridizing in parapatric contact (Heliconius erato and H. himera), phenotypically detectable hybrids form around 10% of the population, but for species in sympatry hybrids usually form less than 0.05% of individuals. There is a roughly exponential decline with genetic distance in the numbers of natural hybrids in collections, both between and within species, suggesting a simple "exponential failure law" of compatibility as found in some prokaryotes. Conclusion: Hybridization between species of Heliconius appears to be a natural phenomenon; there is no evidence that it has been enhanced by recent human habitat disturbance. In some well-studied cases, backcrossing occurs in the field and fertile backcrosses have been verified in insectaries, which indicates that introgression is likely, and recent molecular work shows that alleles at some but not all loci are exchanged between pairs of sympatric, hybridizing species. Molecular clock dating suggests that gene exchange may continue for more than 3 million years after speciation. In addition, one species, H. heurippa, appears to have formed as a result of hybrid speciation. Introgression may often contribute to adaptive evolution as well as sometimes to speciation itself, via hybrid speciation. Geographic races and species that coexist in sympatry therefore form part of a continuum in terms of hybridization rates or probability of gene flow. This finding concurs with the view that processes leading to speciation are continuous, rather than sudden, and that they are the same as those operating within species, rather than requiring special punctuated effects or complete allopatry. Although not qualitatively distinct from geographic races, nor "real" in terms of phylogenetic species concepts or the biological species concept, hybridizing species of Heliconius are stably distinct in sympatry, and remain useful groups for predicting morphological, ecological, behavioural and genetic characteristics. C1 UCL, Galton Lab, London NW1 2HE, England. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Smithsonian Trop Res Inst, Balboa, Panama. Univ Los Andes, Inst Genet, Dept Ciencias Biol, Bogota, Colombia. RP Mallet, J (reprint author), UCL, Galton Lab, Wolfson House,4 Stephenson Way, London NW1 2HE, England. EM j.mallet@ucl.ac.uk; beltran.margarita@gmail.com; walter.neukirchen@arcor.de; mlinares@uniandes.edu.co RI mallet, james/B-5114-2008; Linares, Mauricio/I-3509-2016 OI Linares, Mauricio/0000-0002-1021-0226 NR 102 TC 121 Z9 127 U1 6 U2 66 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD FEB 23 PY 2007 VL 7 AR 28 DI 10.1186/1471-2148-7-28 PG 16 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 146LX UT WOS:000244937000001 PM 17319954 ER PT J AU Norris, DR Marra, PP Kyser, TK Ratcliffe, LM Montgomerie, R AF Norris, D. Ryan Marra, Peter P. Kyser, T. Kurt Ratcliffe, Laurene M. Montgomerie, Robert TI Continent-wide variation in feather colour of a migratory songbird in relation to body condition and moulting locality SO BIOLOGY LETTERS LA English DT Article DE migration; carotenoids; stable isotopes; feather growth ID SEXUAL SELECTION; PLUMAGE COLOR; HOUSE FINCH; CAROTENOIDS; SIGNALS AB Understanding the causes of variation in feather colour in free-living migratory birds has been challenging owing to our inability to track individuals during the moulting period when colours are acquired. Using stable-hydrogen isotopes to estimate moulting locality, we show that the carotenoid-based yellow - orange colour of American redstart (Setophaga ruticilla) tail feathers sampled on the wintering grounds in Central America and the Caribbean is related to the location where feathers were grown the previous season across North America. Males that moulted at southerly latitudes were more likely to grow yellowish feathers compared with males that moulted more orange - red feathers further north. Independent samples obtained on both the breeding and the wintering grounds showed that red chroma - an index of carotenoid content - was not related to the mean daily feather growth rate, suggesting that condition during moult did not influence feather colour. Thus, our results support the hypothesis that feather colour is influenced by ecological conditions at the locations where the birds moulted. We suggest that these colour signals may be influenced by geographical variation in diet related to the availability of carotenoids. C1 Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. Queens Univ, Dept Geol Sci & Geol Engn, Kingston, ON K7L 3N6, Canada. Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. RP Norris, DR (reprint author), Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. EM rnorris@uoguelph.ca RI Montgomerie, Robert/C-6516-2008; Norris, Ryan/F-4720-2011 OI Montgomerie, Robert/0000-0003-4701-4525; NR 15 TC 15 Z9 16 U1 0 U2 10 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD FEB 22 PY 2007 VL 3 IS 1 BP 16 EP 19 DI 10.1098/rsbl.2006.0572 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 126AY UT WOS:000243485800005 PM 17443954 ER PT J AU Dye, S Eales, SA Ashby, MLN Huang, JS Egami, E Brodwin, M Lilly, S Webb, T AF Dye, S. Eales, S. A. Ashby, M. L. N. Huang, J. -S. Egami, E. Brodwin, M. Lilly, S. Webb, T. TI A SCUBA/Spitzer investigation of the far-infrared extragalactic background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE infrared : galaxies; submillimetre ID SPITZER-SPACE-TELESCOPE; 14 HOUR FIELD; MULTIBAND IMAGING PHOTOMETER; DEEP SUBMILLIMETER SURVEY; EXPERIMENT SEARCH; SOURCE COUNTS; GALAXY SURVEY; SCUBA; IDENTIFICATIONS; DETECTIONS AB We have measured the contribution of submillimetre and mid-infrared sources to the extragalactic background radiation at 70 and 160 mu m. Specifically, we have stacked flux in 70- and 160-mu m Spitzer Space Telescope (Spitzer) observations of the Canada-United Kingdom Deep Submillimetre Survey 14-h field at the positions of 850-mu m sources detected by SCUBA and also 8- and 24-mu m sources detected by Spitzer. We find that per source, the SCUBA galaxies are the strongest and the 8-mu m sources the weakest contributors to the background flux at both 70 and 160 mu m. Our estimate of the contribution of the SCUBA sources is higher than previous estimates. However, expressed as a total contribution, the full 8-mu m source catalogue accounts for twice the total 24-mu m source contribution and similar to 10 times the total SCUBA source contribution. The 8-mu m sources account for the majority of the background radiation at 160 mu m with a flux of 0.87 +/- 0.16 MJy sr(-1) and at least a third at 70 mu m with a flux of 0.103 +/- 0.019 MJy sr(-1). These measurements are consistent with current lower limits on the background at 70 and 160 mu m. Finally, we have investigated the 70- and 160-mu m emission from the 8- and 24-mu m sources as a function of redshift. We find that the average 70-mu m flux per 24-mu m source and the average 160-mu m flux per 8- and 24-mu m source is constant over all redshifts, up to z similar to 4. In contrast, the low-redshift half (z < 1) of the of 8-mu m sample contributes approximately four times the total 70-mu m flux of the high-redshift half. These trends can be explained by a single non-evolving SED. C1 Univ Cardiff Wales, Sch Phys & Astron, Cardiff CF24 3AA, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. ETH, Astron Inst, CH-8093 Zurich, Switzerland. Sterrewacht Leiden, NL-233 CA Leiden, Netherlands. RP Dye, S (reprint author), Univ Cardiff Wales, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, Wales. EM s.dye@astro.cf.ac.uk OI Dye, Simon/0000-0002-1318-8343 NR 29 TC 18 Z9 18 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2007 VL 375 IS 2 BP 725 EP 734 DI 10.1111/j.1365-2966.2006.11340.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134KY UT WOS:000244083100027 ER PT J AU Wagg, J Hughes, DH Aretxaga, I Chapin, EL Dunlop, JS Gaztanaga, E Devlin, M AF Wagg, J. Hughes, D. H. Aretxaga, I. Chapin, E. L. Dunlop, J. S. Gaztanaga, E. Devlin, M. TI A broad-band spectroscopic search for CO line emission in HDF850.1: the brightest submillimetre object in the Hubble Deep Field-north SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual; HDF850.1; galaxies : starburst; cosmology : observations; radio lines : galaxies ID SPECTRAL ENERGY-DISTRIBUTION; UNIVERSE GALAXY SURVEY; QUASAR HOST GALAXIES; MOLECULAR GAS; NUMBER COUNTS; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS; ULTRALUMINOUS GALAXY; INFRARED GALAXIES; LENSING CLUSTERS AB Using the 100-m Green Bank Telescope, we have conducted a cm-wavelength search for CO J = 1-0 line emission towards the high-redshift, far-infrared (FIR) luminous object HDF850.1 over the redshift interval 3.3 less than or similar to z less than or similar to 5.4. Despite the wealth of existing multiwavelength observations, and the recent identification of a galaxy counterpart in deep K'-band (2.2 mu m) imaging, an unambiguous spectroscopic redshift has not yet been obtained for this object. A FIR-to-radio wavelength photometric redshift technique, however, predicts a similar to 90 per cent probability that the redshift is in the range, 3.3 less than or similar to z less than or similar to 5.4 (equivalent to an observed redshifted CO J= 1-0 emission line frequency, 26.5 greater than or similar to nu(obs) greater than or similar to 18.0 GHz), making HDF850.1 a potential occupant of the 'high-redshift tail' of submillimetre (submm)-selected galaxies. We have also conducted a search for CO J = 2-1 line emission over the narrower redshift range, 3.9 less than or similar to z less than or similar to 4.3. Although we do not detect any CO line emission in this object, our limits to the CO line luminosity are in broad agreement with the median value measured in the current sample of high-redshift, submm-selected objects detected in high-J CO line emission, but not sufficient to fully test the validity of the photometric redshift technique. C1 INAOE, Puebla 72000, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Edinburgh, Royal Observ, Astron Inst, SUPA Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. CSIC, IEEC, ES-08034 Barcelona, Spain. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Wagg, J (reprint author), INAOE, Apartado Postal 51&216, Puebla 72000, Mexico. EM jwagg@inaoep.mx RI Gaztanaga, Enrique/L-4894-2014 OI Gaztanaga, Enrique/0000-0001-9632-0815 NR 62 TC 10 Z9 10 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2007 VL 375 IS 2 BP 745 EP 752 DI 10.1111/j.1365-2966.2006.11352.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134KY UT WOS:000244083100029 ER PT J AU Fish, VL Reid, MJ AF Fish, Vincent L. Reid, Mark J. TI Large magnetic fields and motions of OH masers in W75N SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (W75N); ISM : kinematics and dynamics; magnetic fields; masers; radio lines : ISM; stars : formation ID FULL-POLARIZATION OBSERVATIONS; YOUNG STELLAR OBJECTS; STAR-FORMING-REGIONS; PROPER MOTIONS; WATER-VAPOR; CEPHEUS-A; OUTFLOW; EMISSION; COLLIMATION; EVOLUTION AB We report on a second epoch of VLBA observations of the 1665 and 1667 MHz OH masers in the massive star-forming region W75N. We find evidence to confirm the existence of very strong (similar to 40mG) magnetic fields near source VLA 2. Themasers near VLA 2 are dynamically distinct and include a very bright spot apparently moving at 50 km s(-1) relative to those around VLA 1. This fast-moving spotmay be an example of a rare class of OH masers seen in outflows in starforming regions. Due to the variability of these masers and the rapidity of their motions, tracking these motions will require multiple observations over a significantly shorter time baseline than obtained here. Proper motions of the masers near VLA 1 are more suggestive of streaming along magnetized shocks rather than Keplerian rotation in a disk. The motions of the easternmost cluster of masers in W75N(B) may be tracing slow expansion around an unseen exciting source. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 31 TC 10 Z9 10 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2007 VL 656 IS 2 BP 952 EP 958 DI 10.1086/510578 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 138BG UT WOS:000244336900031 ER PT J AU Perry, L Dickau, R Zarrillo, S Holst, I Pearsall, DM Piperno, DR Berman, MJ Cooke, RG Rademaker, K Ranere, AJ Raymond, JS Sandweiss, DH Scaramelli, F Tarble, K Zeidler, JA AF Perry, Linda Dickau, Ruth Zarrillo, Sonia Holst, Irene Pearsall, Deborah M. Piperno, Dolores R. Berman, Mary Jane Cooke, Richard G. Rademaker, Kurt Ranere, Anthony J. Raymond, J. Scott Sandweiss, Daniel H. Scaramelli, Franz Tarble, Kay Zeidler, James A. TI Starch fossils and the domestication and dispersal of chili peppers (Capsicum spp. L.) in the Americas SO SCIENCE LA English DT Article ID 3 DOG SITE; ORINOCO VALLEY; SAN-SALVADOR; REAL-ALTO; VENEZUELA; ARTIFACTS; BAHAMAS; REVEAL; PLANTS; MAIZE AB Chili peppers ( Capsicum spp.) are widely cultivated food plants that arose in the Americas and are now incorporated into cuisines worldwide. Here, we report a genus-specific starch morphotype that provides a means to identify chili peppers from archaeological contexts and trace both their domestication and dispersal. These starch microfossils have been found at seven sites dating from 6000 years before present to European contact and ranging from the Bahamas to southern Peru. The starch grain assemblages demonstrate that maize and chilies occurred together as an ancient and widespread Neotropical plant food complex that predates pottery in some regions. C1 Smithsonian Natl Museum Nat Hist, Archaeobiol Program, Dept Anthropol, Washington, DC 20013 USA. Univ Calgary, Dept Archaeol, Calgary, AB T2N 1N4, Canada. Smithsonian Trop Res Inst, Balboa 03092, Panama. Univ Missouri, Dept Anthropol, Columbia, MO 65211 USA. Miami Univ, Ctr Amer & World Cult, Oxford, OH 45056 USA. Univ Maine, Climate Change Inst, Orono, ME 04469 USA. Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. Univ Maine, Dept Anthropol, Orono, ME 04469 USA. Carretera Panamer, Ctr Antropol, Inst Venezolano Invest Cient, Altos De Pipe, Venezuela. Cent Univ Venezuela, Dept Arqueol Etnohist & Ecol Cult, Escuela Antropol, Fac Ciencias Econ & Sociales, Caracas 1041, Venezuela. Colorado State Univ, Ctr Environm Management Mil Lands, Ft Collins, CO 80523 USA. RP Perry, L (reprint author), Smithsonian Natl Museum Nat Hist, Archaeobiol Program, Dept Anthropol, POB 37012, Washington, DC 20013 USA. NR 29 TC 125 Z9 140 U1 8 U2 40 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 16 PY 2007 VL 315 IS 5814 BP 986 EP 988 DI 10.1126/science.1136914 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 136MW UT WOS:000244229800041 PM 17303753 ER PT J AU Warkentin, KM Caldwell, MS Siok, TD D'Amato, AT McDaniel, JG AF Warkentin, Karen M. Caldwell, Michael S. Siok, Timothy D. D'Amato, Alison T. McDaniel, J. Gregory TI Flexible information sampling in vibrational assessment of predation risk by red-eyed treefrog embryos SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE hatching; predator detection; playback; prey uncertainty; seismic; vibration; Leptophis ahaetulla; Leptodeira annulata; Agalychnis callidryas ID AGALYCHNIS-CALLIDRYAS; HATCHING ENZYME; EGGS; FROG; COMMUNICATION; MECHANISMS; AMPHIBIANS; BEHAVIOR; WASPS; CUES AB Prey assessing risk may miss cues and fail to defend themselves, or respond unnecessarily to false alarms. Error rates can be ameliorated with more information, but sampling predator cues entails risk. Red-eyed treefrogs have arboreal eggs and aquatic tadpoles. The embryos use vibrations in snake attacks to cue behaviorally mediated premature hatching, and escape, but vibrations from benign sources rarely induce hatching. Missed cues and false alarms are costly; embryos that fail to hatch are eaten and hatching prematurely increases predation by aquatic predators. Embryos use vibration duration and spacing to inform their hatching decision. This information accrues with cycles of vibration, while risk accrues over time as snakes feed. We used vibration playback experiments to test if embryos adjust sampling of information based on its cost, and measured latency to initiate hatching in videotaped snake attacks. Embryos did not initiate hatching immediately in attacks or playbacks, and the delay varied with the rate at which information accrued. Embryos started hatching sooner in response to stimuli with shorter cycles but sampled fewer cycles (less information) of longer-cycle stimuli before hatching. This flexible sampling is consistent with embryos balancing a trade-off between the value and cost of information. C1 Boston Univ, Dept Biol, Boston, MA 02215 USA. Smithsonian Trop Res Inst, Balboa, Panama. Boston Univ, Dept Aerosp & Mech Engn, Boston, MA 02215 USA. RP Warkentin, KM (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM kwarken@bu.edu NR 40 TC 24 Z9 24 U1 0 U2 14 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD FEB 15 PY 2007 VL 210 IS 4 BP 614 EP 619 DI 10.1242/jeb.001362 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 142ER UT WOS:000244632700012 PM 17267647 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Full of grace: A journey through the history of childhood 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 REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 2007 VL 132 IS 3 BP 121 EP 121 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 134RZ UT WOS:000244103000088 ER PT J AU Rueda, LM Zhao, TY Ma, YJ Gao, Q Ding, ZG Khuntirat, B Sattabongkot, J Wilkerson, RC AF Rueda, Leopoldo M. Zhao, Tongyan Ma, Yajun Gao, Qi Ding, Zhu Guo Khuntirat, Benjawan Sattabongkot, Jetsumon Wilkerson, Richard C. TI Updated distribution records of the Anopheles (Anopheles) hyrcanus species-group (Diptera : Culicidae) in China SO ZOOTAXA LA English DT Article DE Anopheles; Hyrcanus group; Diptera; Culicidae; mosquitoes; malaria; China ID PHYLOGENETIC-RELATIONSHIPS AB Mosquito collections were carried out during July-August 2005 in China. The known distribution of Anopheles hyrcanus species-group in China is updated based on published records and original observations. Twenty-one of about 30 known species of the Old World Hyrcanus group (Anopheles subgenus Anopheles), including An. belenrae Rueda, were recorded in 24 provinces and 2 cities. Anopheles sinensis Wiedemann, recorded in 21 provinces and 2 cities, is the most widely distributed species, followed by An. pullus Yamada and An. kweingyangensis Yao and Wu. The status of the type specimens of some Hyrcanus group species and their importance in disease transmission are also noted. C1 Walter Reed Army Inst Res, Dept Entomol, Walter Reed Biosystemat Unit, Silver Spring, MD 20910 USA. Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD 20746 USA. Beijing Inst Microbiol & Epidemiol, State Key Lab Pathogen & Biosecur, Beijing 100071, Peoples R China. Second Mil Med Univ, Dept Etiol Biol, Shanghai 200433, Peoples R China. Jiangsu Inst Parasit Dis, Wuxi 214064, Jiangsu, Peoples R China. USAMC, AFRIMS, Dept Entomol, Bangkok 10400, Thailand. RP Rueda, LM (reprint author), Walter Reed Army Inst Res, Dept Entomol, Walter Reed Biosystemat Unit, Silver Spring, MD 20910 USA. EM ruedapol@si.edu NR 25 TC 16 Z9 17 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 15 PY 2007 IS 1407 BP 43 EP 55 PG 13 WC Zoology SC Zoology GA 136UZ UT WOS:000244250900005 ER PT J AU Sauvage, B Martin, RV van Donkelaar, A Liu, X Chance, K Jaegle, L Palmer, PI Wu, S Fu, TM AF Sauvage, B. Martin, R. V. van Donkelaar, A. Liu, X. Chance, K. Jaegle, L. Palmer, P. I. Wu, S. Fu, T. -M. TI Remote sensed and in situ constraints on processes affecting tropical tropospheric ozone SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Review ID OPTICAL TRANSIENT DETECTOR; CHEMICAL-TRANSPORT MODELS; MONITORING EXPERIMENT; CARBON-MONOXIDE; NOX EMISSIONS; MINERAL DUST; LIGHTNING DISTRIBUTIONS; SATELLITE-OBSERVATIONS; VERTICAL-DISTRIBUTION; HETEROGENEOUS UPTAKE AB We use a global chemical transport model (GEOSChem) to evaluate the consistency of satellite measurements of lightning flashes and ozone precursors with in situ measurements of tropical tropospheric ozone. The measurements are tropospheric O-3, NO2, and HCHO columns from the GOME satellite instrument, lightning flashes from the OTD and LIS satellite instruments, profiles of O-3, CO, and relative humidity from the MOZAIC aircraft program, and profiles of O-3 from the SHADOZ ozonesonde network. We interpret these multiple data sources with our model to better understand what controls tropical tropospheric ozone. Tropical tropospheric ozone is mainly affected by lightning NOx and convection in the upper troposphere and by surface emissions in the lower troposphere. Scaling the spatial distribution of lightning in the model to the observed flashes improves the simulation of O-3 in the upper troposphere by 5 - 20 ppbv versus in situ observations and by 1 - 4 Dobson Units versus GOME retrievals of tropospheric O-3 columns. A lightning source strength of 6 +/- 2 Tg N/yr best represents in situ observations from aircraft and ozonesonde. Tropospheric NO2 and HCHO columns from GOME are applied to provide top-down constraints on emission inventories of NOx ( biomass burning and soils) and VOCs ( biomass burning). The top-down biomass burning inventory is larger than the bottom-up inventory by a factor of 2 for HCHO and alkenes, and by a factor of 2.6 for NOx over northern equatorial Africa. These emissions increase lower tropospheric O-3 by 5 - 20 ppbv, improving the simulation versus aircraft observations, and by 4 Dobson Units versus GOME observations of tropospheric O-3 columns. Emission factors in the a posteriori inventory are more consistent with a recent compilation from in situ measurements. The ozone simulation using two different dynamical schemes (GEOS-3 and GEOS-4) is evaluated versus observations; GEOS-4 better represents O-3 observations by 5 - 15 ppbv, reflecting enhanced convective detrainment in the upper troposphere. Heterogeneous uptake of HNO3 on aerosols reduces simulated O-3 by 5 - 7 ppbv, reducing a model bias versus in situ observations over and downwind of deserts. Exclusion of HO2 uptake on aerosols increases O-3 by 5 ppbv in biomass burning regions, reducing a model bias versus MOZAIC aircraft measurements. C1 Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Sauvage, B (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM bsauvage@fizz.phys.dal.ca RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Liu, Xiong/P-7186-2014; Fu, Tzung-May/N-3418-2015; Martin, Randall/A-2051-2008; Palmer, Paul/F-7008-2010 OI Martin, Randall/0000-0003-2632-8402; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577; NR 121 TC 80 Z9 81 U1 2 U2 29 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD FEB 14 PY 2007 VL 7 BP 815 EP 838 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 136LJ UT WOS:000244224100007 ER PT J AU McLaughlin, PA Lemaitre, R Ortiz, M AF McLaughlin, Patsy A. Lemaitre, Rafael Ortiz, Manuel TI Redescription of Pylocheles (Bathycheles) cubensis Ortiz & Gomez, 1986, the senior synonym of Pylocheles (B.) chacei Forest, 1987 (Decapoda, Anomura, Paguroidea, Pylochelidae) SO ZOOTAXA LA English DT Article DE Anomura; Paguroidea; Pylochelidae; Pylocheles; Bathycheles; P. (B.) cubensis; P. (B.) chacei; deep-water; Western Atlantic AB A reexamination of the holotypes of Pylocheles cubensis Ortiz & Gomez, 1986 and Pylocheles (Bathycheles) chacei Forest, 1987 has shown that these two deep-water taxa are identical. Pylocheles cubensis is the senior synonym and is assigned to the subgenus Bathycheles Forest, 1987, replacing P. (B.) chacei as the single Western Atlantic representative of the subgenus. Pylocheles (Bathycheles) cubensis is redescribed and illustrated. C1 Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20013 USA. Univ La Habana, Ctr Invest Marinas, Havana, Cuba. RP McLaughlin, PA (reprint author), Western Washington Univ, Shannon Point Marine Ctr, 1900 Shannon Point Rd, Anacortes, WA 98221 USA. EM hermit@fidalgo.net; lemaitrr@si.edu; ortiztouzet@yahoo.com NR 12 TC 2 Z9 2 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 12 PY 2007 IS 1406 BP 41 EP 46 PG 6 WC Zoology SC Zoology GA 134PY UT WOS:000244097000005 ER PT J AU Law, DR Steidel, CC Erb, DK Pettini, M Reddy, NA Shapley, AE Adelberger, KL Simenc, DJ AF Law, David R. Steidel, Charles C. Erb, Dawn K. Pettini, Max Reddy, Naveen A. Shapley, Alice E. Adelberger, Kurt L. Simenc, David J. TI The physical nature of rest-UV galaxy morphology during the peak epoch of galaxy formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : fundamental parameters; galaxies : high-redshift; galaxies : irregular; galaxies : starburst; galaxies : structure ID HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; INTEGRAL-FIELD SPECTROSCOPY; NUMBER-DENSITY EVOLUTION; GOODS-NORTH FIELD; STELLAR POPULATIONS; DEEP FIELD; Z-SIMILAR-TO-2 GALAXIES; HUBBLE SEQUENCE AB Motivated by the irregular and little-understood morphologies of z similar to 2-3 galaxies, we use nonparametric coefficients to quantify the morphologies of 216 galaxies that have been spectroscopically confirmed to lie at redshifts z = 1.8-3.4 in the GOODS-N field. Using measurements of UV and optical spectral lines, multiband photometric data, and stellar population models, we statistically assess possible correlations between galaxy morphology and physical observables such as stellar mass, star formation rate, and the strength of galaxy-scale outflows. We find evidence that dustier galaxies have more nebulous UV morphologies and that larger, more luminous galaxies may drive stronger outflows, but we otherwise conclude that UV morphology is either statistically decoupled from the majority of physical observables or determined by too complex a combination of physical processes to provide characterizations with predictive power. Given the absence of strong correlations between UV morphology and physical parameters such as star formation rates, we are therefore unable to support the hypothesis that morphologically irregular galaxies predominantly represent major galaxy mergers. Comparing galaxy samples, we find that IR-selected BzK galaxies and radio-selected submillimeter galaxies have UV morphologies similar to the optically selected sample, while distant red galaxies are more nebulous. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. McKinsey & Co Inc, Seattle, WA USA. RP Law, DR (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA. EM drlaw@astro.caltech.edu; ccs@astro.caltech.edu; derb@cfa.harvard.edu; pettini@ast.cam.ac.uk; nar@astro.caltech.edu; aes@astro.princeton.edu; kurt@ociw.edu; dsimenc@caltech.edu NR 54 TC 107 Z9 108 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2007 VL 656 IS 1 BP 1 EP 26 DI 10.1086/510357 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133SD UT WOS:000244032600001 ER PT J AU Greene, JE Ho, LC AF Greene, Jenny E. Ho, Luis C. TI X-ray properties of intermediate-mass black holes in active galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; galaxies : Seyfert; X-rays : galaxies ID SEYFERT 1 GALAXIES; QUASI-STELLAR OBJECTS; FE-II EMISSION; GALACTIC NUCLEI; RADIO-QUIET; CHANDRA SURVEY; NGC 4395; ENERGY-DISTRIBUTION; EDDINGTON RATIO; COMPLETE SAMPLE AB We present a pilot study of the X-ray properties of intermediate-mass (similar to 10(5)-10(6) M-circle dot) black holes in active galaxies using the Chandra X-ray telescope. Eight of the 10 active galaxies are detected with a significance of at least 3 sigma, with X-ray luminosities in the range L0.5-2keV approximate to 10(41)-10(43) ergs s(-1). The optical to X-ray flux ratios are consistent with expectations, given the known correlations between alpha(ox) and ultraviolet luminosity, while a couple of objects appear to be anomalously X-ray weak. The range of 0.5 to 2 keV photon indices we measure, 1 < Gamma(s) < 2.7, is entirely consistent with values found in samples of more luminous sources with more massive black holes. Black hole mass is evidently not a primary driver of soft X-ray spectral index. On the other hand, we do find evidence for a correlation between the X-ray power-law slope and both X-ray luminosity and Eddington ratio, which may suggest that X-ray emission mechanisms weaken at high Eddington ratios. Such a weakening may explain the anomalous X-ray weakness of one of our most optically luminous objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Greene, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 90 TC 43 Z9 43 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2007 VL 656 IS 1 BP 84 EP 92 DI 10.1086/509064 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133SD UT WOS:000244032600006 ER PT J AU Porras, A Jorgensen, JK Allen, LE Evans, NJ Bourke, TL Alcala, JM Dunham, MM Blake, GA Chapman, N Cieza, L Harvey, PM Huard, TL Koerner, DW Mundy, LG Myers, PC Padgett, DL Sargent, AI Stapelfeldt, KR Teuben, P van Dishoeck, EF Wahhaj, Z Young, KE AF Porras, Alicia Jorgensen, Jes K. Allen, Lori E. Evans, Neal J., II Bourke, Tyler L. Alcala, Juan M. Dunham, Michael M. Blake, Geoffrey A. Chapman, Nicholas Cieza, Lucas Harvey, Paul M. Huard, Tracy L. Koerner, David W. Mundy, Lee G. Myers, Philip C. Padgett, Deborah L. Sargent, Anneila I. Stapelfeldt, Karl R. Teuben, Peter van Dishoeck, Ewine F. Wahhaj, Zahed Young, Kaisa E. TI The SPITZER c2d survey of large, nearby, interstellar clouds. V. Chamaeleon II observed with IRAC SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : formation; stars : low-mass, brown dwarfs ID YOUNG STELLAR CLUSTER; HERBIG-HARO OBJECTS; ARRAY CAMERA IRAC; DARK-CLOUD; DENSE CORES; SPACE-TELESCOPE; MOLECULAR CLOUDS; STAR-FORMATION; BROWN DWARF; HH 54 AB We present IRAC (3.6, 4.5, 5.8, and 8.0 mu m) observations of the Chamaeleon II molecular cloud. The observed area covers about 1 deg(2) defined by A(V) > 2. Analysis of the data in the 2005 c2d catalogs reveals a small number of sources ( 40) with properties similar to those of young stellar or substellar objects (YSOs). The surface density of these YSO candidates is low, and contamination by background galaxies appears to be substantial, especially for sources classified as Class I or flat spectral energy distribution ( SED). We discuss this problem in some detail and conclude that very few of the candidate YSOs in early evolutionary stages are actually in the Cha II cloud. Using a refined set of criteria, we define a smaller, but more reliable, set of 24 YSO candidates. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAOE, Tonantzintla, Pue, Mexico. Univ Texas, Dept Astron, Austin, TX 78712 USA. Osserv Astron Capodimonte, INAF, Naples, Italy. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA USA. CALTECH, Div Phys Math & Astron, Pasadena, CA USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Leiden Observ, Leiden, Netherlands. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70310 USA. RP Porras, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM aporras@cfa.harvard.edu; jjorgensen@cfa.harvard.edu; leallen@cfa.harvard.edu; nje@astro.as.utexas.edu; tbourke@cfa.harvard.edu; jmae@sun1.na.astro.it; mdunham@astro.as.utexas.edu; gab@gps.caltech.edu; chapman@astro.umd.edu; lcieza@astro.as.utexas.edu; pmh@astro.as.utexas.edu; thuard@cfa.harvard.edu; david.koerner@nau.edu; lgm@astro.umd.edu; pmyers@cfa.harvard.edu; dlp@ipac.caltech.edu; afs@astro.caltech.edu; krs@exoplanet.jpl.nasa.gov; teuben@astro.umd.edu; ewine@strw.LeidenUniv.nl; Zahed.wahhaj@nau.ed; kaisa.young@gmail.com RI Stapelfeldt, Karl/D-2721-2012; OI Alcala, Juan Manuel/0000-0001-8657-095X NR 47 TC 35 Z9 35 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2007 VL 656 IS 1 BP 493 EP 504 DI 10.1086/510422 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133SD UT WOS:000244032600045 ER PT J AU Valencia, D Sasselov, DD O'Connell, RJ AF Valencia, Diana Sasselov, Dimitar D. O'Connell, Richard J. TI Radius and structure models of the first super-earth planet SO ASTROPHYSICAL JOURNAL LA English DT Article DE Earth; planetary systems; planets and satellites : individual (GJ 876d) ID STATIC COMPRESSION; BULK MODULUS; HEAT-FLOW; EQUATION; CONSTRAINTS; MANTLE; GPA; SATELLITE; H2O-ICE; SOLIDS AB With improving methods and surveys, the young field of extrasolar planet studies has recently expanded into a qualitatively new domain - terrestrial ( mostly rocky) planets. The first such planets were discovered during the past year and a half, judging by their measured masses of less than 10 M+ ("super-Earths''). They are introducing a novel physical regime that has not been explored before, as such planets do not exist in our solar system. Their compositions can be completely terrestrial, or they may harbor an extensive ocean ( water and ices) above a rocky core. We model the structure and properties of the first super-Earth ( mass similar to 7.5 M+), discovered in 2005, illustrating the possible compositions and providing radius evaluations in view of future detection of similar planets by transits. We find that there exists a threshold in radius above which a super-Earth most certainly has an extensive water content. In the case of GJ 876d, this threshold is at about 12,000 km. Our results show that unique characterization of the bulk composition of super-Earths will be possible with future transit studies. C1 Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Valencia, D (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM valencia@mail.geophysics.harvard.edu NR 38 TC 91 Z9 95 U1 2 U2 16 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2007 VL 656 IS 1 BP 545 EP 551 DI 10.1086/509800 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133SD UT WOS:000244032600050 ER PT J AU Bakos, GA Noyes, RW Kovacs, G Latham, DW Sasselov, DD Torres, G Fischer, DA Stefanik, RP Sato, B Johnson, JA Pal, A Marcy, GW Butler, RP Esquerdo, GA Stanek, KZ Lazar, J Papp, I Sari, P Sipocz, B AF Bakos, G. A. . Noyes, R. W. Kovacs, G. Latham, D. W. Sasselov, D. D. Torres, G. Fischer, D. A. Stefanik, R. P. Sato, B. Johnson, J. A. Pal, A. Marcy, G. W. Butler, R. P. Esquerdo, G. A. Stanek, K. Z. Lazar, J. Papp, I. Sari, P. Sipocz, B. TI HAT-P-1b: A large-radius, low-density exoplanet transiting one member of a stellar binary SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; planetary systems; stars : individual (ADS 16402AB) ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; HIGH-RESOLUTION SPECTROSCOPY; TESTING BLEND SCENARIOS; EXTRASOLAR GIANT PLANET; LIGHT-CURVE PROJECT; GALACTIC DISK; N2K CONSORTIUM; HOT JUPITERS; 2001 CAMPAIGN AB Using small automated telescopes in Arizona and Hawaii, the HATNet project has detected an object transiting one member of the double star system ADS 16402. This system is a pair of G0 main-sequence stars with age about 3 Gyr at a distance of similar to 139 pc and projected separation of similar to 1550 AU. The transit signal has a period of 4.46529 days and depth of 0.015 mag. From follow-up photometry and spectroscopy, we find that the object is a "hot Jupiter'' planet with mass about 0.53M(J) and radius similar to 1.36R(J) traveling in an orbit with semimajor axis 0.055 AU and inclination about 85.9 degrees, thus transiting the star at impact parameter 0.74 of the stellar radius. Based on a data set spanning 3 yr, ephemerides for the transit center are T(C) = 2453984.397 + Nu 4.46529. The planet, designated HAT-P-1b, appears to be at least as large in radius, and smaller in mean density, than any previously known planet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Konkoly Observ Budapest, Budapest, Hungary. San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. Natl Astron Observ, Okayama Astrophys Observ, Okayama, Japan. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20005 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Hungarian Astron Assoc, Budapest, Hungary. RP Bakos, GA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu; fischer@stars.sfsu.edu RI Butler, Robert/B-1125-2009; OI Fischer, Debra/0000-0003-2221-0861 NR 60 TC 139 Z9 140 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2007 VL 656 IS 1 BP 552 EP 559 DI 10.1086/509874 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133SD UT WOS:000244032600051 ER PT J AU Meibom, A Krot, AN Robert, F Mostefaoui, S Russell, SS Petaev, MI Gounelle, M AF Meibom, Anders Krot, Alexander N. Robert, Francois Mostefaoui, Smail Russell, Sara S. Petaev, Michael I. Gounelle, Matthieu TI Nitrogen and carbon isotopic composition of the Sun inferred from a high-temperature solar nebular condensate SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar system : general; solar wind ID MACROMOLECULAR ORGANIC-MATTER; INTERPLANETARY DUST PARTICLES; BOPP C/1995 O1; LUNAR REGOLITH; ABUNDANCES; ORIGIN; METEORITES; CHEMISTRY AB We report high-precision measurements of nitrogen and carbon isotopic compositions of a carbon-bearing titanium-nitride (osbornite) in a calcium-aluminum-rich inclusion (CAI) from the CH/CB-like carbonaceous chondrite Isheyevo. The mineralogy and petrography of the CAI and thermodynamic calculations indicate that the osbornite formed by gas-solid condensation in a high-temperature (similar to 2000 K) region of the solar nebula. Because isotopic fractionation at high temperature is small, the measured nitrogen [N-15/N-14 = (2.356 +/- 0.018) x 10(-3)] and carbon [C-13/C-12 = 0.01125 +/- 0.00008; 1 sigma] isotopic compositions of the Isheyevo osbornite are representative of the solar nebula and, hence, of the Sun. This conclusion is supported by the observations that ( 1) the measured C-13/C-12 ratio is indistinguishable from the spectroscopic determination of the C-13/C-12 ratio of the solar photosphere and ( 2) the measured N-15/N-14 ratio of osbornite is in excellent agreement with the Galileo spacecraft measurement of the nitrogen isotopic composition of the Jovian atmosphere, the second largest reservoir of nitrogen in the solar system. The inferred N-15/N-14 ratio of the solar nebula is also similar to the nitrogen isotopic composition of the vast majority of chondritic nanodiamonds, suggesting their solar nebula origin. C1 Museum Natl Hist Nat, Lab Etud Mat Extraterr, F-75231 Paris, France. Univ Hawaii Manoa, Hawaii Inst Geophys Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. Nat Hist Museum, Dept Mineral, London SW7 5BD, England. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Meibom, A (reprint author), Museum Natl Hist Nat, Lab Etud Mat Extraterr, F-75231 Paris, France. EM meibom@mnhn.fr; sasha@higp.hawaii.edu; robert@mnhn.fr; smail@mnhn.fr; sara.russell@nhm.ac.uk; mpetaev@cfa.harvard.edu; gounelle@mnhn.fr NR 33 TC 66 Z9 66 U1 1 U2 17 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2007 VL 656 IS 1 BP L33 EP L36 DI 10.1086/512052 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133SG UT WOS:000244032900009 ER PT J AU Ferguson, DC Schmidt, BC AF Ferguson, Douglas C. Schmidt, B. Christian TI Taxonomic review of the Grammia nevadensis species group (Lepidoptera : Arctiidae) with descriptions of two new species SO ZOOTAXA LA English DT Article DE Grammia; eureka; behrii; bowmani; nevadensis; superba; gibsoni; williamsii; incorrupta; Colorado; Utah; taxonomy; Arctiini AB Grammia nevadensis (Grote & Robinson) is revised to consist of four subspecies: nevadensis, geneura (Strecker) revised status, gibsoni (McDunnough) revised status and superba (Stretch). Grammia behrii (Stretch) revised status is raised from synonymy with G. nevadensis and re-described, and a neotype is designated. Two new species of Grammia in the nevadensis species group are described from the western United States: Grammia eureka new species is described from three specimens collected nearly a century ago in central Utah and one specimen ostensibly from southern Idaho. Grammia bowmani new species is a locally common species occurring in southwestern Colorado and southeastern Utah. The adults and male genitalic structures of G. nevadensis, G. behrii, G. incorrupta, G. williamsii, G. eureka and G. bowmani are illustrated. C1 Smithsonian Inst, USDA ARS, PSI, Systemat Entomol Lab, Washington, DC 20013 USA. Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. EM bjorn@ualberta.ca NR 13 TC 4 Z9 4 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 8 PY 2007 IS 1405 BP 39 EP 49 PG 11 WC Zoology SC Zoology GA 134IW UT WOS:000244077700002 ER PT J AU Broderick, AE Narayan, R AF Broderick, Avery E. Narayan, Ramesh TI Where are all the gravastars? Limits upon the gravastar model from accreting black holes SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID STABLE GRAVASTARS; GALACTIC-CENTER; SAGITTARIUS-A; STARS; ASTERISK; QUASARS; GROWTH; MASS AB The gravastar model, which postulates a strongly correlated thin shell of anisotropic matter surrounding a region of anti-de Sitter space, has been proposed as an alternative to black holes. We discuss constraints that presentday observations of well-known black hole candidates place on this model. We focus upon two black hole candidates known to have extraordinarily low luminosities: the supermassive black hole in the galactic centre, Sagittarius A*, and the stellar-mass black hole, XTE J1118 + 480. We find that the length scale for modifications of the type discussed in Chapline et al (2003 Int. J. Mod. Phys. 18 3587 - 90) must be sub-Planckian. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Broderick, AE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, MS 51,60 Garden St, Cambridge, MA 02138 USA. EM abroderick@cfa.harvard.edu; rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 20 TC 36 Z9 36 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD FEB 7 PY 2007 VL 24 IS 3 BP 659 EP 666 DI 10.1088/0264-9381/24/3/009 PG 8 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 125DP UT WOS:000243422500010 ER PT J AU Sternberg, LD Pinzon, MC Moreira, MZ Moutinho, P Rojas, EI Herre, EA AF Sternberg, Leonel da S. L. Pinzon, Maria Camila Moreira, Marcelo Z. Moutinho, Paulo Rojas, Enith I. Herre, Edward Allen TI Plants use macronutrients accumulated in leaf-cutting ant nests SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE leaf-cutting ants; Atta; nitrogen isotopes; nutrients; tropical forests; savannahs ID ROOT DISTRIBUTION; TROPICAL FORESTS; ATTA-CEPHALOTES; COLOMBICA; AMAZONIA; PASTURES; COLONIES; CALCIUM; GROWTH AB Leaf-cutting ants (Atta spp.) are known for their extensive defoliation in neo-tropical forests and savannahs. Debate about the costs and benefits of their activities has been largely dominated by their detrimental effects on agriculture and agroforestry. However, the large accumulation of nutrients and changes in soil properties near their nests might benefit plants growing near them. Here, we test whether trees use nutrients that accumulate in debris piles near, or refuse chambers within, leaf-cutting ant nests. At two tropical sites ( a moist tropical forest site in Panama and a savannah site in Brazil), we fed leaves labelled with the stable isotope N-15 to two species of leaf-cutting ants (Atta colombica and Atta laevigata) and traced the stable isotope label in plants surrounding the two nests. Thus, we show that plants in both sites access resources associated with Atta nests. In addition, leaf tissue of trees near the nests labelled with N-15 had significantly higher calcium concentrations than those of distal, unlabelled conspecifics. It has been documented that calcium is a limiting macronutrient in tropical forests and savannahs. Atta may thus play an important ecological role through their long-distance transport, redistribution and concentration of critical macronutrients. C1 Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. Ctr Energia Nucl Agr, Lab Ecol Isotop Avendia Centenario, BR-13400970 Sao Paulo, Brazil. Inst Pesquisa Ambiental Amazonia, BR-66035170 Belem, PA, Brazil. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Sternberg, LD (reprint author), Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. EM leo@bio.miami.edu RI Moreira, Marcelo/D-4622-2013 NR 27 TC 37 Z9 38 U1 4 U2 15 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD FEB 7 PY 2007 VL 274 IS 1608 BP 315 EP 321 DI 10.1098/rspb.2006.3746 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 124FV UT WOS:000243354100002 ER PT J AU Boul, KE Funk, WC Darst, CR Cannatella, DC Ryan, MJ AF Boul, Kathryn E. Funk, W. Chris Darst, Catherine R. Cannatella, David C. Ryan, Michael J. TI Sexual selection drives speciation in an Amazonian frog SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE speciation; sexual selection; Physalaemus; call variation; gene flow ID PUSTULOSUS SPECIES GROUP; PHYSALAEMUS-PUSTULOSUS; TUNGARA FROG; COMPLEX CALL; MATE CHOICE; PATTERNS; LEPTODACTYLIDAE; PREFERENCES; POPULATIONS; MORPHOLOGY AB One proposed mechanism of speciation is divergent sexual selection, whereby divergence in female preferences and male signals results in behavioural isolation. Despite the appeal of this hypothesis, evidence for it remains inconclusive. Here, we present several lines of evidence that sexual selection is driving behavioural isolation and speciation among populations of an Amazonian frog (Physalaemus petersi). First, sexual selection has promoted divergence in male mating calls and female preferences for calls between neighbouring populations, resulting in strong behavioural isolation. Second, phylogenetic analysis indicates that populations have become fixed for alternative call types several times throughout the species' range, and coalescent analysis rejects genetic drift as a cause for this pattern, suggesting that this divergence is due to selection. Finally, gene flow estimated with microsatellite loci is an average of 30 times lower between populations with different call types than between populations separated by a similar geographical distance with the same call type, demonstrating genetic divergence and incipient speciation. Taken together, these data provide strong evidence that sexual selection is driving behavioural isolation and speciation, supporting sexual selection as a cause for speciation in the wild. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Univ Texas, Texas Mem Museum, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Funk, WC (reprint author), USGS, Forest & Rangeland Ecosyst Sci Ctr, 3200 SW Jefferson Way, Corvallis, OR 97331 USA. EM cfunk@usgs.gov NR 45 TC 118 Z9 119 U1 2 U2 48 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD FEB 7 PY 2007 VL 274 IS 1608 BP 399 EP 406 DI 10.1098/rspb.2006.3736 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 124FV UT WOS:000243354100012 PM 17164204 ER PT J AU Niven, JE AF Niven, Jeremy E. TI Invertebrate memory: Wide-eyed ants retrieve visual snapshots SO CURRENT BIOLOGY LA English DT Editorial Material ID WOOD ANTS; LANDMARK GUIDANCE; FORMICA-RUFA; NAVIGATION; INSECTS; CUES AB Ants retrieve visual memories to guide them en route to their goal. A new study shows that wood ants use object width to retrieve the correct visual memory at the appropriate position along their route. A computational model that accurately reproduces the ants' behaviour raises questions about the underlying mechanisms. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Niven, JE (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM NivenJ@si.edu RI Niven, Jeremy/A-5883-2011 NR 9 TC 3 Z9 3 U1 0 U2 0 PU CELL PRESS PI CAMBRIDGE PA 1100 MASSACHUSETTS AVE, CAMBRIDGE, MA 02138 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD FEB 6 PY 2007 VL 17 IS 3 BP R85 EP R87 DI 10.1016/j.cub.2007.01.018 PG 3 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 135PE UT WOS:000244164700010 PM 17276905 ER PT J AU Ponssa, ML Heyer, WR AF Ponssa, Maria Laura Heyer, W. Ronald TI Osteological characterization of four putative species of the genus Adenomera (Anura : Leptodactylidae), with comments on intra- and interspecific variation SO ZOOTAXA LA English DT Article DE Leptodactylidae; osteology; Adenomera; taxonomy ID AMPHIBIA; ONTOGENY; LIFE AB Previous osteological characterizations of members of the frog genus Adenomera have been based on selected features. The purpose of this study is to establish a detailed osteological description of four putative species of the genus Adenomera. There is considerable variation, which we postulate corresponds to both intra- and interspecific variation. Osteology should provide a set of characters appropriate for cladistic analyses to help elucidate relationships within the Subfamily Leptodactylinae. Much of the adult osteological variation has a high probability of having evolved through the process of heterochrony. C1 Fdn Miguel Lillo, Inst Herpteol, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. Smithsonian Inst, Washington, DC 20013 USA. RP Ponssa, ML (reprint author), Fdn Miguel Lillo, Inst Herpteol, Miguel Lillo 251, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. EM mlponssa@arnet.com.ar; heyerr@si.edu NR 35 TC 15 Z9 15 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 5 PY 2007 IS 1403 BP 37 EP 54 PG 18 WC Zoology SC Zoology GA 133EI UT WOS:000243994800002 ER PT J AU Munthe, J Bodaly, RA Branfireun, BA Driscoll, CT Gilmour, CC Harris, R Horvat, M Lucotte, M Malm, O AF Munthe, John Bodaly, R. A. (Drew) Branfireun, Brian A. Driscoll, Charles T. Gilmour, Cynthia C. Harris, Reed Horvat, Milena Lucotte, Marc Malm, Olaf TI Recovery of mercury-contaminated fisheries SO AMBIO LA English DT Article; Proceedings Paper CT 8th International Conference on Mercury as a Global Pollutant CY AUG 06-11, 2006 CL Madison, WI SP Univ Wisconsin Madison, US Geol Survey, Univ Wisconsin La Crosse ID NORTHEASTERN NORTH-AMERICA; SULFATE-REDUCING BACTERIA; FRESH-WATER SEDIMENTS; DESULFOBULBUS-PROPIONICUS 1PR3; DISSOLVED ORGANIC-MATTER; FRANCISCO BAY-DELTA; LITTLE-ROCK LAKE; GULF-OF-TRIESTE; METHYL-MERCURY; METHYLMERCURY CONCENTRATIONS AB In this paper, we synthesize available information on the links between changes in ecosystem loading of inorganic mercury (Hg) and levels of methylmercury (MeHg) in fish. Although it is widely hypothesized that incroased Hg load to aquatic ecosystems leads to increases in MeHg in fish, there is limited quantitative data to test this hypothesis. Here we examine the available evidence from a range of sources: studies of ecosystems contaminated by industrial discharges, observations of fish MeHg responses to changes in atmospheric load, studies over space and environmental gradients, and experimental manipulations. A summary of the current understanding of the main processes involved in the transport and transformation from Hg load to MeHg in fish is provided. The role of Hg loading is discussed in context with other factors affecting Hg cycling and bioaccumulation in relation to timing and magnitude of response in fish MoHg. The main conclusion drawn is that changes in Hg loading (increase or decrease) will yield a response in fish MeHg but that the timing and magnitude of the response will vary depending of ecosystem-specific variables and the form of the Hg loaded. C1 Swedish Environm Res Inst, IVL, Dept Environm Effects & Atmospher Chem, SE-40014 Gothenburg, Sweden. Penobscot River Mercury Study Maine, Salt Spring Isl, BC V8K 2W5, Canada. Univ Toronto, Programs Environm, Mississauga, ON L5L 1C6, Canada. Syracuse Univ, Dept Civil & Environm Engn, Syracuse, NY 14244 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Tetra Tech Inc, Oakville, ON L6J 4E6, Canada. Josef Stefan Inst, Dept Environm Sci, SI-1000 Ljubljana, Slovenia. Univ Quebec, Geotop, Montreal, PQ H3C 3P8, Canada. Univ Fed Rural Rio de Janeiro, Lab Radioisotopos EPF, Inst Biofis CCF, BR-21941900 Rio De Janeiro, Brazil. RP Munthe, J (reprint author), Swedish Environm Res Inst, IVL, Dept Environm Effects & Atmospher Chem, POB 5302, SE-40014 Gothenburg, Sweden. EM john.munthe@ivl.se; drewbodaly@yahoo.ca; brian.branfireun@utoronto.ca; ctdrisco@mailbox.syr.edu; gilmourc@si.edu; rharris6@cogeco.ca; milena.horvat@ijs.si; lucotte.marc_michel@uqam.ca; olaf@biof.ufrj.br RI Malm, Olaf/H-1724-2012; Driscoll, Charles/F-9832-2014; Mason, Robert/A-6829-2011; Gilmour, Cynthia/G-1784-2010; OI Gilmour, Cynthia/0000-0002-1720-9498; Driscoll, Charles/0000-0003-2692-2890 NR 161 TC 185 Z9 188 U1 12 U2 83 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0044-7447 J9 AMBIO JI Ambio PD FEB PY 2007 VL 36 IS 1 BP 33 EP 44 DI 10.1579/0044-7447(2007)36[33:ROMF]2.0.CO;2 PG 12 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 144SY UT WOS:000244817800006 PM 17408189 ER PT J AU Eggens, F Popp, M Nepokroeff, M Wagner, WL Oxelman, B AF Eggens, Frida Popp, Magnus Nepokroeff, Molly Wagner, Warren L. Oxelman, Bengt TI The origin and number of introductions of the Hawaiian endemic Silene species (Caryophyllaceae) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Caryophyllaceae; Hawaiian Silene; ITS; phylogeny; RPB2; rps16; Silene antirrhina; woodiness ID NORTH-AMERICAN ORIGIN; RBCL SEQUENCE DATA; MOLECULAR EVIDENCE; PHYLOGENETIC ANALYSIS; GENUS PSYCHOTRIA; CHLOROPLAST DNA; EVOLUTION; COLONIZATION; DISPERSAL; ISLANDS AB The Hawaiian endemic Silene are a small group of woody or semiwoody representatives from a large, predominantly herbaceous, species-rich genus. We here investigated the origin and number of introductions of the endemic Hawaiian Silene based on phylogenetic relationships inferred from DNA sequences from both the plastid (the rps16 intron) and the nuclear (ribosomal internal transcribed sequences, ITS, and intron 23 of the RPB2 gene) genomes. Silene antirrhina, a widespread weedy American annual, is strongly supported as sister to a monophyletic group consisting of the Hawaiian Silene, indicating a single colonization event. There are no obvious morphological similarities between S. antirrhina and any of the species of Hawaiian Silene. Our results suggest an American origin for the Hawaiian endemics because that would require only a single trans-ocean dispersal. Two of the Hawaiian endemics (S. struthioloides and S. hawaiiensis) that form a subclade in the analyses have evolved woodiness after introduction to the Hawaiian Islands. Our results contribute to other recent results based on molecular phylogenetics that emphasize the American continent as a source area for the Hawaiian flora and support a striking morphological radiation and evolution of woodiness from a single introduction to the archipelago. C1 Univ Uppsala, Evolutionary Biol Ctr, Dept Systemat Bot, SE-75236 Uppsala, Sweden. Univ Oslo, Nat Hist Museum, Natl Ctr Biosystemat, NO-0318 Oslo, Norway. Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Natl Trop Bot Garden, Kalaheo, HI 96741 USA. RP Eggens, F (reprint author), Univ Uppsala, Evolutionary Biol Ctr, Dept Systemat Bot, Norbyvagen 18D, SE-75236 Uppsala, Sweden. EM frida.eggens@ebc.uu.se RI Oxelman, Bengt/F-2944-2010; Popp, Magnus/A-7481-2010 OI Oxelman, Bengt/0000-0002-6104-4264; NR 60 TC 25 Z9 27 U1 0 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 FEB PY 2007 VL 94 IS 2 BP 210 EP 218 DI 10.3732/ajb.94.2.210 PG 9 WC Plant Sciences SC Plant Sciences GA 136RM UT WOS:000244241800008 PM 21642223 ER PT J AU Lopano, CL Heaney, PJ Post, JE Hanson, J Komarneni, S AF Lopano, Christina L. Heaney, Peter J. Post, Jeffrey E. Hanson, Jonathan Komarneni, Sridiiar TI Time-resolved structural analysis of K- and Ba-exchange reactions with synthetic Na-birnessite using synchrotron X-ray diffraction SO AMERICAN MINERALOGIST LA English DT Article DE birnessite; cation exchange; synchrotron; X-ray diffraction; Mn-oxide ID POWDER DIFFRACTION; RIETVELD REFINEMENT; ION-EXCHANGE; MANGANESE; CRYSTALLIZATION; TRANSFORMATION; MANGANATES; TODOROKITE; PARAMETERS; MAGNESIUM AB Time-resolved Rietveld refinements using synchrotron X-ray diffraction (XRD) have documented real-time changes in unit-cell parameters in response to cation substitution in synthetic Na-birnessite. Potassium- and Ba-birnessite, like Na-birnessite, were found to have triclinic symmetry. Rietveld analyses of the XRD patterns for K- and Ba-exchanged birnessite revealed decreases in the a, c, and P unit-cell parameters, with a decrease of 1.7 and 0.5%, respectively, in unit-cell volume relative to Na-birnessite. Fourier electron difference syntheses revealed that the changes in the configuration of the interlayer species, and the charge, size, and hydration of the substituting cations, serve as the primary controls on changes in unit-cell parameters. Split electron density maxima with centers at (0 0 0.5) were present for Na, K, and Ba end-members; however, with increased substitution of K+ for Na+ the axis connecting the split-site maxima rotated from an orientation parallel to the b-axis to along the a-axis. Substitution of Ba2+ for Na+ did not result in rotation, but splitting of the interlayer site was more pronounced. C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian NMNH, Dept Mineral Sci, Washington, DC 20013 USA. Brookhaven Natl Lab, Dept Chem, Upton, NY 11973 USA. Penn State Univ, Dept Crop & Soil Sci, University Pk, PA 16802 USA. Penn State Univ, Inst Mat Res, University Pk, PA 16802 USA. RP Lopano, CL (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM clopano@geosc.psu.edu RI Hanson, jonathan/E-3517-2010 NR 38 TC 32 Z9 32 U1 0 U2 23 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD FEB-MAR PY 2007 VL 92 IS 2-3 BP 380 EP 387 DI 10.2138/am.2007.2242 PG 8 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 138SM UT WOS:000244382600014 ER PT J AU Casadio, F Douglas, JG Faber, KT AF Casadio, Francesca Douglas, Janet G. Faber, Katherine T. TI Noninvasive methods for the investigation of ancient Chinese jades: an integrated analytical approach SO ANALYTICAL AND BIOANALYTICAL CHEMISTRY LA English DT Article DE jade; nephrite; XRD; Raman spectroscopy; visible spectrophotometry ID RAMAN MICROPROBE; TREMOLITE AB This paper reports on an integrated analytical approach for the noninvasive characterization of Chinese nephrite samples, encompassing both geological reference specimens and museum objects. Natural variations induced by cationic substitutions, as well as human-induced alterations such as heating, which both affect color, are the focus of this contribution. Totally noninvasive methods of analysis were used, including X-ray fluorescence spectroscopy, Raman microspectroscopy, visible reflectance spectroscopy and X-ray diffraction; moreover, the feasibility of using a portable Raman spectrometer for the in-field identification of jades has been demonstrated. Fe/Fe+Mg (% p.f.u.) ratios of the jades have been calculated based on hydroxyl stretching Raman bands, which will provide an important addition to similar data that are being collected at major museums in the Western and Eastern hemispheres. C1 Art Inst Chicago, Dept Conservat Sci, Chicago, IL 60603 USA. Smithsonian Inst, Freer Gallery Art & Arthur M Sackler Gallery, Dept Conservat & Sci Res, Washington, DC 20560 USA. Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. RP Casadio, F (reprint author), Art Inst Chicago, Dept Conservat Sci, 111 S Michigan Ave, Chicago, IL 60603 USA. EM fcasadio@artic.edu RI Faber, Katherine/B-6741-2009 NR 27 TC 20 Z9 21 U1 2 U2 12 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1618-2642 J9 ANAL BIOANAL CHEM JI Anal. Bioanal. Chem. PD FEB PY 2007 VL 387 IS 3 BP 791 EP 801 DI 10.1007/s00216-006-0684-y PG 11 WC Biochemical Research Methods; Chemistry, Analytical SC Biochemistry & Molecular Biology; Chemistry GA 130RA UT WOS:000243815500007 PM 16912863 ER PT J AU Hawley, DM AF Hawley, D. M. TI Population bottlenecks: the importance of looking beyond genetics SO ANIMAL CONSERVATION LA English DT Editorial Material C1 Virginia Tech Univ, Dept Biol, Blacksburg, VA 24060 USA. Smithsonian Inst, Genet Program, Washington, DC USA. RP Hawley, DM (reprint author), Virginia Tech Univ, Dept Biol, Blacksburg, VA 24060 USA. EM hawleyd@vt.edu OI Hawley, Dana/0000-0001-9573-2914 NR 5 TC 1 Z9 1 U1 1 U2 5 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD FEB PY 2007 VL 10 IS 1 BP 17 EP 18 DI 10.1111/j.1469-1795.2006.00094.x PG 2 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 128ZB UT WOS:000243697100005 ER PT J AU Schulte, BA Freeman, EW Goodwin, TE Hollister-Smith, J Rasmussen, LEL AF Schulte, Bruce Alexander Freeman, Elizabeth Watson Goodwin, Thomas Elton Hollister-Smith, Julie Rasmussen, L. Elizabeth Little TI Honest signalling through chemicals by elephants with applications for care and conservation SO APPLIED ANIMAL BEHAVIOUR SCIENCE LA English DT Review DE communication; honesty; management; pheromone ID SOLID-PHASE MICROEXTRACTION; FEMALE ASIAN ELEPHANTS; MALE AFRICAN ELEPHANTS; LOXODONTA-AFRICANA; (Z)-7-DODECENYL ACETATE; PREOVULATORY PHEROMONE; MAXIMUS; BEHAVIOR; MUSTH; COMMUNICATION AB Chemical signals are difficult to fake because they are often directly associated with phenotype and physiological condition, and hence likely to be honest signals for intraspecific communication. Chemical signals may be modified after release by the sender or by the environment. The proximate and ultimate signal meanings are dependent not only on the condition of the sender, but also on the physiological status of the receiver. Understanding the relationships and linkage among signal modality, signal function and receiver response is an essential first step before using natural signals for animal care and conservation. Our studies on chemical communication in Asian and African elephants combine observational and experimental work in captive and wild settings to further this understanding. Recent discoveries of pheromones in Asian elephants and the biochemistry of these compounds provide strong evidence that such chemical signals are honest indicators of reproductive status. Chemically identifying the signals and verifying their functional context with statistically robust behavioural studies are essential aspects for understanding the communication system. Additionally, the investigative process of discovering, identifying and verifying the function of chemical signals among captive elephants offers safe and stimulating enrichments. The knowledge garnered from such studies has potential conservation benefits for managing wild elephant populations. A firm foundation of scientific information is required for successful behavioural investigations and applied conservation and enrichment components. (c) 2006 Elsevier B.V. All rights reserved. C1 Georgia So Univ, Dept Biol, Statesboro, GA 30460 USA. Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Hendrix Coll, Dept Chem, Conway, AR 72032 USA. Duke Univ, Dept Biol, Durham, NC 27708 USA. OHSU, Dept Environm & Biomol Syst, OGI Sch Sci & Engn, Beaverton, OR 97006 USA. RP Schulte, BA (reprint author), Georgia So Univ, Dept Biol, POB 8042, Statesboro, GA 30460 USA. EM bschulte@georgiasouthern.edu NR 110 TC 13 Z9 14 U1 4 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1591 J9 APPL ANIM BEHAV SCI JI Appl. Anim. Behav. Sci. PD FEB PY 2007 VL 102 IS 3-4 BP 344 EP 363 DI 10.1016/j.applanim.2006.05.035 PG 20 WC Agriculture, Dairy & Animal Science; Behavioral Sciences; Veterinary Sciences SC Agriculture; Behavioral Sciences; Veterinary Sciences GA 128PL UT WOS:000243670000010 ER PT J AU Stevenson, CM Wheeler, D Novak, SW Speakman, RJ Glascock, MD AF Stevenson, C. M. Wheeler, D. Novak, S. W. Speakman, R. J. Glascock, M. D. TI A new dating method for high-calcium archaeological glasses based upon surface-water diffusion: Preliminary calibrations and procedures SO ARCHAEOMETRY LA English DT Article DE alkali exchange; dating; diffusion; glass; infrared; mean ceramic date; Monticello; SIMS; vapour hydration ID LIME-SILICA GLASSES; MELTING CHARACTERISTICS; CHEMICAL DURABILITY; RELATIVE-HUMIDITY; HYDRATION; HYDROGEN; MEDIEVAL AB The first European settlers came to North America in the early 17th century using glass in the form of containers and decorative objects. Thus, glass is a horizon marker for all historic period settlements and a potential source of chronometric dates at archaeological sites belonging to the historic period in the Americas. We have developed a new absolute dating method based upon water diffusion into the surface of manufactured glasses that predicts diffusion coefficients based upon variation in glass chemical constituents. Low-temperature (< 190 degrees C) hydration experiments have been performed on a set of five high-calcium (21.7-28.3%) glasses that were used to manufacture wine bottles from the 17th-19th centuries. Infrared spectroscopy and secondary ion mass spectrometry was used to model the water diffusion/alkali exchange process. The ability of the model to accurately predict archaeological ages was evaluated with artefacts recovered from ceramic-dated contexts at Thomas Jefferson's plantation known as Monticello. C1 Virginia Dept Hist Resources, Richmond, VA 23221 USA. Thomas Jefferson Fdn, Charlottesville, VA 22902 USA. Evans E, Windsor Ctr 104, E Windsor, NJ 08520 USA. Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. RP Stevenson, CM (reprint author), Virginia Dept Hist Resources, 2801 Kensington Ave, Richmond, VA 23221 USA. NR 45 TC 8 Z9 8 U1 1 U2 9 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD FEB PY 2007 VL 49 BP 153 EP 177 DI 10.1111/j.1475-4754.2007.00293.x PN 1 PG 25 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA 138EA UT WOS:000244344700009 ER PT J AU Scalo, J Kaltenegger, L Segura, AG Fridlund, M Ribas, I Kulikov, YN Grenfell, JL Rauer, H Odert, P Leitzinger, M Selsis, F Khodachenko, ML Eiroa, C Kasting, J Lammer, H AF Scalo, John Kaltenegger, Lisa Segura, Ant Gona Fridlund, Malcolm Ribas, Ignasi Kulikov, Yu. N. Grenfell, John L. Rauer, Heike Odert, Petra Leitzinger, Martin Selsis, F. Khodachenko, Maxim L. Eiroa, Carlos Kasting, Jim Lammer, Helmut TI M stars as targets for terrestrial exoplanet searches and biosignature detection SO ASTROBIOLOGY LA English DT Review DE M star planets; habitable planets; life and stellar activity; spectral biosignatures; terrestrial planet formation; exoplanet properties ID EARTH-LIKE PLANETS; SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; X-RAY-EMISSION; CARBON-DIOXIDE CLOUDS; SUN-LIKE STARS; CYCLOBUTANE PYRIMIDINE DIMERS; EXTRASOLAR GIANT PLANETS; HOBBY-EBERLY TELESCOPE AB The changing view of planets orbiting low mass stars, M stars, as potentially hospitable worlds for life and its remote detection was motivated by several factors, including the demonstration of viable atmospheres and oceans on tidally locked planets, normal incidence of dust disks, including debris disks, detection of planets with masses in the 5-20 M-circle plus range, and predictions of unusually strong spectral biosignatures. We present a critical discussion of M star properties that are relevant for the long- and short-term thermal, dynamical, geological, and environmental stability of conventional liquid water habitable zone (HZ) M star planets, and the advantages and disadvantages of M stars as targets in searches for terrestrial HZ planets using various detection techniques. Biological viability seems supported by unmatched very long-term stability conferred by tidal locking, small HZ size, an apparent shortfall of gas giant planet perturbers, immunity to large astrosphere compressions, and several other factors, assuming incidence and evolutionary rate of life benefit from lack of variability. Tectonic regulation of climate and dynamo generation of a protective magnetic field, especially for a planet in synchronous rotation, are important unresolved questions that must await improved geodynamic models, though they both probably impose constraints on the planet mass. M star HZ terrestrial planets must survive a number of early trials in order to enjoy their many Gyr of stability. Their formation may be jeopardized by an insufficient initial disk supply of solids, resulting in the formation of objects too small and/or dry for habitability. The small empirical gas giant fraction for M stars reduces the risk of formation suppression or orbit disruption from either migrating or nonmigrating giant planets, but effects of perturbations from lower mass planets in these systems are uncertain. During the first similar to 1 Gyr, atmospheric retention is at peril because of intense and frequent stellar flares and sporadic energetic particle events, and impact erosion, both enhanced, the former dramatically, for M star HZ semimajor axes. Loss of atmosphere by interactions with energetic particles is likely unless the planetary magnetic moment is sufficiently large. For the smallest stellar masses a period of high planetary surface temperature, while the parent star approaches the main sequence, must be endured. The formation and retention of a thick atmosphere and a strong magnetic field as buffers for a sufficiently massive planet emerge as prerequisites for an M star planet to enter a long period of stability with its habitability intact. However, the star will then be subjected to short-term fluctuations with consequences including frequent unpredictable variation in atmospheric chemistry and surficial radiation field. After a review of evidence concerning disks and planets associated with M stars, we evaluate M stars as targets for future HZ planet search programs. Strong advantages of M stars for most approaches to HZ detection are offset by their faintness, leading to severe constraints due to accessible sample size, stellar crowding (transits), or angular size of the HZ (direct imaging). Gravitational lensing is unlikely to detect HZ M star planets because the HZ size decreases with mass faster than the Einstein ring size to which the method is sensitive. M star Earth-twin planets are predicted to exhibit surprisingly strong bands of nitrous oxide, methyl chloride, and methane, and work on signatures for other climate categories issummarized. The rest of the paper is devoted to an examination of evidence and implications of the unusual radiation and particle environments for atmospheric chemistry and surface radiation doses, and is summarized in the Synopsis. We conclude that attempts at remote sensing of biosignatures and nonbiological markers from M star planets are important, not as tests of any quantitative theories or rational arguments, but instead because they offer an inspection of the residues from a Gyr-long biochemistry experiment in the presence of extreme environmental fluctuations. A detection or repeated nondetections could provide a unique opportunity to partially answer a fundamental and recurrent question about the relation between stability and complexity, one that is not addressed by remote detection from a planet orbiting a solar-like star, and can only be studied on Earth using restricted microbial systems in serial evolution experiments or in artificial life simulations. This proposal requires a planet that has retained its atmosphere and a water supply. The discussion given here suggests that observations of M star exoplanets can decide this latter question with only slight modifications to plans already in place for direct imaging terrestrial exoplanet missions. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. Inst Estudis Especials Catalunya, Barcelona, Spain. Inst Ciencias Espaciais, Barcelona, Spain. Russian Acad Sci, Polar Geophys Inst, Murmansk, Russia. Inst Planet Forsch Extrasolare Planet & Atmosphar, Berlin, Germany. Graz Univ, Inst Phys, Graz, Austria. Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. Ctr Rech Astrophys Lyon, Lyon, France. Ecole Normale Super, Lyon, France. Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. Penn State Univ, Dept Geosci, State Coll, PA USA. RP Scalo, J (reprint author), Univ Texas, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM parrot@astro.as.utexas.edu RI Ribas, Ignasi/M-2134-2014; Kulikov, Yuri/B-7866-2017; Kulikov, Yuri/H-7799-2013 OI Ribas, Ignasi/0000-0002-6689-0312; Kulikov, Yuri/0000-0002-1741-3907; Kulikov, Yuri/0000-0001-5475-3284 NR 427 TC 155 Z9 157 U1 6 U2 80 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD FEB PY 2007 VL 7 IS 1 BP 85 EP 166 DI 10.1089/ast.2006.0000 PG 82 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 157MT UT WOS:000245724900006 PM 17407405 ER PT J AU Tafoya, D Gomez, Y Anglada, G Loinard, L Torrelles, JM Miranda, LF Osorio, M Franco-Hernandez, R Nyman, LA Nakashima, J Deguchi, S AF Tafoya, D. Gomez, Y. Anglada, G. Loinard, L. Torrelles, J. M. Miranda, L. F. Osorio, M. Franco-Hernandez, R. Nyman, L. -A. Nakashima, J. Deguchi, S. TI Detection of HCO+ emission toward the planetary nebula K3-35 SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : molecules; planetary nebulae : general; radio lines : ISM; stars : individual (K3-35) ID ASYMPTOTIC GIANT BRANCH; WATER-MASER EMISSION; RADIO MORPHOLOGY; CO; ENVELOPES; STARS AB We report the detection, for the first time, of HCO+(J = 1 -> 0) emission, as well as marginal CO(J = 1 -> 0) emission, toward the planetary nebula (PN) K3-35 as a result of a molecular survey carried out toward this source. We also report new observations of the previously detected CO( J 2 ! 1) and water maser emission, as well as upper limits for the emission of the SiO, (HCO+)-C-13, HNC, HCN, HC3OH, HC5N, CS, HC3N, (CO)-C-13, CN, and NH3 molecules. From the ratio of CO(J = 2 -> 1) to CO(J = 1 -> 0) emission we have estimated the kinetic temperature of the molecular gas, obtaining a value of similar or equal to 20 K. Using this result we have estimated a molecular mass for the envelope of similar or equal to 0.017M(circle dot) and an HCO+ abundance relative to H-2 of 6 x 10(-7), similar to the abundances found in other PNe. K3-35 is remarkable because it is one of the two PNe reported to exhibit water maser emission, which is present in the central region, as well as at a distance of similar or equal to 5000 AU from the center. The presence of molecular emission provides some clues that could help in understanding the persistence of water molecules in the envelope of K3-35. The HCO+ emission could be arising in dense molecular clumps, which may provide the shielding mechanism that protects water molecules in this source. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Astrofis Andalucia, Granada, Spain. Univ Barcelona, Fac Fis, Inst Ciencias Espacio, E-08028 Barcelona, Spain. Univ Barcelona, Inst Estudis Espacials Catalunya, E-08028 Barcelona, Spain. European So Observ, Swedish ESO Submillimetre Telescope, Santiago 19, Chile. Onsala Space Observ, Onsala, Sweden. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Grad Univ Adv Studies, Dept Astron Sci, Nobeyama Radio Observ, NAOJ,Minamisa Ku, Nagano, Japan. RP Tafoya, D (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia, Michoacan, Mexico. EM d.tafoya@astrosmo.unam.mx; y.gomez@astrosmo.unam.mx; guillem@iaa.es; l.loinard@astrosmo.unam.mx; torrelles@ieec.fcr.es; lfm@iaa.es; osorio@iaa.es; rfranco@cfa.harvard.edu; lnyman@eso.org; junichi@asiaa.sinica.edu.tw; deguchi@nro.nao.ac.jp RI Nakashima, Jun-ichi/D-3113-2009; OI Nakashima, Jun-ichi/0000-0003-3324-9462; Torrelles, Jose Maria/0000-0002-6896-6085 NR 27 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2007 VL 133 IS 2 BP 364 EP 369 DI 10.1086/509776 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129LC UT WOS:000243730000002 ER PT J AU Garg, A Stubbs, CW Challis, P Wood-Vasey, WM Blondin, S Huber, ME Cook, K Nikolaev, S Rest, A Smith, RC Olsen, K Suntzeff, NB Aguilera, C Prieto, JL Becker, A Miceli, A Miknaitis, G Clocchiatti, A Minniti, D Morelli, L Welch, DL AF Garg, Arti Stubbs, Christopher W. Challis, Peter Wood-Vasey, W. Michael Blondin, Stephane Huber, Mark E. Cook, Kem Nikolaev, Sergei Rest, Armin Smith, R. Chris Olsen, Knut Suntzeff, Nicholas B. Aguilera, Claudio Prieto, Jose Luis Becker, Andrew Miceli, Antonino Miknaitis, Gajus Clocchiatti, Alejandro Minniti, Dante Morelli, Lorenzo Welch, Douglas L. TI Light curves of type Ia supernovae from near the time of explosion SO ASTRONOMICAL JOURNAL LA English DT Article DE Magellanic Clouds; supernovae : general; surveys ID LARGE-MAGELLANIC-CLOUD; HIGH-REDSHIFT SUPERNOVAE; HUBBLE CONSTANT; IMAGE SUBTRACTION; K-CORRECTIONS; B-BAND; EXTINCTION; PROJECT; SPECTROGRAPH; TELESCOPE AB We present a set of 11 Type Ia supernova (SN Ia) light curves with dense, premaximum sampling. These supernovae (SNe), in galaxies behind the Large Magellanic Cloud (LMC), were discovered by the SuperMACHO survey. The SNe span a redshift range of z = 0.11 - 0.35. Our light curves contain some of the earliest premaximum observations of SNe Ia to date. We also give a functional model that describes the SN Ia light-curve shape (in our VR band). Our function uses the "expanding fireball" model of Goldhaber et al. to describe the rising light curve immediately after explosion but constrains it to smoothly join the remainder of the light curve. We fit this model to a composite observed VR-band light curve of three SNe between redshifts of 0.135 and 0.165. These SNe have not been K-corrected or adjusted to account for reddening. In this redshift range, the observed VR band most closely matches the rest-frame V band. Using the best fit to our functional description of the light curve, we find the time between explosion and observed VR-band maximum to be 17.6 +/- 1.3(stat) +/- 0.07(sys) rest-frame days for a SN Ia with a VR-band Delta m(-10) of 0.52 mag. For the redshifts sampled, the observed VR-band time of maximum brightness should be the same as the rest-frame V-band maximum to within 1.1 rest-frame days. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Livermore, CA USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. Ohio State Univ, Columbus, OH 43210 USA. Univ Washington, Seattle, WA 98195 USA. Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. Pontificia Univ Catolica Chile, Santiago, Chile. McMaster Univ, Hamilton, ON, Canada. RP Garg, A (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM artigarg@fas.harvard.edu RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 NR 38 TC 42 Z9 42 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2007 VL 133 IS 2 BP 403 EP 419 DI 10.1086/510118 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129LC UT WOS:000243730000006 ER PT J AU Ganguly, R Brotherton, MS Arav, N Heap, SR Wisotzki, L Aldcroft, TL Alloin, D Behar, E Canalizo, G Crenshaw, DM De Kool, M Chambers, K Cecil, G Chatzichristou, E Everett, J Gabel, J Gaskell, CM Galliano, E Green, RF Hall, PB Hines, DC Junkkarinen, VT Kaastra, JS Kaiser, ME Kazanas, D Konigl, A Korista, KT Kriss, GA Laor, A Leighly, KM Mathur, S Ogle, P Proga, D Sabra, B Sivron, R Snedden, S Telfer, R Vestergaard, M AF Ganguly, Rajib Brotherton, Michael S. Arav, Nahum Heap, Sara R. Wisotzki, Lutz Aldcroft, Thomas L. Alloin, Danielle Behar, Ehud Canalizo, Gabriela Crenshaw, D. Michael De Kool, Martijn Chambers, Kenneth Cecil, Gerald Chatzichristou, Eleni Everett, John Gabel, Jack Gaskell, C. Martin Galliano, Emmanuel Green, Richard F. Hall, Patrick B. Hines, Dean C. Junkkarinen, Vesa T. Kaastra, Jelle S. Kaiser, Mary Elizabeth Kazanas, Demosthenes Konigl, Arieh Korista, Kirk T. Kriss, Gerard A. Laor, Ari Leighly, Karen M. Mathur, Smita Ogle, Patrick Proga, Daniel Sabra, Bassem Sivron, Ran Snedden, Stephanie Telfer, Randal Vestergaard, Marianne TI Hubble Space Telescope ultraviolet spectroscopy of 14 low-redshift quasars SO ASTRONOMICAL JOURNAL LA English DT Article DE quasars : absorption lines; quasars : emission lines; surveys ID BROAD ABSORPTION-LINE; ACTIVE GALACTIC NUCLEI; C-IV LAMBDA-1549; RADIATION-DRIVEN WINDS; RADIO-QUIET QUASARS; DIGITAL SKY SURVEY; STELLAR OBJECTS; EMISSION-LINE; INTRINSIC ABSORPTION; IMAGING SPECTROGRAPH AB We present low-resolution ultraviolet spectra of 14 low-redshift (z(em) less than or similar to 0.8) quasars observed with the Hubble Space Telescope STIS as part of a Snapshot project to understand the relationship between quasar outflows and luminosity. By design, all observations cover the C (IV) emission line. Ten of the quasars are from the Hamburg-ESO catalog, three are from the Palomar-Green catalog, and one is from the Parkes catalog. The sample contains a few interesting quasars, including two broad absorption line (BAL) quasars (HE 0143 - 3535 and HE 0436 - 2614), one quasar with a mini-BAL (HE 1105 - 0746), and one quasar with associated narrow absorption (HE 0409 - 5004). These BAL quasars are among the brightest known (although not the most luminous) since they lie at z(em) < 0.8. We compare the properties of these BAL quasars to the z(em) < 0.5 Palomar-Green and z(em) > 1.4 Large Bright Quasar Survey samples. By design, our objects sample luminosities in between these two surveys, and our four absorbed objects are consistent with the v similar to L-0.62 relation derived by Laor & Brandt (2002). Another quasar, HE 0441 - 2826, contains extremely weak emission lines, and our spectrum is consistent with a simple power-law continuum. The quasar is radio-loud but has a steep spectral index and a lobe-dominated morphology, which argues against it being ablazar. The unusual spectrum of this quasar resembles the spectra of the quasars PG 1407 + 265, SDSS J1136 + 0242, and PKS 1004 + 13, for which several possible explanations have been entertained. C1 Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. NASA, Goddard Space Flight Ctr, Lab Astron & Solar Phys, Greenbelt, MD 20771 USA. Astrophys Inst Potsdam, Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, Santiago 19, Chile. Univ Paris 07, UMR 7158, CEA Saclay, DSM,DAPNIA,Serv Astrophys,CNRS, Paris, France. Technion, Dept Phys, Haifa, Israel. Univ Calif Riverside, Dept Phys, Riverside, CA 92521 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT, Australia. Inst Astron, Honolulu, HI USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC USA. Natl Observ Athens, Inst Astron & Astrophys, Athens, Greece. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON, Canada. Univ Wisconsin, Dept Astron, Dept Phys, Madison, WI USA. Univ Wisconsin, Ctr Magnet Self Org, Madison, WI USA. Univ Nebraska, Dept Phys & Astron, Lincoln, NE 68588 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Large Binocular Telescope Observ, Tucson, AZ USA. York Univ, Dept Phys & Astron, Toronto, ON M3J 2R7, Canada. Space Sci Inst, Boulder, CO USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92103 USA. SRON Netherlands Inst Space Res, Utrecht, Netherlands. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Univ Notre Dame, Fac Nat & Appl Sci, Zouk Mosbeh, Lebanon. Baker Univ, Dept Phys, Baldwin City, KS USA. Apache Point Observ, Sunspot, NM USA. Orbital Sci Corp, Greenbelt, MD USA. Univ Arizona, Steward Observ, Tucson, AZ USA. RP Ganguly, R (reprint author), Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. EM ganguly@uwyo.edu RI heap, sara/E-2237-2012; Vestergaard, Marianne/M-5247-2014; OI Vestergaard, Marianne/0000-0001-9191-9837; Gaskell, C/0000-0003-4888-2009; Chambers, Kenneth /0000-0001-6965-7789 NR 52 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 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2007 VL 133 IS 2 BP 479 EP 486 DI 10.1086/510129 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129LC UT WOS:000243730000011 ER PT J AU Bonanos, AZ Stanek, KZ Szentgyorgyi, AH Sasselov, DD Bakos, GA AF Bonanos, A. Z. Stanek, K. Z. Szentgyorgyi, A. H. Sasselov, D. D. Bakos, G. A. . TI The RR lyrae distance to the draco dwarf spheroidal galaxy (vol 127, pg 861, 2004) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bonanos, Alceste/K-5392-2013 OI Bonanos, Alceste/0000-0003-2851-1905 NR 1 TC 2 Z9 2 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2007 VL 133 IS 2 BP 756 EP 756 DI 10.1086/510311 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129LC UT WOS:000243730000037 ER PT J AU Garay, G Mardones, D Bronfman, L Brooks, KJ Rodriguez, LF Gusten, R Nyman, LA Franco-Hernandez, R Moran, JM AF Garay, G. Mardones, D. Bronfman, L. Brooks, K. J. Rodriguez, L. F. Guesten, R. Nyman, L. -A. Franco-Hernandez, R. Moran, J. M. TI Discovery of an energetic bipolar molecular outflow towards IRAS 16547-4247 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : jets and outflows; ISM : molecules; stars : formation ID MASSIVE STAR-FORMATION; CO LINE FORMATION; PROTOSTELLAR CANDIDATES; POINT SOURCES; DENSE CORES; REGIONS; FLOWS; CONTINUUM; CLOUDS; ENVIRONMENT AB Aims. We present molecular line observations of the molecular core associated with IRAS 16547-4247, which have allowed us to determine its physical and kinematical properties at angular resolutions of similar to 18". Methods. The observations were made using the Atacama Pathfinder Experiment Telescope in the J = 3 -> 2 transitions of (12)CO and (13)CO, J = 4 -> 3 transitions of HCO(+) and H(13)CO(+), and J = 7 -> 6 transition of CS. Results. Our observations reveal the presence of a collimated bipolar outflow with lobes similar to 0.7 pc in extent and aligned with the thermal jet located at the center of the core. The morphology and velocity structure of the flow are well described by a biconical outflow that is inclined from the line of sight by an angle of 84 degrees, has a semi-opening angle of 14 degrees, and in which the gas moves outwards with a constant total velocity, with respect to the cone apex, of similar to 120 km s(-1). The outflow is massive and energetic (flow mass similar to 110 M(circle dot); mass outflow rate similar to 2 x 10(-2) M(circle dot) yr(-1); momentum similar to 2 x 10(3) M(circle dot) km s(-1) and kinetic energy similar to 9 x 10(47) erg), and has a dynamical time scale of 6 x 10(3) yr. These parameters are consistent with the flow being driven by a young massive stellar object with L(bol) similar to 6 x 10(4) L(circle dot). C1 Univ Chile, Dept Astron, Santiago, Chile. Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Michoacan 58089, Mexico. Max Planck Inst Radioastron, D-53121 Bonn, Germany. European So Observ, Santiago 19, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Garay, G (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM guido@das.uchile.cl RI Garay, Guido/H-8840-2013; Bronfman, Leonardo/H-9544-2013; Mardones, Diego/I-5719-2016; OI Garay, Guido/0000-0003-1649-7958; Bronfman, Leonardo/0000-0002-9574-8454; Brooks, Kate/0000-0001-9373-8992; Moran, James/0000-0002-3882-4414 NR 35 TC 20 Z9 20 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2007 VL 463 IS 1 BP 217 EP 224 DI 10.1051/0004-6361:20065329 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 132KO UT WOS:000243941900019 ER PT J AU Giardino, G Favata, F Micela, G Sciortino, S Winston, E AF Giardino, G. Favata, F. Micela, G. Sciortino, S. Winston, E. TI The onset of X-ray emission in young stellar objects - A Chandra observation of the Serpens star-forming region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : clouds; ISM : individual objects : Serpens cloud; stars : pre-main sequence; X-rays : stars ID CLOUD CORE; PROTOSTELLAR JET; INFRARED IMAGES; MOLECULAR CLOUD; HIGH-RESOLUTION; DARK CLOUD; XMM-NEWTON; CLASS-I; DISCOVERY; OUTFLOW AB Aims. To study the properties of X-ray emission from young stellar objects (YSOs) through their evolution from Class I to Class III and determine whether Class 0 protostars emit X-rays. Methods. A deep Chandra X-ray observation of the Serpens star-forming region was obtained. The Serpens Cloud Core is ideally suited for this type of investigation, being populated by a dense and extremely young cluster whose members are found in all evolutionary stages, including six well-studied Class 0 sources. Results. None of the six Class 0 protostars is detected in our observations, excluding the presence of sources with typical X-ray luminosities greater than or similar to 0.4 x 10(30) erg s(-1) (for column densities of the order of 4 x 10(23) cm(-2), or A(V) similar to 200). A total of 85 X-ray sources are detected and the light curves and spectra of 35 YSOs are derived. There is a clear trend of decreasing absorbing column densities as one moves from Class I to Class III sources, and some evidence of decreasing plasma temperatures, too. We observe a strong, long-duration, flare from a Class II low-mass star, for which we derive a flaring loop length of the order of 20 stellar radii. We interpret the flaring event as originating from a magnetic flux tube connecting the star to its circumstellar disk. The presence of such a disk is supported by the detection, in the spectrum of this star, of 6.4 keV Fe fluorescent emission. C1 ESTEC, Astrophys Div, Res & Sci Support Dept ESA, NL-2200 AG Noordwijk, Netherlands. INAF, Osserv Astron Palermo, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Giardino, G (reprint author), ESTEC, Astrophys Div, Res & Sci Support Dept ESA, Postbus 299, NL-2200 AG Noordwijk, Netherlands. OI Micela, Giuseppina/0000-0002-9900-4751 NR 54 TC 34 Z9 34 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2007 VL 463 IS 1 BP 275 EP U53 DI 10.1051/0004-6361:20066424 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 132KO UT WOS:000243941900026 ER PT J AU Bao, X Zhang, H Lin, J Stenborg, GA AF Bao, X. Zhang, H. Lin, J. Stenborg, G. A. TI Coronal mass ejections and the associated activities on the solar disk observed on October 26, 2003 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : coronal mass ejections; Sun : filaments; Sun : flares; Sun : activity ID SMM OBSERVATIONS; FLARES; TRANSIENTS; ERUPTIONS; LASCO; SOHO AB Aims: Coronal mass ejections (CMEs) are usually considered fast (slow) if their velocities are greater (less) than 500 kms(-1). It is generally believed that fast CMEs are well associated with activity manifested on the solar disk, such as solar flares, and that slow CMEs are often associated with filament eruptions out of active regions and can hardly leave any signature on the solar disk. However, this may not be totally true for the cases we are studying in the present work, where we have explored more explicitly than in previous studies the relationship between different types of CMEs and the associated on-disk activities. Methods: We analyzed four CMEs that happen to take of near the west limb of the Sun on October 26, 2003. Their maximum speeds varied from 300 to 1800 km s(-1), with average accelerations from about 6 ms(-2) up to 330 ms(-2). They span over almost the full range of speeds of typical CMEs, from slow to fast. The evolution and kinematical properties of each CME at their early stages as well as the corresponding processes on the solar disk are examined. Results: Three out of the four events analyzed, including slow and fast ones, exhibited apparent acceleration during their early development and a likely association with solar disk activity as manifested by ribbon flares and post-event loops. The fourth event (the CME that did not show any clear association with solar disk activity) was not the slowest one: it had a median speed (<= 400 km s(-1)). This suggests that some existing conclusions about the CME-flare correlation need to be re-investigated. In addition, the correlation of the coronal mass ejection angular widths to their speeds is also discussed. C1 Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. Chinese Acad Sci, Natl Astron Observ China, Yunnan Astron Observ, Yunnan 650011, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Bao, X (reprint author), Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. EM xbao@bao.ac.cn RI LIN, JUN/B-9890-2017 NR 38 TC 5 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2007 VL 463 IS 1 BP 321 EP 331 DI 10.1051/0004-6361:20065471 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 132KO UT WOS:000243941900031 ER PT J AU Schodel, R Krips, M Markoff, S Neri, R Eckart, A AF Schoedel, R. Krips, M. Markoff, S. Neri, R. Eckart, A. TI The millimetre variability of M81*- Multi-epoch dual frequency mm-observations of the nucleus of M81 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; galaxies : active; galaxies : jets; radio continuum : galaxies ID SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; DOMINATED ACCRETION FLOWS; SGR-A; CIRCULAR-POLARIZATION; LINEAR-POLARIZATION; GALACTIC-CENTER; RADIO OUTBURSTS; EMISSION-LINES; JET MODEL AB Aims. There are still many open questions as to the physical mechanisms at work in Low Luminosity AGN that accrete in the extreme sub-Eddington regime. Simultaneous multi-wavelength studies have been very successful in constraining the properties of Sgr A*, the extremely sub-Eddington black hole at the centre of our Milky Way. M81*, the nucleus of the nearby spiral galaxy M81, is an ideal source to extend the insights obtained on Sgr A* toward higher luminosity AGN. Here we present observations at 3 and 1mm that were obtained within the framework of a coordinated, multi-wavelength campaign on M81*. Methods. The continuum emission from M81* was observed during three epochs with the IRAM Plateau de Bure Interferometer simultaneously at wavelengths of 3 and 1 mm. Results. We present the first flux measurements of M81* at wavelengths around 1 mm. We find that M81* is a continuously variable source with the higher variability observed at the shorter wavelength. Also, the variability at 3 and 1mm appears to be correlated. Like Sgr A*, M81* appears to display the strongest flux density and variability in the mm-to-submm regime. There remains still some ambiguity concerning the exact location of the turnover frequency from optically thick to optically thin emission. The observed variability time scales point to an upper size limit of the emitting region of the order 25 Schwarzschild radii. Conclusions. The data show that M81* is indeed a system with very similar physical properties to Sgr A* and an ideal bridge toward high luminosity AGN. The data obtained clearly demonstrate the usefulness and, above all, the necessity of simultaneous multi-wavelength observations of LLAGN. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Harvard Smithsonian Ctr Astrophys, SMA Project, Hilo, HI 96720 USA. Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. RP Schodel, R (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM rainer@ph1.uni-koeln.de; mkrips@cfa.harvard.edu; sera@science.uva.nl; neri@iram.fr; eckart@ph1.uni-koeln.de RI Schoedel, Rainer/D-4751-2014 OI Schoedel, Rainer/0000-0001-5404-797X NR 44 TC 15 Z9 15 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2007 VL 463 IS 2 BP 551 EP 557 DI 10.1051/0004-6361:20066383 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134FU UT WOS:000244069700017 ER PT J AU Branduardi-Raymont, G Bhardwaj, A Elsner, RF Gladstone, GR Ramsay, G Rodriguez, P Soria, R Waite, JH Cravens, TE AF Branduardi-Raymont, G. Bhardwaj, A. Elsner, R. F. Gladstone, G. R. Ramsay, G. Rodriguez, P. Soria, R. Waite, J. H., Jr. Cravens, T. E. TI A study of Jupiter's aurorae with XMM-Newton SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites : general; planets and satellites : individual : Jupiter; X-rays : general ID BREMSSTRAHLUNG X-RAYS; SOLAR-WIND IONS; EMISSION; PRECIPITATION; SPECTRA AB We present a detailed analysis of Jupiter's X-ray (0.2-10 keV) auroral emissions as observed over two XMM-Newton revolutions in Nov. 2003 and compare it with that of an earlier observation in Apr. 2003. We discover the existence of an electron bremsstrahlung component in the aurorae, which accounts for essentially all the X-ray flux above 2 keV: its presence had been predicted but never detected for lack of sensitivity of previous X-ray missions. This bremsstrahlung component varied significantly in strength and spectral shape over the 3.5 days covered by the Nov. 2003 observation, displaying substantial hardening of the spectrum with increasing flux. This variability may be linked to the strong solar activity taking place at the time, and may be induced by changes in the acceleration mechanisms inside Jupiter's magnetosphere. As in Apr. 2003, the auroral spectra below 2 keV are best fitted by a superposition of line emission most likely originating from ion charge exchange, with OVII playing the dominant role. We still cannot resolve conclusively the ion species responsible for the lowest energy lines (around 0.3 keV), so the question of the origin of the ions (magnetospheric or solar wind) is still open. It is conceivable that both scenarios play a role in what is certainly a very complex planetary structure. High resolution spectra of the whole planet obtained with the XMM-Newton Reflection Grating Spectrometer in the range 0.5-1 keV clearly separate emission lines (mostly of iron) originating at low latitudes on Jupiter from the auroral lines due to oxygen. These are shown to possess very broad wings which imply velocities of similar to 5000 km s(-1). Such speeds are consistent with the energies at which precipitating and charge exchanging oxygen ions are expected to be accelerated in Jupiter's magnetosphere. Overall we find good agreement between our measurements and the predictions of recently developed models of Jupiter's auroral processes. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. NSSTC XD12, NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA. SW Res Inst, San Antonio, TX 78228 USA. XMM Newton SOC, Madrid 28080, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. RP Branduardi-Raymont, G (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM gbr@mssl.ucl.ac.uk OI Bhardwaj, Anil/0000-0003-1693-453X NR 34 TC 41 Z9 41 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2007 VL 463 IS 2 BP 761 EP 774 DI 10.1051/0004-6361:20066406 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134FU UT WOS:000244069700042 ER PT J AU Neuhauser, R Mugrauer, M Fukagawa, M Torres, G Schmidt, T AF Neuhaeuser, R. Mugrauer, M. Fukagawa, M. Torres, G. Schmidt, T. TI Direct detection of exoplanet host star companion gamma Cep B and revised masses for both stars and the sub-stellar object SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation : adapive optics; binaries : spectroscopic; binaries : visual; planetary systems; star : individual : gamma Cep ID SEARCH AB Context. The star gamma Cep is known as a single-lined spectroscopic triple system at a distance of 13.8 pc, composed of a K1 III-IV primary star with V = 3.2 mag, a stellar-mass companion in a 66-67 year orbit (Torres 2007, ApJ, 654, 1095), and a substellar companion with M-p sin i = 1.7 M-Jup that is most likely a planet (Hatzes et al. 2003, ApJ, 599, 1383). Aims. We aim to obtain a first direct detection of the stellar companion, to determine its current orbital position ( for comparison with the spectroscopic and astrometric data), its infrared magnitude and, hence, mass. Methods. We use the Adaptive Optics camera CIAO at the Japanese 8 m telescope Subaru on Mauna Kea, Hawaii, with the semitransparent coronograph to block most of the light from the bright primary. Cep A, and to detect at the same time the faint companion B. In addition, we also used the IR camera Omega Cass at the Calar Alto 3.5 m telescope, Spain, to image. Cep A and B by adding up many very short integrations (without AO). Results. gamma Cep B is clearly detected on our CIAO and Omega Cass images. We use a photometric standard star to determine the magnitude of B after PSF subtraction in the Subaru image, and the magnitude difference between A and B in the Calar Alto images, and find an average value of K = 7.3 +/- 0.2 mag. The separations and position angles between A and B are measured on 15 July 2006 and 11 and 12 Sept. 2006, B is slightly south of west of A. Conclusions. By combining the radial velocity, astrometric, and imaging data, we have refined the binary orbit and determined the dynamical masses of the two stars in the gamma Cep system, namely 1.40 +/- 0.12 M-circle dot for the primary and 0.409 +/- 0.018 M-circle dot for the secondary ( consistent with being a M4 dwarf). We also determine the minimum mass of the sub-stellar companion to be M-p sin i = 1.60 +/- 0.13 M-Jup. C1 Univ Jena, Inst Astrophys, D-07745 Jena, Germany. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Nagoya Univ, Div Particle & Astrophys Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Neuhauser, R (reprint author), Univ Jena, Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany. EM rne@astro.uni-jena.de NR 10 TC 53 Z9 53 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2007 VL 462 IS 2 BP 777 EP 780 DI 10.1051/0004-6361:20066581 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 128VH UT WOS:000243686600039 ER PT J AU Shporer, A Hartman, J Mazeh, T Pietsch, W AF Shporer, A. Hartman, J. Mazeh, T. Pietsch, W. TI Photometric analysis of the optical counterpart of the black hole HMXB M 33 X-7 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : binaries : eclipsing; X-rays : individuals : M 33 X-7 ID STELLAR ATMOSPHERE MODELS; LIMB-DARKENING LAW; X-RAY SOURCES; THEORETICAL ISOCHRONES; ECLIPSING BINARIES; SURFACE GRAVITIES; GALAXY M33; SYSTEMS; LIGHT; CURVES AB Aims. Study the high-mass X-ray binary X-7 in M33 using broad-band optical data. Methods. We used recently published CFHT r' and i' data for variable stars in M33 to extract the light curve of the optical counterpart of X-7. We combined these data with DIRECT B and V measurements in order to search for an independent optical modulation with the X-ray periodicity. The periodic modulation is modelled with the ellipsoidal effect. We used UBVRr' i' magnitudes of the system to constrain the temperature and radius of the optical component. Results. The optical data revealed a periodicity of 3.4530 +/- 0.0014 days, which is consistent with the known X-ray period. Double modulation, which we attributed to ellipsoidal modulation, is clearly seen in four different optical bands. The absolute magnitude in six optical bands is most consistent with a stellar counterpart with 33 000 < Te. < 47 000 K and 15 < R < 20 R (circle dot). We modelled the optical periodic modulation and derived the masses of the two components as a function of the orbital inclination and the radius of the stellar component. The resulting mass range for the compact object is 1.3 < M < 23 M-circle dot. Conclusions. The system is probably a black hole HMXB, similar to Cyg X-1, LMC X-1 and LMC X-3. C1 Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Shporer, A (reprint author), Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. EM shporer@wise.tau.ac.il OI Hartman, Joel/0000-0001-8732-6166 NR 28 TC 8 Z9 8 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2007 VL 462 IS 3 BP 1091 EP 1095 DI 10.1051/0004-6361:20066354 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129IJ UT WOS:000243721900040 ER PT J AU Lai, KS Huang, JS Fazio, G Cowie, LL Hu, EM Kakazu, Y AF Lai, Kamson Huang, Jia-Sheng Fazio, Giovanni Cowie, Lennox L. Hu, Esther M. Kakazu, Yuko TI The stellar population of Ly alpha-emitting galaxies at z similar to 5.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : high-redshift ID HIGH-REDSHIFT GALAXIES; LYMAN BREAK GALAXIES; DEEP-FIELD-NORTH; STAR-FORMATION RATE; LUMINOSITY FUNCTION; SPACE-TELESCOPE; RADIATIVE-TRANSFER; EMITTERS; SPITZER; HUBBLE AB We present a study of three Ly alpha-emitting galaxies (LAEs), selected via a narrowband survey in the GOODS northern field and spectroscopically confirmed to have redshifts of z similar to 5.65. Using HSTACS and Spitzer IRAC data, we constrain the rest-frame UV-to-optical spectral energy distributions (SEDs) of the galaxies. Fitting stellar population synthesis models to the observed SEDs, we find best-fit stellar populations with masses between similar to 10(9) and 10(10) M(circle dot), and ages between similar to 5 and 100 Myr, assuming a simple starburst star formation history. However, stellar populations as old as 700 Myr are admissible if a constant star formation rate model is considered. Very deep near-IR observations may help to narrow the range of allowed models by providing extra constraints on the rest-frame UV spectral slope. Our narrowband-selected objects and other IRAC-detected z similar to 6 i'-dropout galaxies have similar 3.6 mu m magnitudes and z' -[3.6] colors, suggesting that they possess stellar populations of similar masses and ages. This similarity may be the result of a selection bias, since the IRAC-detected LAEs and i'-dropouts probably only sample the bright end of the luminosity function. On the other hand, our LAEs have blue i' - z' colors compared to the i'-dropouts and would have been missed by the i'-dropout selection criterion. A better understanding of the overlap between the LAE and the i'-dropout populations is necessary in order to constrain the properties of the overall high-redshift galaxy population, such as the total stellar mass density at z similar to 6. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Lai, KS (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM klai@cfa.harvard.edu NR 50 TC 76 Z9 76 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2007 VL 655 IS 2 BP 704 EP 713 DI 10.1086/510285 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000003 ER PT J AU Gibson, RR Canizares, CR Marshall, HL Young, AJ Lee, JC AF Gibson, Robert R. Canizares, Claude R. Marshall, Herman L. Young, Andrew J. Lee, Julia C. TI Line variability in the high-resolution X-ray spectrum of MCG-6-30-15 SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : individual (MCG-6-30-15); quasars : emission lines; X-rays : individual (MCG-6-30-15) ID ACTIVE GALACTIC NUCLEI; SEYFERT-1 GALAXY MCG-6-30-15; DUSTY WARM ABSORBER; BLACK-HOLE MASS; IONIZED-GAS; INTRINSIC ABSORPTION; CHANDRA HETGS; XMM-NEWTON; IRON LINE; IONS AB The recent 540 ks Chandra HETGS spectrum of the well-studied, variable active galactic nucleus (AGN) MCG -6-30-15 shows strong 1s-2p absorption lines from many ions. The spectrum was obtained over a period of about 10 days, and the large number of counts in the spectrum makes it ideal for testing variability on short timescales. We apply quantitative tests for line variability to the 1s-2p absorption lines of H- and He-like Ne, Mg, Si, and S. We find significant correlations and anticorrelations between lines as a function of time, much as we would expect if ionization levels in the absorber were varying. We also find evidence for variation in at least one 1s-2p resonance absorption line as a function of luminosity. We consider several possibilities to explain the line variation. First we consider factors that could change ionization levels in the absorber: radial motion, density variation, luminosity variation, and continuum shape variation. None of these individually can explain the line variation, although we cannot completely constrain continuum shape variation without simultaneous knowledge of the ultraviolet (UV) continuum. Other factors, considered individually, are also unable to explain all the variation: multiple changing continuum components, variable obscuration, and changes in velocity dispersion. Changes in line emission are an unlikely cause of significant variation in absorption-line measurements, but we are unable to fully constrain them. Variability could be due to a changing line of sight through a structured absorber. Modeling such scenarios should produce useful constraints on continuum emission mechanisms and absorber structure. 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, Cambridge, MA 02139 USA. EM rgibson@astro.psu.edu; crc@space.mit.edu; hermanm@space.mit.edu; ayoung@space.mit.edu; jclee@cfa.harvard.edu RI Lee, Julia/G-2381-2015 OI Lee, Julia/0000-0002-7336-3588 NR 47 TC 5 Z9 5 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 FEB 1 PY 2007 VL 655 IS 2 BP 749 EP 761 DI 10.1086/510441 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000007 ER PT J AU Crook, AC Huchra, JP Martimbeau, N Masters, KL Jarrett, T Macri, LM AF Crook, Aidan C. Huchra, John P. Martimbeau, Nathalie Masters, Karen L. Jarrett, Tom Macri, Lucas M. TI Groups of galaxies in the two micron all sky redshift survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : distances and redshifts; large scale structure of universe ID LARGE-SCALE STRUCTURE; LUMINOSITY FUNCTION; IRAS GALAXIES; LOCAL GROUP; CFA SURVEY; CATALOG; MASS; 2MASS; VELOCITY; CLUSTERS AB We present the results of applying a percolation algorithm to the initial release of the Two Micron All Sky Survey Extended Source Catalog, using subsequently measured redshifts for almost all of the galaxies with K < 11.25 mag. This group catalog is based on the first near-IR all-sky flux-limited survey that is complete to vertical bar b vertical bar = 5 degrees. We explore the dependence of the clustering on the length and velocity scales involved. The paper describes a group catalog, complete to a limiting redshift of 10(4) km s(-1), created by maximizing the number of groups containing three or more members. A second catalog is also presented, created by requiring a minimum density contrast of delta rho/rho >= 80 to identify groups. We identify known nearby clusters in the catalogs and contrast the groups identified in the two catalogs. We examine and compare the properties of the determined groups and verify that the results are consistent with the UZC-SSRS2 and northern CfA redshift survey group catalogs. The all-sky nature of the catalog will allow the development of a flow-field model based on the density field inferred from the estimated cluster masses. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Crook, AC (reprint author), MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM acc@space.mit.edu OI Masters, Karen/0000-0003-0846-9578; Macri, Lucas/0000-0002-1775-4859 NR 57 TC 90 Z9 90 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2007 VL 655 IS 2 BP 790 EP 813 DI 10.1086/510201 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000011 ER PT J AU Rakowski, CE Raymond, JC Szentgyorgyi, AH AF Rakowski, Cara E. Raymond, John C. Szentgyorgyi, Andrew H. TI [Ne v] imaging of N49 in the Large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : structure; shock waves; supernova remnants; supernovae : individual (N49); ultraviolet : ISM ID SUPERNOVA REMNANT N49; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; CYGNUS LOOP; FAR-ULTRAVIOLET; RADIATIVE SHOCKS; X-RAY; TELESCOPE OBSERVATIONS; NONRADIATIVE SHOCK; EMISSION; FILAMENT AB We present subarcsecond imaging in [Ne V] of N49, the brightest optical SNR in the LMC. Between the "cool'' optical and "hot'' X-ray regimes, [Ne V] emission indicates intermediate temperatures for collisionally excited plasmas (2-6 x 10(5) K), for which imaging has been extremely limited. We compare the flux in these images to the O VI measured spectroscopically by FUSE in individual apertures and find dereddened line ratios that are reasonably consistent with our predictions for intermediate velocity shocks. The overall luminosity in [Ne V] for the entire remnant is 1.2 x 10(36) ergs s(-1), which, given the measured line ratios, implies an overall O VI luminosity of 1.5 x 10(38) ergs s(-1). These large radiative losses indicate that this material must have been shocked recently relative to the total lifetime of the remnant. We also explore the complex spatial structure. We find [Ne V] tracing the [O III] emission more closely than it does H alpha, measure significant shifts (similar to 0.1 pc) between the peaks of different emission lines, and find 2 orders of magnitude variations in the flux ratios for different filaments across the remnant. These properties, as well as the general filamentary character of the optical emission, suggest thermally unstable intermediate-velocity shocks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rakowski, CE (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM crakowski@cfa.harvard.edu NR 37 TC 6 Z9 6 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 FEB 1 PY 2007 VL 655 IS 2 BP 885 EP 891 DI 10.1086/509322 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000018 ER PT J AU Walsh, AJ Myers, PC Di Francesco, J Mohanty, S Bourke, TL Gutermuth, R Wilner, D AF Walsh, Andrew J. Myers, Philip C. Di Francesco, James Mohanty, Subhanjoy Bourke, Tyler L. Gutermuth, Robert Wilner, David TI A large-scale survey of NGC 1333 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : kinematics and dynamics; stars : formation ID INITIAL MASS FUNCTION; OPHIUCHI MOLECULAR CLOUD; HERBIG-HARO OBJECTS; STAR-FORMATION; STELLAR CLUSTERS; DARK CLOUDS; DENSE CORES; ACCRETION; MOTIONS; GAS AB We observed the clustered star forming complex NGC 1333 with the BIMA and FCRAO telescopes in the transitions HCO+(1-0) and N2H+(1-0) over an 11' x 11' area with resolution similar to 10" (0.015 pc). The N2H+ emission follows very closely the submillimeter dust continuum emission, while HCO+ emission appears more spatially extended and also traces outflows. We have identified 93 N2H+ cores using the CLUMPFIND algorithm, and we derive N2H+ core masses between 0.05 and 2.5M(circle dot), with uncertainties of a factor of a few, dominated by the adopted N2H+ abundance. From a comparison with virial masses, we argue that most of these N2H+ cores are likely to be bound, even at the lowest masses, suggesting that the cores do not trace transient structures, and implies the entire mass distribution consists of objects that can potentially form stars. We find that the mass distribution of N2H+ cores resembles the field star IMF, which suggests that the IMF is locked in at the prestellar stage of evolution. We find that the N2H+ cores associated with stars identified from Spitzer infrared images have a flat mass distribution. This might be because lower mass cores lose a larger fraction of their mass when forming a star. Even in this clustered environment, we find no evidence for ballistic motions of the cores relative to their lower density surroundings traced by isotopic CO emission, although this conclusion must remain tentative until the surroundings are observed at the same high resolution as the N2H+. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada. RP Walsh, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM awalsh@cfa.harvard.edu RI Walsh, Andrew/B-5627-2013 OI Walsh, Andrew/0000-0001-9506-0855 NR 38 TC 57 Z9 58 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2007 VL 655 IS 2 BP 958 EP 972 DI 10.1086/510193 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000024 ER PT J AU Allen, PR Luhman, KL Myers, PC Megeath, ST Allen, LE Hartmann, L Fazio, GG AF Allen, P. R. Luhman, K. L. Myers, P. C. Megeath, S. T. Allen, L. E. Hartmann, L. Fazio, G. G. TI New low-mass stars and brown dwarfs with disks in Lupus SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; planetary systems : protoplanetary disks; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; T-TAURI STARS; EVOLUTIONARY MODELS; ACCRETION DISK; FORMING REGION; DARK CLOUD; YOUNG; EXTINCTION; MEMBERS AB Using the Infrared Array Camera and the Multiband Imaging Photometer aboard the Spitzer Space Telescope, we have obtained images of the Lupus 3 star-forming cloud at 3.6, 4.5, 5.8, 8.0, and 24 mu m. We present photometry in these bands for the 41 previously known members that are in our images. In addition, we have identified 19 possible new members of the cloud based on red 3.6-8.0 mu m colors that are indicative of circumstellar disks. We have performed optical spectroscopy on six of these candidates, all of which are confirmed as young low- mass members of Lupus 3. The spectral types of these new members range from M4.75 to M8, corresponding to masses of 0.2-0.03 M-circle dot for ages of similar to 1 Myr according to theoretical evolutionary models. We also present optical spectroscopy of a candidate disk-bearing object in the vicinity of the Lupus 1 cloud, 2M 1541-3345, which Jayawardhana & Ivanov recently classified as a young brown dwarf (M similar to 0:03 M-circle dot) with a spectral type of M8. In contrast to their results, we measure an earlier spectral type of M5:75 +/- 0: 25 for this object, indicating that it is probably a low-mass star (M similar to 0:1 M-circle dot). In fact, according to its gravity-sensitive absorption lines and its luminosity, 2M 1541-3345 is older than members of the Lupus clouds (tau similar to 1 Myr) and instead is probably a more evolved pre-main-sequence star that is not directly related to the current generation of star formation in Lupus. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Allen, PR (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM pallen@astro.psu.edu NR 33 TC 26 Z9 26 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 FEB 1 PY 2007 VL 655 IS 2 BP 1095 EP 1102 DI 10.1086/510363 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000035 ER PT J AU Holman, MJ Winn, JN Fuentes, CI Hartman, JD Stanek, KZ Torres, G Sasselov, DD Gaudi, BS Jones, RL Fraser, W AF Holman, Matthew J. Winn, Joshua N. Fuentes, Cesar I. Hartman, Joel D. Stanek, K. Z. Torres, Guillermo Sasselov, Dimitar D. Gaudi, B. Scott Jones, R. Lynne Fraser, Wesley TI The transit light curve project. IV. Five transits of the exoplanet OGLE-TR-10B SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems stars : individual (OGLE-TR10) techniques : photometric ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EXTRASOLAR GIANT PLANETS; GALACTIC DISK; HOT-JUPITERS; IMAGE SUBTRACTION; 2001 CAMPAIGN; HD 209458B; FOLLOW-UP; STAR AB We present I and B photometry of five distinct transits of the exoplanet OGLE-TR-10b. By modeling the light curves, we find the planetary radius to be RP (1:06 +/- 0:08) R-Jup and the stellar radius to be R-S 1:10 +/- 0:07 R (circle dot). The uncertainties are dominated by statistical errors in the photometry. Our estimate of the planetary radius is smaller than previous estimates that were based on lower precision photometry, and hence the planet is not as anomalously large as was previously thought. We provide updated determinations of all the system parameters, including the transit ephemerides. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada. RP Holman, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mholman@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012; Fuentes, Cesar /G-7506-2016; OI Hartman, Joel/0000-0001-8732-6166 NR 54 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2007 VL 655 IS 2 BP 1103 EP 1109 DI 10.1086/510342 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000036 ER PT J AU Penev, K Sasselov, D Robinson, F Demarque, P AF Penev, Kaloyan Sasselov, Dimitar Robinson, Frank Demarque, Pierre TI On dissipation inside turbulent convection zones from three-dimensional simulations of solar convection SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; Sun : interior; turbulence ID CLOSE BINARY STARS; TIDAL DISSIPATION; P-MODES; CIRCULARIZATION; VISCOSITY; EXCITATION; EVOLUTION; JUPITER; ORIGIN AB The development of two-dimensional and three-dimensional simulations of solar convection has lead to a picture of convection quite unlike the usually assumed Kolmogorov spectrum turbulent flow. We investigate the impact of this changed structure on the dissipation properties of the convection zone, parameterized by an effective viscosity coefficient. We use an expansion treatment developed by Goodman & Oh, applied to a numerical model of solar convection, to calculate effective viscosity as a function of frequency and compare this to currently existing prescriptions based on the assumption of Kolmogorov turbulence. The results quite closely match a linear scaling with period, even though this same formalism applied to a Kolmogorov spectrum of eddies gives a scaling with a power-law index of 5/3. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Yale Univ, Dept Astron, New Haven, CT 06511 USA. RP Penev, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Penev, Kaloyan/0000-0003-4464-1371 NR 21 TC 34 Z9 34 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2007 VL 655 IS 2 BP 1166 EP 1171 DI 10.1086/507937 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JS UT WOS:000243726000042 ER PT J AU Prochaska, JX Chen, HW Bloom, JS Dessauges-Zavadsky, M O'Meara, JM Bernstein, R Burles, S Dupree, AK Falco, E Thompson, IB AF Prochaska, J. X. Chen, H. -W. Bloom, J. S. Dessauges-Zavadsky, M. O'Meara, J. M. Bernstein, R. Burles, S. Dupree, A. K. Falco, E. Thompson, I. B. TI The interstellar medium of gamma ray burst host galaxies. I. Echelle spectra of swift GRB Afterglows SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : ISM; gamma rays : bursts ID RESONANCE-ABSORPTION LINES; ALPHA ABUNDANCE DATABASE; WAVELENGTHS LONGWARD; LYMAN LIMIT; ATOMIC DATA; FE II; SPECTROSCOPY; TELESCOPE; SYSTEMS; REDSHIFT AB We present optical echelle spectra of four gamma-ray burst (GRB) afterglows ( GRB 050730, GRB 050820, GRB 051111, and GRB 060418) discovered during the first 1.5 yr of operation of the Swift satellite and localized by either the Swift telescope or follow-up ground-based imaging. We analyze the spectra to derive accurate column density measurements for the transitions arising in the interstellar medium( ISM) of the GRB host galaxies. These measurements can be used to constrain the physical properties of the ISM, including the metallicity, dust-to-gas ratio, ionization state, and chemical abundances of the gas. We also present measurements of the strong Mg II systems in the GRB afterglow spectra. With the publication of this paper, we provide the first data release of echelle afterglow spectra by the GRAASP collaboration to the general community. C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Univ Chicago, Dept Astron, Chicago, IL 60637 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. Penn State Worthington Scranton, Dept Phys, Dunmore, PA USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Prochaska, JX (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. EM xavier@ucolick.org; hchen@oddjob.uchicago.edu NR 34 TC 60 Z9 60 U1 0 U2 1 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 FEB PY 2007 VL 168 IS 2 BP 231 EP 267 DI 10.1086/510239 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133SI UT WOS:000244033100003 ER PT J AU van Donkelaar, A Martin, RV Park, RJ Heald, CL Fu, TM Liao, H Guenther, A AF van Donkelaar, Aaron Martin, Randall V. Park, Rokjin J. Heald, Colette L. Fu, Tzung-May Liao, Hong Guenther, Alex TI Model evidence for a significant source of secondary organic aerosol from isoprene SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE isoprene; secondary organic aerosol; organic carbon ID UNITED-STATES; PARTICLE CONCENTRATION; CARBONACEOUS AEROSOLS; BIOGENIC HYDROCARBONS; PHOTOOXIDATION; EMISSIONS; OXIDATION; CHEMISTRY; FORESTS; TRENDS AB We investigate how a recently suggested pathway for production of secondary organic aerosol (SOA) affects the consistency of simulated organic aerosol (OA) mass in a global three-dimensional model of oxidant-aerosol chemistry (GEOS-Chem) versus surface measurements from the interagency monitoring of protected visual environments (IMPROVE) network. Simulations in which isoprene oxidation products contribute to SOA formation, with a yield of 2.0% by mass reduce a model bias versus measured OA surface mass concentrations. The resultant increase in simulated OA mass concentrations during summer of 0.6-1.0 mu g m(-3) in the southeastern United States reduces the regional RMSE to 0.88 mu g m(-3) from 1.26 mu g m(-3). Spring and fall biases are also reduced, with little change in winter when isoprene emissions are negligible. (c) 2006 Elsevier Ltd. All rights reserved. C1 Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Chinese Acad Sci, Inst Atmospher Phys, Beijing 100864, Peoples R China. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM kelaar@dal.ca RI Martin, Randall/A-2051-2008; Heald, Colette/A-6813-2011; Wang, ZF/D-7202-2012; Martin, Randall/C-1205-2014; Guenther, Alex/B-1617-2008; Chem, GEOS/C-5595-2014; Park, Rokjin/I-5055-2012; Fu, Tzung-May/N-3418-2015 OI Wang, ZF/0000-0002-7062-6012; Martin, Randall/0000-0003-2632-8402; Guenther, Alex/0000-0001-6283-8288; Park, Rokjin/0000-0001-8922-0234; NR 47 TC 29 Z9 29 U1 2 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD FEB PY 2007 VL 41 IS 6 BP 1267 EP 1274 DI 10.1016/j.atmosenv.2006.09.051 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 136OG UT WOS:000244233400014 ER PT J AU Lapolla, JS Suman, T Sosa-Calvo, J Schultz, TR AF Lapolla, John S. Suman, Ted Sosa-Calvo, Jeffrey Schultz, Ted R. TI Leaf litter ant diversity in Guyana SO BIODIVERSITY AND CONSERVATION LA English DT Article DE ALL protocol; biodiversity; conservation; formicidae; Guiana Shield; leaf litter ants ID SPECIES RICHNESS; BIODIVERSITY; FORESTS AB Leaf litter ants are an important group of organisms for informing conservation planning. This study presents the beginning of a leaf litter ant dataset for Guyana. Following the ants of the leaf litter protocol, ants were extracted from sifted leaf litter sampled along eight transects from across Guyana. A total of 230 species were collected from 44 genera. Of those 230 species, 122 species (ca. 53%) were found at only one site. Out of the 122 species found at only one site, 43 species (ca. 19%) were singletons, being known from only one specimen. Using a cluster analysis, faunistic composition was compared among sites. While the lowland sites accounted for the highest species richness, Mt. Ayanganna possessed an especially distinctive ant fauna and may represent a center of endemism. Three leaf litter ant communities were identified: lowland and two Mt. Ayanganna communities, mid-elevation and upper elevation. Recent mining operations on Mt. Ayanganna threaten its pristine nature and this study confirms the need for further biological study of the area. With upwards of 70% of its area still forested Guyana has the opportunity to preserve its biological heritage before widespread deforestation occurs. If expanded, this leaf litter ant dataset will be increasingly useful for country-wide conservation planning. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Lapolla, JS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,NHB,CE518,MRC 188 Washington, Washington, DC 20013 USA. EM lapollaj@si.edu NR 33 TC 9 Z9 10 U1 2 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD FEB PY 2007 VL 16 IS 2 BP 491 EP 510 DI 10.1007/s10531-005-6229-4 PG 20 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 133PP UT WOS:000244025100014 ER PT J AU Hunt, G Park, LE LaBarbera, M AF Hunt, Gene Park, Lisa E. LaBarbera, Michael TI A novel crustacean swimming stroke: Coordinated four-paddled locomotion in the cypridoidean ostracode Cypridopsis vidua (Muller) SO BIOLOGICAL BULLETIN LA English DT Article ID ESCAPE BEHAVIOR; CALANOID COPEPOD; ISOPODA; LARVAE; SPEED; DRAG AB Despite the diversity and ecological importance of cypridoidean ostracodes, there have been no kinematic studies of how they swim. We used regular and high-speed video of tethered ostracodes to document locomotion in the cypridoidean species Cypridopsis vidua. Swimming in this species is drag-based, with thrust provided by both antennulae and antennae. About 15 complete power and recovery strokes occur per second; maximal speeds for the limb tips were about 30 mm/s for the antennulae and 50 mm/s for the antennae. These speeds correspond to Reynolds numbers on the order of 10(-1) to 10(0) for the limb tips and 10(-2) to 10(-1) for the setae that extend outward from the swimming limbs and provide much of the surface area of the limb. The strokes of the four thrust-producing limbs are coordinated in a manner that seems to be unique among aquatic arthropods. When viewed from the anterior, power strokes are synchronized diagonally: left antennula and right antenna power strokes start at the same time and terminate just as the power strokes for the right antennula and left antenna begin. Because power strokes occur throughout the stroke cycle, swimming in this species is smoothly continuous, without the rapid accelerations and decelerations characteristic of most small aquatic arthropods. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Univ Akron, Dept Geol, Akron, OH 44325 USA. Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. RP Hunt, G (reprint author), Smithsonian Inst, Dept Paleobiol, Museum Natl Hist Nat, Washington, DC 20013 USA. EM hunte@si.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 NR 31 TC 2 Z9 2 U1 2 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 FEB PY 2007 VL 212 IS 1 BP 67 EP 73 PG 7 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 140LP UT WOS:000244507000008 PM 17301332 ER PT J AU Bellemain, E Nawaz, MA Valentini, A Swenson, JE Taberlet, P AF Bellemain, Eva Nawaz, Muhammad Ali Valentini, Alice Swenson, Jon E. Taberlet, Pierre TI Genetic tracking of the brown bear in northern Pakistan and implications for conservation SO BIOLOGICAL CONSERVATION LA English DT Article DE bottleneck; feces; individual identification; Pakistan; Ursus arctos ID RECENT POPULATION BOTTLENECKS; MICROSATELLITE ANALYSIS; URSUS-ARCTOS; NATURAL-POPULATIONS; ELUSIVE ANIMALS; CENTRAL-ASIA; DNA; FECES; IDENTIFICATION; DIVERSITY AB Asian bears face major threats due to the impact of human activities as well as a critical lack of knowledge about their status, distribution and needs for survival. Once abundant in northern Pakistan, the Himalayan brown bear (Ursus arctos isabellinus) has been exterminated in most of its former distribution range. It presently occurs sparsely, in small populations, the Deosai National Park supporting the largest isolate. This decline might imply a reduction in genetic diversity, compromising the survival of the population. Using a combination of fecal DNA analysis and field data, our study aimed at assessing the size and genetic status of the Deosai population and give guidelines for its conservation and management. Using fecal genetic analysis, we estimated the population to be 40-50 bears, which compares well with the field census of 38 bears. The northern Pakistani brown bear population may have undergone an approximate 200-300-fold decrease during the last thousand years, probably due to glaciations and the influence of growing human population. However, in spite of the presence of a bottleneck genetic signature, the Deosai population has a moderate level of genetic diversity and is not at immediate risk of inbreeding depression. Gene flow might exist with adjacent populations. We recommend careful monitoring of this population in the future both with field observations and genetic analyses, including sampling of adjacent populations to assess incoming gene flow. The connectivity with adjacent populations in Pakistan and India will be of prime importance for the longterm survival of Deosai bears. (c) 2006 Elsevier Ltd. All rights reserved. C1 Univ Grenoble 1, CNRS, Lab Ecole Alpine, UMR 5553, F-38041 Grenoble 9, France. Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, NO-1432 As, Norway. Univ Tuscia, Dipartimento Ecol & Sviluppo Econ Sostenibile, I-01100 Viterbo, Italy. Norwegian Inst Nat Res, NO-7485 Trondheim, Norway. Himalayan Wildlife Fdn, Islamabad, Pakistan. RP Bellemain, E (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. EM evabellemain@gmail.com; ali.nawaz@umb.no; alice.valentini@e.ujf-grenoble.fr; jon.swenson@umb.no; pierre.taberlet@ujf-grenoble.fr RI Bellemain, Eva/B-4493-2011; Nawaz, Muhammad Ali/C-1125-2012; Swenson, Jon/E-2883-2013; OI Nawaz, Muhammad Ali/0000-0001-5632-9014; valentini, alice/0000-0001-5829-5479 NR 51 TC 27 Z9 30 U1 0 U2 16 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD FEB PY 2007 VL 134 IS 4 BP 537 EP 547 DI 10.1016/j.biocon.2006.09.004 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 144BJ UT WOS:000244769800008 ER PT J AU Dove, CJ Agreda, A AF Dove, Carla J. Agreda, Ana TI Differences in plumulaceous feather characters of dabbling and diving ducks SO CONDOR LA English DT Article DE ducks; feather characters; microscopic; plumulaceous ID IDENTIFICATION AB We examined variation in five microscopic plumulaceous (downy) feather characters of eighteen species of dabbling (Anatini) and diving (Aythyini, Mergini) ducks to quantify the differences between these tribes, and to explain how the plumulaceous feather ultrastructure in ducks may be influenced by different ecological requirements. Over 75% of the variation in feather characters among these ducks was explained by the first two components of a principal components analysis (PCA). Component I explained 51% of the variation and was positively correlated with the characters that quantified the number of barbules with expanded nodes and the number of expanded nodes on barbules. The microscopic feather characters of dabbling ducks (Anatini) have triangular-shaped, expanded nodes on most proximal barbules, whereas diving ducks (Aythyini and Mergini) lack expanded nodes on some barbules. Anatini also have a greater density of expanded nodes per barbule, wider nodes, shorter distance between expanded nodes, and longer barbule length. Further analysis of node density across all taxa showed that as dive depths increase, the number of expanded nodes per barbule decreases, and in the deepest divers many of the barbules completely lack expanded nodes. The significantly greater density of expanded nodes in dabbling ducks suggests that the downy nodes may function to trap more air. Diving species have fewer expanded nodes, less buoyant plumage, and are more efficient at foraging in deeper water than dabbling ducks. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC USA. Catholic Univ Ecuador, Dept Biol, Quito, Ecuador. RP Dove, CJ (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, E-600,MRC 116,POB 37012, Washington, DC USA. EM dovec@si.edu NR 17 TC 6 Z9 8 U1 0 U2 6 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 FEB PY 2007 VL 109 IS 1 BP 192 EP 199 DI 10.1650/0010-5422(2007)109[192:DIPFCO]2.0.CO;2 PG 8 WC Ornithology SC Zoology GA 135HX UT WOS:000244145800019 ER PT J AU Gonzales, EE van der Zee, M Dictus, WJAG van den Biggelaar, J AF Gonzales, Eric E. van der Zee, Maurijn Dictus, Wim J. A. G. van den Biggelaar, Jo TI Brefeldin A or monensin inhibits the 3D organizer in gastropod, polyplacophoran, and scaphopod molluscs SO DEVELOPMENT GENES AND EVOLUTION LA English DT Article DE developmental signaling center; monensin; brefeldin A; spiral cleavage; 3D organizer ID PATELLA-VULGATA; MESENTOBLAST DETERMINATION; ILYANASSA-OBSOLETA; D MACROMERE; EMBRYOS; SPECIFICATION; MICROMERES; EVOLUTION; BILATERIA; PATTERNS AB In molluscs, the 3D vegetal blastomere acts as a developmental signaling center, or organizer, and is required to establish bilateral symmetry in the embryo. 3D is similar to organizing centers in other metazoans, but detailed comparisons are difficult, in part because its organizing function is poorly understood. To elucidate 3D function in a standardized fashion, we used monensin and brefeldin A (BFA) to rapidly and reversibly interfere with protein processing and secretion, thereby inhibiting the signaling interactions that underlie its specification and patterning. In the gastropods, Patella vulgata and Lymnaea stagnalis, the polyplacophoran, Mopalia muscosa, and the scaphopod, Antalis entalis, treatments initiated before the organizer-dependent onset of bilateral cleavage resulted in radialization of subsequent development. In radialized P. vulgata, L. stagnalis, and M. muscosa, organizer specification was blocked, and embryos failed to make the transition to bilateral cleavage. In all four species, the subsequent body plan was radially symmetric and was similarly organized about a novel aboral-oral axis. Our results demonstrate that brefeldin A (BFA) and monensin can be used to inhibit 3D's organizing function in a comparative fashion and that, at least in M. muscosa, the organizer-dependent developmental architecture of the embryo predicts subsequent patterns of morphogenetic movements in gastrulation and, ultimately, the layout of the adult body plan. C1 Univ Calif Berkeley, Ctr Integrat Genom, Berkeley, CA 94720 USA. Univ Utrecht, Dept Dev Biol, NL-3584 CH Utrecht, Netherlands. Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Gonzales, EE (reprint author), Univ Calif Berkeley, Ctr Integrat Genom, 142 Life Sci Addit, Berkeley, CA 94720 USA. EM eegonzales@berkeley.edu NR 31 TC 9 Z9 9 U1 2 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0949-944X J9 DEV GENES EVOL JI Dev. Genes Evol. PD FEB PY 2007 VL 217 IS 2 BP 105 EP 118 DI 10.1007/s00427-006-0118-z PG 14 WC Cell Biology; Evolutionary Biology; Developmental Biology SC Cell Biology; Evolutionary Biology; Developmental Biology GA 131XC UT WOS:000243904400002 PM 17120024 ER PT J AU Sousa, WP Kennedy, PG Mitchell, BJ Ordonez, BM AF Sousa, Wayne P. Kennedy, Peter G. Mitchell, Betsy J. Ordonez, Benjamin M. TI Supply-side ecology in mangroves: Do propagule dispersal and seedling establishment explain forest structure? SO ECOLOGICAL MONOGRAPHS LA English DT Review DE Avicennia germinans; dispersal limitation; hydrochory; Laguncularia racemosa; mangrove; propagule dispersal; Rhizophora mangle; seedling establishment; supply-side ecology; tidal sorting hypothesis; tropical forests; zonation ID AVICENNIA-MARINA PROPAGULES; COMMUNITY-LEVEL CONSEQUENCES; INDO-WEST-PACIFIC; NEOTROPICAL PALEOBOTANY; RHIZOPHORA-MANGLE; GENETIC-STRUCTURE; EARLY GROWTH; SEA-LEVEL; INTERTIDAL DISTRIBUTION; SOUTHEASTERN AUSTRALIA AB Theory and empirical evidence suggest that spatial and temporal variation in propagule availability can have as great or greater an influence on community structure as post-recruitment biotic interactions, a phenomenon known as supply-side ecology. One of the first theories to invoke supply-side dynamics, D. Rabinowitz's Tidal Sorting Hypothesis (TSH), attributed the tidal zonation of mangrove tree species to the interacting effects of water depth and propagule size on dispersal and establishment. According to the TSH, smaller propagules are carried farther inland by flood tides than larger ones, stranding and establishing in greater numbers at upper tidal elevations. In contrast, larger propagules are better able to establish in deeper, more seaward areas because their size affords greater access to the soil surface and resistance to buffeting by moving water. Here we present results of the first comprehensive investigation of the TSH. In a series of experiments conducted at Punta Galeta on the Caribbean coast of Panama, we quantified patterns of propagule dispersal and establishment of the three dominant species: Avicennia germinans, Laguncularia racemosa, and Rhizophora mangle. To measure dispersal patterns, we monitored movements (directions and distances) of marked propagules released at three elevations along each of three transects. On all transects, regardless of species or elevation, propagules moved seaward rather than being carried inland by tides, as predicted by the TSH. Rates of seedling establishment were monitored in experiments conducted at different tidal elevations. Contrary to the TSH, all three species established best in the lower intertidal, where they were in prolonged contact with the soil surface during low tides, and established more poorly in the upper intertidal basin, where standing water made rooting difficult. Seedling establishment was lowest in the wave-exposed, back reef habitat, but in accordance with the TSH, the large propagules of Rhizophora rooted and persisted better in this turbulent habitat than did the smaller propagules of the other species. We conclude that the TSH does not explain the vertical distributions of mangrove species on Punta Galeta. Rather, a different form of supply-side dynamics imposed by the strong seaward movement of dispersing propagules is important in structuring our study forests. C1 Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Galeta Marine Lab, APO, AA 34002 USA. RP Sousa, WP (reprint author), Univ Calif Berkeley, Dept Integrat Biol, 3060 Valley Life Sci Bldg, Berkeley, CA 94720 USA. EM wpsousa@berkeley.edu NR 127 TC 46 Z9 50 U1 7 U2 48 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9615 J9 ECOL MONOGR JI Ecol. Monogr. PD FEB PY 2007 VL 77 IS 1 BP 53 EP 76 DI 10.1890/05-1935 PG 24 WC Ecology SC Environmental Sciences & Ecology GA 155UM UT WOS:000245603900004 ER PT J AU Sorensen, S AF Sorensen, Sorena TI About the review process SO ELEMENTS LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Sorensen, S (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1811-5209 J9 ELEMENTS JI Elements PD FEB PY 2007 VL 3 IS 1 BP 6 EP 6 PG 1 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 140GG UT WOS:000244492000004 ER PT J AU Russell, MJ Montagna, PA AF Russell, Marc J. Montagna, Paul A. TI Spatial and temporal variability and drivers of net ecosystem metabolism in western Gulf of Mexico estuaries SO ESTUARIES AND COASTS LA English DT Article ID DISSOLVED-OXYGEN DYNAMICS; FRESH-WATER INFLOW; CHESAPEAKE BAY; US ESTUARIES; RESPIRATION; TEXAS; CARBON AB Net ecosystem metabolism (NEM) is becoming a commonly used ecological indicator of estuarine ecosystem metabolic rates. Estuarine ecosystem processes are spatially and temporally variable, but the corresponding variability in NEM has not been properly assessed. Spatial and temporal variability in NEM was assessed in four western Gulf of Mexico shallow water estuaries. NEM was calculated from high-frequency dissolved oxygen measurements. Interbay, intrabay, and water column spatial scales were assessed for NEM, gross primary production (GPP), and respiration (R) rate variability. Seasonal, monthly, and daily temporal scales in NEM, GPP, and R were also assessed. Environmental conditions were then compared to NEM to determine which factors were correlated with each temporal and spatial scale. There was significant NEM spatial variability on interbay, intrabay, and water column spatial scales. Significant spatial variability was ephemeral, so it was difficult to ascertain which environmental conditions were most influential at each spatial scale. Significant temporal variability in NEM on seasonal, monthly, and daily scales was found and it was correlated to temperature, salinity, and freshwater inflow, respectively. NEM correlated strongly with dissolved oxygen, temperature, and salinity, but the relationships where different in each bay. The dynamics of NEM on daily scales indicate that freshwater inflow events may be the main driver of NEM in the semiarid estuaries studied. The variable nature of NEM found here is further evidence that it is not valid to use single station monitoring deployments for assessment of whole estuarine ecosystem metabolic rates in large ecosystems. The relationship between NEM and temperature, salinity, and freshwater inflow events could drive predictive models assessing the potential influence of projected climate change and watershed development scenarios on estuarine metabolic rates. C1 Univ Texas, Inst Marine Sci, Port Aransas, TX 78373 USA. RP Russell, MJ (reprint author), Smithsonian Environm Res Inst, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21027 USA. EM russellm@si.edu NR 27 TC 26 Z9 27 U1 1 U2 12 PU ESTUARINE RESEARCH FEDERATION PI PORT REPUBLIC PA 2018 DAFFODIL, PO BOX 510, PORT REPUBLIC, MD 20676 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD FEB PY 2007 VL 30 IS 1 BP 137 EP 153 PG 17 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 149GD UT WOS:000245134200014 ER PT J AU Baena, ML Eberhard, WG AF Baena, M. L. Eberhard, W. G. TI Appearances deceive: female "resistance" behaviour in a sepsid fly is not a test of male ability to hold on SO ETHOLOGY ECOLOGY & EVOLUTION LA English DT Article DE female resistance behaviour; sexual selection; female choice; sexually antagonistic coevolution; sepsid flies ID COQUILLETT DIPTERA-CERATOPOGONIDAE; SEXUAL SIZE DIMORPHISM; MATING-BEHAVIOR; FUNCTIONAL-MORPHOLOGY; MATE CHOICE; BODY-SIZE; FLUCTUATING ASYMMETRY; REPRODUCTIVE BEHAVIOR; GENITALIC SURSTYLI; MALE ARCHISEPSIS AB Female rejections of males are crucial events in sexual selection by female choice and sexually antagonistic coevolution, but there are few detailed studies of the process of rejection. Female struggles when mounted by males are often assumed to function to dislodge the male. But this study, in which female receptivity was manipulated by using females of different ages, showed that this "dislodgement" hypothesis is incorrect in a group (sepsid flies) in which energetic female shaking behaviour was previously interpreted as female attempts to dislodge males. Mounts in Archisepsis diversiformis often failed, but males were nevertheless seldom thrown off; instead, they almost always dismounted while the female was quiet. Males also showed signs of being in control of dismounts, as they dismounted more quickly if the female had recently been mounted by another male. Predictions from two other hypotheses for the function of female resistance behaviour also either failed or were not consistently supported: (1) females resist in order to filter males with respect to their ability to hold on to the female or outlast her resistance, or to court while mounted ("male endurance/ female exhaustion" hypothesis); (2) females resist in order to sense the male's grip on her wings and thus filter males with respect to their species-specific clamps or to elicit other male courtship ("male screening" hypothesis). Several predictions of a further possibility, that (3) females resist in order to communicate their lack of receptivity to the male, and to induce him to leave ("communication" hypothesis), were confirmed. Although one type of data did not fit easily with the communication hypothesis, overall it was the most likely explanation for female shaking behaviour. Our results call into question conclusions from previous studies regarding male-female conflict in this and other groups, and suggest testable alternative hypotheses. A survey of behaviour in other flies (which are presumably indicative of other animals in this respect) indicates that female "resistance" behaviour probably has a variety of functions. In sum, facile interpretations of a forceful resistance function should not be accepted without careful analyses. C1 Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Smithsonian Trop Res Inst, Balboa, Panama. RP Baena, ML (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. EM archisepsis@biologia.ucr.ac.cr NR 66 TC 12 Z9 12 U1 1 U2 9 PU UNIVERSITA DEGLI STUDI DI FIRENZE PI FLORENCE PA C/O PROF F DESSI-FULGHERI, VIA ROMANA 17, 50125 FLORENCE, ITALY SN 0394-9370 J9 ETHOL ECOL EVOL JI Ethol. Ecol. Evol. PD FEB PY 2007 VL 19 IS 1 BP 27 EP 50 PG 24 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 167MB UT WOS:000246454700002 ER PT J AU Weltzin, JF Belote, RT Williams, LT Keller, JK Engel, EC AF Weltzin, Jake F. Belote, R. Travis Williams, Leigh T. Keller, Jason K. Engel, E. Cayenne TI Ensuring that "authors" write - The authors reply SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Letter C1 Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. Virginia Polytech Inst & State Univ, Dept Biol Sci, Blacksburg, VA 24061 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Weltzin, JF (reprint author), Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. EM jweltzin@utk.edu NR 0 TC 0 Z9 0 U1 0 U2 4 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD FEB PY 2007 VL 5 IS 1 BP 11 EP 11 PG 1 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 133VP UT WOS:000244042300017 ER PT J AU Santiago, LS Wright, SJ AF Santiago, L. S. Wright, S. J. TI Leaf functional traits of tropical forest plants in relation to growth form SO FUNCTIONAL ECOLOGY LA English DT Article DE canopy crane; leaf life span; liana; palm; photosynthesis; tropical forest physiology ID WATER-STRESS; TREES; LIANAS; LEAVES; SHADE; SUN; CONDUCTIVITY; RECRUITMENT; GENERALITY; STRATEGIES AB 1. We tested the generality of global leaf trait relationships among 44 tropical plant species from a broad array of growth forms (trees, lianas and understorey plants) in lowland Panama to determine how leaf trait relationships vary with whole-plant morphology within one site. 2. We observed significant variation among growth forms for seven out of 10 leaf traits. Variation in leaf traits among growth forms was more pronounced per area than per mass. Thirteen bivariate leaf trait relationships that describe how plants allocate resources to photosynthesis were significant across all species. Growth forms showed distinct slopes, intercepts or shifts in the common slope for 12 of the 13 relationships. 3. Trait relationships within trees and lianas showed good agreement with a global leaf trait data set. However, for understorey plants, trait relationships that included specific leaf area (SLA) deviated from the global data set, suggesting that understorey leaf-allocation patterns optimize SLA, and hence growth. 4. Lianas showed lower values and rates of gas exchange than trees, and longer leaf life span for a given SLA, illustrating variation in leaf traits associated with growth form and canopy geometry. 5. Functional variation in allocation to photosynthetic capacity among tropical forest species is related to microhabitat variations in light availability and whole-plant morphology among growth forms. C1 Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Santiago, LS (reprint author), Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. EM santiago@ucr.edu RI Wright, Stuart/M-3311-2013; Santiago, Louis/E-3185-2016 OI Wright, Stuart/0000-0003-4260-5676; Santiago, Louis/0000-0001-5994-6122 NR 41 TC 94 Z9 105 U1 4 U2 54 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2007 VL 21 IS 1 BP 19 EP 27 DI 10.1111/j.1365-2435.2006.01218.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 124ZV UT WOS:000243412200003 ER PT J AU Liu, F Chen, J Chai, J Zhang, X Bai, X He, D Roubik, DW AF Liu, F. Chen, J. Chai, J. Zhang, X. Bai, X. He, D. Roubik, D. W. TI Adaptive functions of defensive plant phenolics and a non-linear bee response to nectar components SO FUNCTIONAL ECOLOGY LA English DT Article DE Apis cerana; bees; nectar constituents; phenolics ID MIMICKING FLORAL NECTARS; APIS-MELLIFERA L.; HONEY-BEES; ALMOND NECTAR; TOXIC NECTAR; AMINO-ACIDS; POLLEN; HYMENOPTERA; QUANTIFICATION; ATTRACTIVENESS AB 1. Secondary compounds such as phenolics, usually present in floral nectar, may act in combination with sugar components to influence the evolution of pollination mutualism. 2. Previous work on the significance of secondary compounds in nectar considers honey bee responses to those compounds alone, but neglects sugar. Our experiments demonstrated that phenolic sugar syrups were attractants to free-flying Asian Apis cerana Fab. when sugar concentrations were 15-35%, but were deterrents below or above this range. 3. Synergism between nectar phenolics and sugar may thus provide a novel mechanism for plants to encourage pollinating bees and reduce energy investment in nectar, operating as exaptations by co-opting defence mechanisms against herbivores. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Kunming Div, Kunming 650223, Peoples R China. Yunnan Acad Agr Sci, Inst Sericulture & Apiculture, Mengzi 661101, Peoples R China. RP Roubik, DW (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM roubikd@si.edu RI Marion-Poll, Frederic/D-8882-2011 OI Marion-Poll, Frederic/0000-0001-6824-0180 NR 45 TC 27 Z9 32 U1 2 U2 28 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2007 VL 21 IS 1 BP 96 EP 100 DI 10.1111/j.1365-2435.2006.01200.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 124ZV UT WOS:000243412200010 ER PT J AU Guyer, JI Lambin, EF Cliggett, L Walker, P Amanor, K Bassett, T Colson, E Hay, R Homewood, K Linares, O Pabi, O Peters, P Scudder, T Turner, M Unruh, J AF Guyer, Jane I. Lambin, Eric F. Cliggett, Lisa Walker, Peter Amanor, Kojo Bassett, Thomas Colson, Elizabeth Hay, Rod Homewood, Katherine Linares, Olga Pabi, Opoku Peters, Pauline Scudder, Thayer Turner, Matthew Unruh, John TI Temporal heterogeneity in the study of African land use - Interdisciplinary collaboration between anthropology, human geography and remote sensing SO HUMAN ECOLOGY LA English DT Article DE African land use; temporal heterogeneity; anthropology; long term studies; remote sensing ID COVER CHANGE; GIS; ECOLOGY; LANDSCAPE; INTENSIFICATION; DEFORESTATION; ETHNOGRAPHY; MANAGEMENT; SAVANNA; GUINEA AB This paper introduces a set of four collaborative papers exploring temporal heterogeneity in the analysis of African land use over a decadal time period, from 10 to 50 years, in the second half of the twentieth century. The four cases were chosen amongst the seven teams of anthropologists, human geographers and remote sensing specialists who had carried out long-term research and who met to discuss their findings at a workshop in 2003. All seven teams' work and the collective discussion-on Casamance (Senegal), Brong Ahafo (Ghana), Southern Niger/Northern Cote d'Ivoire, Oyo State (Nigeria), Maasai Mara (Kenya and Tanzania), Gwembe (Zambia), and Malawi-inform this introduction. We identify several temporal processes in all the cases, each operating on its own temporal frame: population growth and, above all, mobility; livelihood change through crop and occupational change; tenure ambiguity; powerful though "punctuated" interventions by state policy; and climate change. Conceptual and methodological implications are disussed. C1 Johns Hopkins Univ, Dept Anthropol, Baltimore, MD USA. Catholic Univ Louvain, Dept Geog, B-1348 Louvain La Neuve, Belgium. Univ Kentucky, Dept Anthropol, Lexington, KY USA. Univ Oregon, Dept Geog, Eugene, OR 97403 USA. Univ Ghana, Inst African Studies, Legon, Ghana. Univ Illinois, Dept Geog, Urbana, IL 61801 USA. Univ Calif Berkeley, Dept Anthropol, Berkeley, CA 94720 USA. Calif State Univ Dominguez Hills, Dept Earth Sci, Carson, CA 90747 USA. UCL, Dept Anthropol, London, England. Smithsonian Trop Res Inst, Balboa, Panama. Univ Ghana, Geog & Resource Dept, Legon, Ghana. Harvard Univ, Kennedy Sch Govt, Cambridge, MA 02138 USA. CALTECH, Dept Anthropol, Pasadena, CA 91125 USA. Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. McGill Univ, Dept Geog, Montreal, PQ, Canada. RP Guyer, JI (reprint author), Johns Hopkins Univ, Dept Anthropol, Baltimore, MD USA. EM jiguyer@jhu.edu; lambin@geog.ucl.ac.be; cligget@uky.edu; pwalker@uoregon.edu; ksamanor@ug.edu.gh; bassett@uiuc.edu; colson@sscl.berkeley.edu; RIIAY@csudh.edu; k.homewood@ucl.ac.uk; linareso@si.edu; opabi@yahoo.com; Pauline_Peters@harvard.edu; tzs@hss.caltech.edu; turner@geography.wisc.edu; jon.unruh@mcgill.ca OI Homewood, Katherine/0000-0001-7391-985X NR 96 TC 16 Z9 16 U1 3 U2 29 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0300-7839 EI 1572-9915 J9 HUM ECOL JI Hum. Ecol. PD FEB PY 2007 VL 35 IS 1 BP 3 EP 17 DI 10.1007/s10745-006-9085-2 PG 15 WC Anthropology; Environmental Studies; Sociology SC Anthropology; Environmental Sciences & Ecology; Sociology GA 136BQ UT WOS:000244198000002 ER PT J AU Busch, MW Ostro, SJ Benner, LAM Giorgim, JD Magri, C Howell, ES Nolan, MC Hine, AA Campbell, DB Shapiro, II Chandler, JF AF Busch, Michael W. Ostro, Steven J. Benner, Lance A. M. Giorgim, Jon D. Magri, Christopher Howell, Ellen S. Nolan, Michael C. Hine, Alice A. Campbell, Donald B. Shapiro, Irwin I. Chandler, John F. TI Arecibo radar observations of Phobos and Deimos SO ICARUS LA English DT Article DE Mars, satellites; radar observations; regoliths ID ASTEROIDS; GRAVITY AB In November 2005, we observed the moons of Mars using the Arecibo 2380-MHz (13-cm) radar, obtaining a result for the OC radar albedo of Phobos (0.056 +/- 0.014) consistent with its previously reported radar albedo and implying an upper bound on its near-surface bulk density of 1.6 +/- 0.3 g cm(-3). We detected Deimos by radar for the first time, finding its OC radar albedo to be 0.021 +/- 0.006, implying an upper bound on its near-surface density of 1.1 +/- 0.3 g cm(-3), consistent with a high-porosity regolith. We briefly discuss reasons for these low radar albedos, Deimos' being possibly the lowest of any Solar System body yet observed by radar. (c) 2006 Elsevier Inc. All rights reserved. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Maine, Farmington, ME 04938 USA. Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Busch, MW (reprint author), CALTECH, Div Geol & Planetary Sci, MC 150-21, Pasadena, CA 91125 USA. EM busch@caltech.edu RI Nolan, Michael/H-4980-2012 OI Nolan, Michael/0000-0001-8316-0680 NR 19 TC 6 Z9 6 U1 1 U2 2 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 FEB PY 2007 VL 186 IS 2 BP 581 EP 584 DI 10.1016/j.icarus.2006.11.003 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134KF UT WOS:000244081200022 ER PT J AU Walther, P Eisaman, MD Andre, A Massou, F Fleischhauer, M Zibrov, AS Lukin, MD AF Walther, P. Eisaman, M. D. Andre, A. Massou, F. Fleischhauer, M. Zibrov, A. S. Lukin, M. D. TI Generation of narrow-bandwidth single photons using electromagnetically induced transparency in atomic ensembles SO INTERNATIONAL JOURNAL OF QUANTUM INFORMATION LA English DT Article; Proceedings Paper CT Workshop on Advances in Foundations of Quantum Mechanics and Quantium Information with Atoms and Photons CY MAY 03-05, 2006 CL Ints Nazl Ric Metrol, Turin, ITALY SP Univ Bari, Univ Torino HO Ints Nazl Ric Metrol DE quantum repeater; atomic ensemble; EIT; single-photon ID QUANTUM COMMUNICATION; TURNSTILE DEVICE; LINEAR OPTICS; BELL THEOREM; LIGHT; STATE; ENTANGLEMENT; STORAGE; DEMAND; CRYPTOGRAPHY AB We review recent experiments [M. D. Eisaman et al., Nature 438 (2005) 837] demonstrating the generation of narrow-bandwidth single photons using a room-temperature ensemble of Rb-87 atoms. Our method involves creation of an atomic coherence via Raman scattering and projective measurement, followed by the coherent transfer of this atomic coherence onto a single photon using electromagnetically induced transparency (EIT). The single photons generated using this method are shown to have many properties necessary for quantum information protocols, such as narrow bandwidths, directional emission, and controllable pulse shapes. The narrow bandwidths of these single photons (similar to MHz), resulting from their matching to the EIT resonance(similar to MHz), allow them to be stored in narrow-bandwidth quantum memories. We demonstrate this by using dynamic EIT to store and retrieve the single photons in a second ensemble for storage times up to a few microseconds. We also describe recent improvements to the single-photon fedelity compared to the work by M. D. Eisaman in Nature 438 (2005) 837. These techniques may prove useful in quantum information applications such as quantum repeaters, linear-optics quantum computation, and daytime free-space quantum communication. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tech Univ Kaiserslautern, Fachbereich Phys, D-67663 Kaiserslautern, Germany. PN Lebedev Phys Inst, Moscow 117924, Russia. RP Walther, P (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Eisaman, Matthew/E-8006-2011; Fleischhauer, Michael/G-6716-2011; Zibrov, Alexander/G-7419-2014; OI Eisaman, Matthew/0000-0002-3814-6430; Walther, Philip/0000-0002-4964-817X NR 56 TC 8 Z9 8 U1 1 U2 5 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0219-7499 J9 INT J QUANTUM INF JI Int. J. Quantum Inf. PD FEB-APR PY 2007 VL 5 IS 1-2 BP 51 EP 62 DI 10.1142/S0219749907002773 PG 12 WC Computer Science, Theory & Methods; Physics, Particles & Fields; Physics, Mathematical SC Computer Science; Physics GA 230FV UT WOS:000250862500008 ER PT J AU van Ballegooijen, AA DeLuca, EE Squires, K Mackay, DH AF van Ballegooijen, A. A. DeLuca, E. E. Squires, K. Mackay, D. H. TI Modeling magnetic flux ropes in the solar atmosphere SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article; Proceedings Paper CT Huntsville Workshop on Challenges to Modeling the Sun-Earth System CY OCT 18-22, 2004 CL Huntsville, AL DE solar corona; solar magnetic fields; coronal mass ejections; solar prominences ID CONFIGURATIONS SUPPORTING PROMINENCES; FORCE-FREE; ACTIVE-REGION; QUIESCENT PROMINENCES; HEMISPHERIC PATTERN; FILAMENT CHANNEL; LATERAL FEET; FIELDS; EVOLUTION; HELICITY AB Coronal flux ropes are highly sheared or twisted magnetic fields overlying polarity inversion lines on the solar photosphere. The formation of such flux ropes is briefly discussed. A coronal flux rope can be stable for many days and then suddenly lose equilibrium and erupt, producing a coronal mass ejection (CME). To understand what causes such eruptions, we need to determine the 3D magnetic structure of observed active regions prior to CMEs. This requires constructing nonlinear force free field models of active regions based on observed photospheric vector fields, H alpha filaments, or coronal loop structures. We describe a new method for constructing models containing flux ropes. (c) 2006 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nashoba Reg High Sch, Bolton, MA 01740 USA. Univ St Andrews, Dept Math & Computat Sci, St Andrews KY16 9SS, Fife, Scotland. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vanballe@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 44 TC 12 Z9 12 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD FEB PY 2007 VL 69 IS 1-2 BP 24 EP 31 DI 10.1016/j.jastp.2006.06.007 PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 141CC UT WOS:000244553100004 ER PT J AU McLaughlin, PA Lemaitre, R Sorhannus, U AF McLaughlin, Patsy A. Lemaitre, Rafael Sorhannus, Ulf TI Hermit crab phylogeny: A reappraisal and its "fall-out" SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Review ID EARLY JUVENILE DEVELOPMENT; FRESH-WATER CRABS; CRUSTACEA-DECAPODA; PAGURUS-POLLICARUS; SHELL POSITION; POSTURAL CONTROL; NEOGLYPHEA-INOPINATA; SUPERFICIAL MUSCLES; AEGLA DECAPODA; ANOMURA AB The hypothesis of monophyly in Paguroidea and the relationship of this superfamily to the other three superfamilies of Anomura have been reassessed using current cladistic methods and computer generated analysis. In the analysis, 79 external morphological characters were examined for an in-group consisting of the seven paguroid families, Pylochelidae, Coenobitidae, Diogenidae, Pylojacquesidae, Paguridae, Parapaguridae, and Lithodidae (divided into the subfamilies Lithodinae and Hapalogastrinae), three hippoid families, Blepharipodidae, Albuneidae, and Hippidae, five galatheoid families, Galatheidae, Chirostylidae, Kiwaidae, Aeglidae, and Porcellanidae, and the Lomisoidea's monotypic Lomisidae. The out-group was comprised of Neoglyphea inopinata, representing Fractosternalia, and the families Dromiidae and Dynomenidae representing Brachyura. This analysis has shown that Anomura indeed is a monophyletic infraorder, as is Hippoidea a monophyletic superfamily. However, while six of the paguroid families form a cohesive clade, the two subfamilies of Lithodidae form a distinct clade more closely related to the superfamily Hippoidea than to the other paguroids. Galatheoidea, as presently constituted, is polyphyletic. Aeglidae, like Lithodidae, is more closely related to Hippoidea than to the galatheoid clade formed by the families Galatheidae, Chirostylidae, and Porcellanidae. Kiwaidae is also distinct from Galatheoidea sensu stricto, but its relationship, and that of Lomisoidea, to the remainder of the anomuran taxa are unresolved in the present analysis. As a result of this reappraisal, we propose that Lithodidae be removed from Paguroidea sensu lato and elevated to superfamily rank with families Lithodidae and Hapalogastridae. Similarly, we propose that Galatheoidea be restricted to the families Galatheidae, Chirostylidae, and Porcellanidae, whereas Kiwaidae and Aeglidae are each to be elevated to superfamily rank. Anomura will then consist of seven superfamilies, Hippoidea, Lithodoidea, Aegloidea, Lomisoidea, Kiwaoidea, Galatheoidea sensu stricto, and Paguroidea sensu stricto. C1 Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. Edinboro Univ Penn, Dept Biol & Hlth Serv, Edinboro, PA 16444 USA. RP McLaughlin, PA (reprint author), Western Washington Univ, Shannon Point Marine Ctr, 1900 Shannon Point Rd, Anacortes, WA 98221 USA. EM hermit@fidalgo.net; lemaitrr@si.edu NR 166 TC 79 Z9 84 U1 0 U2 12 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD FEB PY 2007 VL 27 IS 1 BP 97 EP 115 DI 10.1651/S-2675.1 PG 19 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 134ZB UT WOS:000244122300014 ER PT J AU Henry, M Kalko, EKV AF Henry, Mickael Kalko, Elisabeth K. V. TI Foraging strategy and breeding constraints of Rhinophylla pumilio (Phyllostomidae) in the Amazon lowlands SO JOURNAL OF MAMMALOGY LA English DT Article DE activity pattern; breeding behavior; foraging activity; French Guiana; fruit bat; lactation; Phyllostomidae; Rhinophylla pumilio ID CAROLLIA-CASTANEA PHYLLOSTOMIDAE; BATS MYOTIS-LUCIFUGUS; FRENCH-GUIANA; FOREST FRAGMENTS; FRUGIVOROUS BAT; LOS-TUXTLAS; HOME-RANGE; PIPISTRELLUS-PIPISTRELLUS; ARTIBEUS-JAMAICENSIS; INSECTIVOROUS BAT AB Bat diversity peaks in neotropical lowland forests, where 70-100 species may coexist in local assemblages. Understanding of factors that promote and maintain this diversity requires a thorough knowledge of the ecology and behavior of individual species. We studied the movement pattern, focusing on range size and foraging strategy, of the small frugivorous bat Rhinophylla pumilio (Phyllostomidae), with particular emphasis on constraints females have to deal with when rearing young. Because of the scattered distribution of its main food resource, infructescences of epiphytes, we hypothesized that R. pumilio should spend most of its flight time searching for food. Because its small body size incurs higher flight costs in comparison to larger fruit-eating bats, we further proposed that it should feed within small foraging areas that are close to each other and that commuting flights between foraging areas should be short and infrequent, resulting in small home ranges. Furthermore, we predicted that lactating females would change range size as well as activity budget by performing more search flights to increase food intake for milk production and more commuting flights to feed their young during nighttime. We radiotracked 9 females (4 nonreproductive, 4 lactating, and I subadult) and 2 males in the primary rain forest of Nouragues, French Guiana, for a total of 49 nights. Supporting our initial prediction, the foraging strategy of R. pumilio was mostly restricted to short (40- to 120-m) search flights in a single, rather small foraging area (3.5-14.1 ha). We observed a decrease in flight distances and size of foraging area, and an increase in total flight time throughout the night in lactating females that probably transported their young and nursed them in their foraging areas at night. Finally, we propose that the sensitivity of R. pumilio to forest fragmentation reported in previous studies may in part be caused by its foraging strategy because it consists mostly of short-distance search flights that make it difficult or impossible, particularly for lactating females, to regularly cross broad expanses of inhospitable matrix in fragmented forests. Fragmentation may therefore decrease breeding success and foster population decline in this species. C1 Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. CNRS, MNHN, UMR 5176, Dept Ecol & Gest Biodivers, F-91800 Brunoy, France. RP Kalko, EKV (reprint author), Univ Ulm, Dept Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM elisabeth.kalko@uni-ulm.de NR 69 TC 18 Z9 18 U1 1 U2 12 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD FEB PY 2007 VL 88 IS 1 BP 81 EP 93 DI 10.1644/06-MAMM-A-001R1.1 PG 13 WC Zoology SC Zoology GA 142BK UT WOS:000244623500010 ER PT J AU Lambert, JB Kozminski, MA Fahlstrom, CA Santiago-Blay, JA AF Lambert, Joseph B. Kozminski, Michael A. Fahlstrom, Carl A. Santiago-Blay, Jorge A. TI Proton nuclear magnetic resonance characterization of resins from the family Pinaceae SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID CLASSIFICATION AB Proton magnetic resonance spectra were recorded for solutions of resinous materials harvested from 82 species in seven genera of the gymnospermous plant family Pinaceae. Data were recorded in both one and two (COSY) dimensions. Approximately 11 peaks in the 1D spectra and 10 cross-peaks in the 2D spectra were present in almost all pinacean spectra, providing a familial diagnostic. Some 40 1D peaks or peak clusters and 60 2D cross-peaks or clusters were considered significant and are reported, when present, for all species. Whereas previous solid-state C-13 data were diagnostic primarily at the family level, the patterns of 1D and 2D peaks may provide diagnostic information at the genus and species levels. These spectra constitute the first broad use of H-1 NMR to study plant exudates in general and to provide taxonomic characterization in particular. C1 Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. Smithsonian Inst, Museum Natl Hist Nat, 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 12 TC 8 Z9 11 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD FEB PY 2007 VL 70 IS 2 BP 188 EP 195 DI 10.1021/np060486i PG 8 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 138VH UT WOS:000244390900007 PM 17315958 ER PT J AU Pfaff, A Robalino, J Walker, R Aldrich, S Caldas, M Reis, E Perz, S Bohrer, C Arima, E Laurance, W Kirby, K AF Pfaff, Alexander Robalino, Juan Walker, Robert Aldrich, Steven Caldas, Marcellus Reis, Eustaquio Perz, Stephen Bohrer, Claudio Arima, Eugenio Laurance, William Kirby, Kathryn TI Roads and deforestation in the Brazilian Amazon SO JOURNAL OF REGIONAL SCIENCE LA English DT Article ID LAND-USE; ENVIRONMENT; SATELLITE AB Understanding the impact of road investments on deforestation is part of a complete evaluation of the expansion of infrastructure for development. We find evidence of spatial spillovers from roads in the Brazilian Amazon: deforestation rises in the census tracts that lack roads but are in the same county as and within 100 km of a tract with a new paved or unpaved road. At greater distances from the new roads the evidence is mixed, including negative coefficients of inconsistent significance between 100 and 300 km, and if anything, higher neighbor deforestation at distances over 300 km. C1 Columbia Univ, Earth Inst, New York, NY 10025 USA. Michigan State Univ, Dept Geog, E Lansing, MI 48824 USA. Inst Pesquisa Econ Aplicada, BR-20020 Rio De Janeiro, Brazil. Univ Florida, Dept Sociol, Gainesville, FL 32611 USA. Univ Fed Fluminense, Dept Geog, BR-24210340 Niteroi, RJ, Brazil. Hobart & William Smith Coll, Dept Environm Studies, Geneva, NY 14456 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Pfaff, A (reprint author), Columbia Univ, Earth Inst, Hogan Hall,2910 Broadway, New York, NY 10025 USA. EM ap196@columbia.edu; jar101@columbia.edu; rwalker@msu.edu; aldric30@msu.edu; caldasma@msu.edu; ejreis@ipea.gov.br; sperz@mail.clas.ufl.edu; bohrer@vm.uff.br; arima@hws.edu; laurance@si.edu RI Aldrich, Stephen/E-6577-2011; Caldas, Marcellus/C-1955-2014; OI Aldrich, Stephen/0000-0002-0492-2841; Robalino, Juan/0000-0003-1450-7382 NR 21 TC 61 Z9 66 U1 2 U2 17 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-4146 J9 J REGIONAL SCI JI J. Reg. Sci. PD FEB PY 2007 VL 47 IS 1 BP 109 EP 123 DI 10.1111/j.1467-9787.2007.00502.x PG 15 WC Economics; Environmental Studies; Planning & Development SC Business & Economics; Environmental Sciences & Ecology; Public Administration GA 131LM UT WOS:000243870500006 ER PT J AU Zotz, G AF Zotz, G. TI Johansson revisited: the spatial structure of epiphyte assemblages SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Bromeliaceae; Cactaceae; Johansson scheme; niche; Orchidaceae; San Lorenzo crane site; substrate preference; vertical structure ID RAIN-FOREST; VASCULAR EPIPHYTES; CENTRAL VERACRUZ; CLOUD FOREST; COSTA-RICA; TREE SIZE; MEXICO; COMMUNITIES; VEGETATION; VENEZUELA AB Question: Vertical zonation schemes are widely used in bio-diversity studies with vascular epiphytes as a toot to capture spatial distribution patterns, the one most commonly used was proposed by Johansson more than 30 years ago. Does a survey of the epiphytes found on larger trees really yield a representative sample of the local community? Location: Lowland rainforest of the San Lorenzo Crane Plot, Republic of Panama. Methods: A complete census of the vascular epiphytes on all trees > 1 cm DBH in 0.4 ha of undisturbed lowland forest was analysed with both cluster and discriminant analysis to detect groupings of epiphyte species. Results: Six different groups of species were detected, five of them preferring different substrates on larger trees (as defined by (1) the height above ground at the attachment site, (2) the diameter of the substrate and (3) the occurrence on stem vs branches/twigs) and resembling to some extent the original Johansson zones. A sixth group of epiphytes, comprising ca. 10% of all taxa, was almost always found on small diameter stems and branches of trees with small DBH at lower and intermediate heights within the forest. Conclusions: Applying pre-established zonation schemes may lead to misleading results in bio-diversity studies with epiphytes. Important aspects of spatial distribution patterns may be missed, and the determination of relative species abundances may carry a strong quantitative and qualitative bias when analyses rely completely on epiphytic plants found on larger trees. C1 Carl von Ossietzky Univ Oldenburg, AG Funkt Okol Pflanzen, Inst Biol & Umweltwissensch, D-26111 Oldenburg, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, AG Funkt Okol Pflanzen, Inst Biol & Umweltwissensch, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 35 TC 30 Z9 32 U1 3 U2 14 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD FEB PY 2007 VL 18 IS 1 BP 123 EP 130 DI 10.1658/1100-9233(2007)18[123:JRTSSO]2.0.CO;2 PG 8 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 153IZ UT WOS:000245427300014 ER PT J AU Miglietta, MP Piraino, S Kubota, S Schuchert, P AF Miglietta, M. P. Piraino, S. Kubota, S. Schuchert, P. TI Species in the genus Turritopsis (Cnidaria, Hydrozoa): a molecular evaluation SO JOURNAL OF ZOOLOGICAL SYSTEMATICS AND EVOLUTIONARY RESEARCH LA English DT Article DE Turritopsis; Hydrozoa; phylogeny; systematics; species introduction ID ATHECATE HYDROIDS; LIFE-CYCLE; NUTRICULA AB Mitochondrial ribosomal gene sequences were used to investigate the status of several populations of hydromedusae belonging to the genus Turritopsis (family Oceaniidae). Several nominal species have been described for this genus, but most of them had been synonymized and attributed to one cosmopolitan species, Turritopsis nutricula. A recent revision based on morphological and reproductive characters, however, has shown that many different populations can be distinguished and that several of the nominal Turritopsis species are likely valid biological species. Our investigation using molecular sequence data of 16S mitochondrial gene confirms these results. The Mediterranean Turritopsis must be attributed to Turritopsis dohrnii and the Turritopsis of New Zealand must be referred to Turritopsis rubra. The situation of the Japanese Turritopsis is more complex, though all sampled populations are clearly distinct from T. nutricula, a species likely confined to the Western Atlantic. The Japanese Turritopsis fall into three widely separated lineages. One of them, corresponding likely to Turritopsis pacifica, is closely related to T. rubra. A second clade, which potentially represents an as yet undescribed species, produces smaller medusae than T. pacifica and is morphologically distinguishable from it. Finally, a third group was distinguished by a single haplotype sequence that is identical with a Mediterranean sample of T. dohrnii. It is postulated that the last group of Japanese Turritopsis is likely a recent introduction, most probably by human activity. A survey of all known and potentially valid Turritopsis species is given in table format to facilitate identifications and future revisory work. C1 Duke Univ, Dept Biol, Durham, NC USA. Univ Lecce, Dipartimento Sci & Tecnol Biol Ambientali, I-73100 Lecce, Italy. Kyoto Univ, Seto Marine Biol Lab, Field Sci Educ & Res Ctr, Wakayama, Japan. Museum Nat Hist, Geneva, Switzerland. RP Miglietta, MP (reprint author), Smithsonian Trop Res Inst, Naos Lab, Box 0843-03092, Balboa, Panama. EM migliettam@si.edu; stefano.piraino@unile.it; shkubota@medusanpolyp.mbox.media.kyoto.u.ac.jp; peter.schuchert@mhn.ville-ge.ch RI Piraino, Stefano/J-5234-2012 OI Piraino, Stefano/0000-0002-8752-9390 NR 55 TC 28 Z9 35 U1 12 U2 108 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 FEB PY 2007 VL 45 IS 1 BP 11 EP 19 DI 10.1111/j.1439-0469.2006.00379.x PG 9 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 130HZ UT WOS:000243792000002 ER PT J AU Blakie, PB Rey, AM Bezett, A AF Blakie, P. B. Rey, A. -M. Bezett, A. TI Thermodynamics of quantum degenerate gases in optical lattices SO LASER PHYSICS LA English DT Article ID BOSE-EINSTEIN CONDENSATE; ULTRACOLD ATOMS; STATES; PHASE AB The entropy-temperature curves are calculated for noninteracting Bose and Fermi gases in a 3D optical lattice. These curves facilitate understanding of how adiabatic changes in the lattice depth affect the temperature, and we demonstrate regimes where the atomic sample can be significantly heated or cooled by the loading process. We assess the effects of interactions on a Bose gas in a deep optical lattice and show that interactions ultimately limit the extent of cooling that can occur during lattic loading. C1 Univ Otago, Dept Phys, Jack Dodd Ctr Photon & Ultra Cold Atoms, Dunedin, New Zealand. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Blakie, PB (reprint author), Univ Otago, Dept Phys, Jack Dodd Ctr Photon & Ultra Cold Atoms, Dunedin, New Zealand. EM bblakie@physics.otago.ac.nz RI Blakie, Peter/A-1554-2009 OI Blakie, Peter/0000-0003-4772-6514 NR 22 TC 6 Z9 6 U1 1 U2 3 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1054-660X J9 LASER PHYS JI Laser Phys. PD FEB PY 2007 VL 17 IS 2 BP 198 EP 204 DI 10.1134/S1054660X07020259 PG 7 WC Optics; Physics, Applied SC Optics; Physics GA 137OA UT WOS:000244300700025 ER PT J AU Sunshine, JM Bus, SJ Corrigan, CM Mccoy, TJ Burbine, TH AF Sunshine, Jessica M. Bus, Schelte J. Corrigan, Catherine M. McCoy, Timothy J. Burbine, Thomas H. TI Olivine-dominated asteroids and meteorites: Distinguishing nebular and igneous histories SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SPECTROSCOPIC SURVEY; REFLECTANCE SPECTRA; PYROXENE MIXTURES; PHASE-II; TEMPERATURE; CHEMISTRY; CHONDRITES; MINERALOGY; TAXONOMY; SAMPLES AB Melting models indicate that the composition and abundance of olivine systematically co-vary and are therefore excellent petrologic indicators. However, heliocentric distance, and thus surface temperature, has a significant effect on the spectra of olivine-rich asteroids. We show that composition and temperature complexly interact spectrally, and must be simultaneously taken into account in order to infer olivine composition accurately. We find that most (7/9) of the olivinedominated asteroids are magnesian and thus likely sampled mantles differentiated from ordinary chondrite sources (e.g., pallasites). However, two other olivine-rich asteroids (289 Nenetta and 246 Asporina) are found to be more ferroan. Melting models show that partial melting cannot produce olivine-rich residues that are more ferroan than the chondrite precursor from which they formed. Thus, even moderately ferroan olivine must have non-ordinary chondrite origins, and therefore likely originate from oxidized R chondrites or melts thereof, which reflect variations in nebular composition within the asteroid belt. This is consistent with the meteoritic record in which R chondrites and brachinites are rare relative to pallasites. C1 Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Hawaii, Astron Inst, Hilo, HI 96720 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. RP Sunshine, JM (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM jess@astro.umd.edu NR 65 TC 29 Z9 29 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD FEB PY 2007 VL 42 IS 2 BP 155 EP 170 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 134TH UT WOS:000244106500001 ER PT J AU Barros, SCC Marsh, TR Dhillon, VS Groot, PJ Littlefair, S Nelemans, G Roelofs, G Steeghs, D Wheatley, PJ AF Barros, S. C. C. Marsh, T. R. Dhillon, V. S. Groot, P. J. Littlefair, S. Nelemans, G. Roelofs, G. Steeghs, D. Wheatley, P. J. TI ULTRACAM photometry of the ultracompact binaries V407 Vul and HM Cnc SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrometry; binaries : close; stars : individual : V407 Vul; stars : individual : HM Cnc; stars : magnetic fields; white dwarfs; X-rays : stars ID DOUBLE WHITE-DWARFS; SHORTEST PERIOD BINARY; RX J0806.3+1527; SPIN-UP; GRAVITATIONAL-RADIATION; CHANDRA OBSERVATIONS; INTERMEDIATE POLARS; MASS-TRANSFER; TIME-SERIES; SPACED DATA AB V407 Vul (RXJ1914.4+2456) and HM Cnc (RXJ0806.3+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 are thought possibly to represent the orbital periods of close pairs of white dwarfs. In this paper we present optical light curves taken with the high-speed CCD camera ULTRACAM on the 4.2-m William Hershel Telescope in 2003 May and 2005 August and with the VLT in 2005 November. The optical and X-ray light curves of HM Cnc have been reported as being in antiphase, but we find that in fact the X-rays peak around 0.2 cycles after the maximum of the optical light, as seen also in V407 Vul. The X-ray/optical phase shifts are well explained under the accreting models of the systems if most of the optical modulation comes from the heated faces of the mass donors and if the X-ray emitting spots are positioned in advance of the mass donors, as is expected given the angular momentum of the accreting material. Some optical emission may also come from the vicinity of the X-ray spot, and we further show that this can explain the non-sinusoidal light curves of HM Cnc. On the basis of this model we constrain the temperature of the heated face of the companion star finding a bolometric luminosity > 10(33) erg s(-1) and a distance, d > 1.1 kpc. We can identify no explanation for the X-ray/optical phase shifts under the intermediate polar and unipolar inductor models of the systems. The only significant difference between the two stars is that V407 Vul is observed to have the spectrum of a G star. The variation in position on the sky of a blend of a variable and a constant star can be used as a measure of their separation, and is sensitive to values well below the limit set by seeing. We apply this 'pulsation astrometry' to deduce that the G star is separated from the variable by about 0.027 arcsec and hence plays no role in the variability of V407 Vul. We show that light traveltime variations could influence the period change in V407 Vul if it forms a triple system with the G star. C1 Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. 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; 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; Littlefair, Stuart/0000-0001-7221-855X; Wheatley, Peter/0000-0003-1452-2240 NR 44 TC 17 Z9 17 U1 0 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 1 PY 2007 VL 374 IS 4 BP 1334 EP 1346 DI 10.1111/j.1365-2966.2006.11244.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 128DB UT WOS:000243636300014 ER PT J AU Hossain, S Tayal, SS Smith, SJ Raymond, JC Chutjian, A AF Hossain, S. Tayal, S. S. Smith, S. J. Raymond, J. C. Chutjian, A. TI Measurement and calculation of absolute cross sections for excitation of the 3s(2)3p P-2(1/2)o-3s(2)3p P-2(3/2)o fine-structure transition in Fe13+ SO PHYSICAL REVIEW A LA English DT Article ID ELECTRON-EXCITATION; SEYFERT-GALAXIES; CORONAL LINE; FE-XIV; IRON; PROGRAM; REGION AB Experimental cross sections are reported for the Fe13+ coronal green line transition 3s(2)3p P-2(1/2)o-3s(2)3p P-2(3/2)o at lambda 5303 A (2.338 eV). The center-of-mass interaction energies are in the range 1.7 eV (below threshold) through threshold, to 6.6 eV (2.9xthreshold). Data are compared with results of a 135-level Breit-Pauli R-matrix theory. Present experiment detects a strong maximum in the excitation cross section of magnitude 15x10(-16) cm(2) at 2.6 eV. Smaller structures are observed between 3 eV and 6.6 eV, with a maximum cross section never exceeding about 1.2x10(-16) cm(2). All features are due to enhancement of the direct excitation via a multitude of narrow, closely-spaced resonances calculated by the theory, the effects of which are convoluted by the 125 meV energy resolution of the present experiment. Iron is present in practically every astrophysical object, as well as being an impurity in fusion plasmas. Present results are the highest charge state in any ion for which an absolute excitation cross section has been measured. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Clark Atlanta Univ, Dept Phys, Atlanta, GA 30314 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hossain, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 23 TC 9 Z9 9 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 FEB PY 2007 VL 75 IS 2 AR 022709 DI 10.1103/PhysRevA.75.022709 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 140UN UT WOS:000244532300077 ER PT J AU Small, LM AF Small, Lawrence M. TI From the secretary - Out of Africa ('African Vision', Walt Disney-Tishman African Art Collection) SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD FEB PY 2007 VL 37 IS 11 BP 32 EP 32 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 129EA UT WOS:000243710000020 ER PT J AU Niven, JE AF Niven, Jeremy E. TI Brains, islands and evolution: breaking all the rules SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID HOMO-FLORESIENSIS; SAPIENS AB The announcement in 2004 that a small-brained hominin, Homo floresiensis, had been discovered on the island of Flores, Indonesia, was hailed as a major scientific breakthrough because it challenged preconceptions about the evolution of our closest relatives. Now, just over two years later, questions raised by the interpretation of the fossil abound. In a series of recent papers, critics have questioned the interpretation of the small brain volume of the fossil as that of a new hominin species, suggesting instead that it was due to microcephaly. The arguments raised by critics and advocates alike prompt a re-examination of ideas about what is possible during the evolution of the brain. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Niven, JE (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM nivenj@si.edu RI Niven, Jeremy/A-5883-2011 NR 17 TC 31 Z9 33 U1 1 U2 22 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 FEB PY 2007 VL 22 IS 2 BP 57 EP 59 DI 10.1016/j.tree.2006.11.009 PG 3 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 135QX UT WOS:000244169200001 PM 17157407 ER PT J AU Laurance, WF AF Laurance, William F. TI Have we overstated the tropical biodiversity crisis? SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID AMAZONIAN FOREST FRAGMENTS; DEFORESTATION RATES; EXTINCTION; FUTURE; HOTSPOTS; COVER; REGION AB Tropical forests are the most biologically diverse and ecologically complex of terrestrial ecosystems, and are disappearing at alarming rates. It has long been suggested that rapid forest loss and degradation in the tropics, if unabated, could ultimately precipitate a wave of species extinctions, perhaps comparable to mass extinction events in the geological history of the Earth. However, a vigorous debate has erupted following a study by Wright and Muller-Landau that challenges the notion of large-scale tropical extinctions, at least over the next century. Here, I summarize this controversy and describe how the debate is stimulating a serious examination of the causes and biological consequences of future tropical deforestation. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@si.edu RI Laurance, William/B-2709-2012 NR 58 TC 125 Z9 134 U1 13 U2 98 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 FEB PY 2007 VL 22 IS 2 BP 65 EP 70 DI 10.1016/j.tree.2006.09.014 PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 135QX UT WOS:000244169200002 PM 17011069 ER PT J AU Craven, D Braden, D Ashton, MS Berlyn, GP Wishnie, M Dent, D AF Craven, D. Braden, D. Ashton, M. S. Berlyn, G. P. Wishnie, M. Dent, D. TI Between and within-site comparisons of structural and physiological characteristics and foliar nutrient content of 14 tree species at a wet, fertile site and a dry, infertile site in Panama SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE environmental gradient; native tree species; Tectona grandis; Cedrela odorata; neotropics; reforestation ID TROPICAL FOREST; RAIN-FOREST; SOIL FERTILITY; COSTA-RICA; GROWTH; PLANTATIONS; ECOLOGY; RESTORATION; LANDS AB Structural and physiological characteristics and foliar nutrient content of 14 tree species were evaluated at two sites, one being seasonally wet with relatively fertile soils and the other being seasonally dry with relatively infertile soils. Differences in environmental stress between these sites drove the resulting differences in structural and physiological characteristics and leaf nutrient content of the investigated tree species. At the wet site, trees were more productive as site conditions allowed for greater photosynthetic activity to occur. The growth of pioneer tree species such as Spondias mombin, Guazuma ulmifolia, and Luehea seemanni, correlated strongly with high water-use efficiency and large, low-density leaves. Tree species, especially N-fixing species such as Albizia adinocephala, Albizia guachapele, Enterolobium cyclocarpum, and Gliricidia sepium, adapted to the greater levels of environmental stress at the dry site with infertile soils by increasing their water-use efficiency. Species differences were also significant, indicating that certain species adapted physiologically and structurally to environmental stress. Tree productivity operated under different structural and physiological constraints at each site. Leaf mass area (LMA), foliar N, and leaf area index (LAI) best predicted mass-based net photosynthetic capacity at the more fertile, wet site while foliar N was the best predictor of mass-based net photosynthetic capacity at the less fertile, dry site. Results from this study suggest the use of pioneer species at wet, fertile sites and N-fixing species at dry, infertile sites for restoration projects. (c) 2006 Elsevier B.V. All rights reserved. C1 Smithsonian Trop Res Inst, Unit 0948, Ctr Trop Forest Sci, PRP RENA,Nativ Species Reforestat Project, Miami, FL 34002 USA. Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Craven, D (reprint author), Smithsonian Trop Res Inst, Unit 0948, Ctr Trop Forest Sci, PRP RENA,Nativ Species Reforestat Project, APO,AA, Miami, FL 34002 USA. EM dylan.craven@aya.yale.edu RI Craven, Dylan/K-2717-2012; Dent, Daisy/L-3549-2016 OI Craven, Dylan/0000-0003-3940-833X; Dent, Daisy/0000-0002-1219-7344 NR 45 TC 19 Z9 19 U1 1 U2 21 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD JAN 30 PY 2007 VL 238 IS 1-3 BP 335 EP 346 DI 10.1016/j.foreco.2006.10.030 PG 12 WC Forestry SC Forestry GA 129WV UT WOS:000243761700031 ER PT J AU Smith, RK Bautz, MW Edgar, RJ Fujimoto, R Hamaguchi, K Hughes, JR Ishida, M Kelley, R Kilbourne, CA Kuntz, KD McCammon, D Miller, E Mitsuda, K Mukai, K Plucinsky, PP Porter, FS Snowden, SL Takei, Y Terada, Y Tsuboi, Y Yamasaki, NY AF Smith, Randall K. Bautz, Mark W. Edgar, Richard J. Fujimoto, Ryuichi Hamaguchi, Kenji Hughes, John R. Ishida, Manabu Kelley, Richard Kilbourne, Caroline A. Kuntz, K. D. McCammon, Dan Miller, Eric Mitsuda, Kazuhisa Mukai, Koji Plucinsky, Paul P. Porter, F. Scott Snowden, Steve L. Takei, Yoh Terada, Yukikatsu Tsuboi, Yohko Yamasaki, Noriko Y. TI Suzaku observations of the local and distant hot ISM SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE ISM : bubbles; plasmas; X-rays : ISM ID INTERSTELLAR-MEDIUM; RAY; EMISSION; SPECTRUM; CHANDRA; PLASMA; BUBBLE; HALO; SKY AB Suzaku observed the molecular cloud MBM 12 and a blank field less than 3 degrees away to separate the local and distant components of the diffuse soft X-ray background. Towards MBM 12, a local (D less than or similar to 275 pc) O VII emission line was clearly detected with an intensity of 3.5 photons cm(-2) s(-1) sr(-1) (or line units, LU), and the O VIII flux was < 0.34 LU. The origin of this O VII emission could be hot gas in the Local Hot Bubble (LHB), charge exchange within the heliosphere with oxygen ions from the solar wind (SWCX), or both. If entirely from the LHB, the emission could be explained by a region with emission measure of 0.0075 cm(-6) pc and a temperature of 1.2 x 10(6) K. However, this temperature and emission measure implies 1/4 keV emission in excess of observations. There is no evidence in the X-ray light curve or solar wind data for a significant contribution from geocoronal SWCX, although interplanetary SWCX is still possible. In any case, the observed O VII flux represents an upper limit to both the LHB emission and interplanetary SWCX in this direction. The blank field was observed immediately afterwards. The net off-cloud O VII and O VIII intensities were (respectively) 2.34 +/- 0.33 and 0.77 +/- 0.16 LU, after subtracting the on-cloud foreground emission. If this more distant O VII and O VIII emission is from a thermal plasma in collisional equilibrium beyond the Galactic disk, we infer it has a temperature of (2.1 +/- 0.1) x 10(6) K with an emission measure of (4 +/- 0.6) x 10(-3) cm(-6) pc. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, Cambridge, MA 02138 USA. Rutgers State Univ, Piscataway, NJ 08854 USA. Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan. Japan Aerosp Explorat Agcy, JAXA, ISAS, Dept High Energy Astrophys, Sagamihara, Kanagawa 2298510, Japan. RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. Chuo Univ, Fac Sci & Engn, Dept Phys, Bunkyo Ku, Tokyo 1128551, Japan. RP Smith, RK (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM rsmith@milkyway.gsfc.nasa.gov RI Yamasaki, Noriko/C-2252-2008; Mitsuda, Kazuhisa/C-2649-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012; Terada, Yukikatsu/A-5879-2013; XRAY, SUZAKU/A-1808-2009 OI Porter, Frederick/0000-0002-6374-1119; Terada, Yukikatsu/0000-0002-2359-1857; NR 35 TC 70 Z9 70 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD JAN 30 PY 2007 VL 59 SI 1 BP S141 EP S150 DI 10.1093/pasj/59.sp1.S141 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139ON UT WOS:000244441700009 ER PT J AU Rahbek, C Gotelli, NJ Colwell, RK Entsminger, GL Rangel, TFLVB Graves, GR AF Rahbek, Carsten Gotelli, Nicholas J. Colwell, Robert K. Entsminger, Gary L. Rangel, Thiago Fernando L. V. B. Graves, Gary R. TI Predicting continental-scale patterns of bird species richness with spatially explicit models SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE diversity gradients; South American avifauna; climate-based models; species richness patterns; mid-domain effect; spatially explicit stochastic models ID GEOGRAPHIC RANGE SIZE; GEOMETRIC CONSTRAINTS; AUTOREGRESSIVE MODELS; SOUTH-AMERICA; FOREST BIRDS; ECOLOGY; BIODIVERSITY; DIVERSITY; AUTOCORRELATION; SPECIATION AB The causes of global variation in species richness have been debated for nearly two centuries with no clear resolution in sight. Competing hypotheses have typically been evaluated with correlative models that do not explicitly incorporate the mechanisms responsible for biotic diversity gradients. Here, we employ a fundamentally different approach that uses spatially explicit Monte Carlo models of the placement of cohesive geographical ranges in an environmentally heterogeneous landscape. These models predict species richness of endemic South American birds ( 2248 species) measured at a continental scale. We demonstrate that the principal single-factor and composite ( species-energy, water-energy and temperature-kinetics) models proposed thus far fail to predict ( r(2) <= 0.05) the richness of species with small to moderately large geographical ranges ( first three range-size quartiles). These species constitute the bulk of the avifauna and are primary targets for conservation. Climate-driven models performed reasonably well only for species with the largest geographical ranges ( fourth quartile) when range cohesion was enforced. Our analyses suggest that present models inadequately explain the extraordinary diversity of avian species in the montane tropics, the most species-rich region on Earth. Our findings imply that correlative climatic models substantially underestimate the importance of historical factors and small-scale niche-driven assembly processes in shaping contemporary species-richness patterns. C1 Univ Copenhagen, Inst Biol, Ctr Macroecol, DK-2100 Copenhagen O, Denmark. Univ Vermont, Dept Biol, Burlington, VT 05405 USA. Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. Acquired Intelligence Inc, Rocky Mt Biol Labs, Montrose, CO 81401 USA. Univ Fed Goias, ICB, Dept Biol Geral, Grad Program Ecol & Evolut, BR-74001970 Goiania, Go, Brazil. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Rahbek, C (reprint author), Univ Copenhagen, Inst Biol, Ctr Macroecol, Univ Parken 15, DK-2100 Copenhagen O, Denmark. EM crahbek@bi.ku.dk; ngotelli@uvm.edu RI Rangel, Thiago/H-8708-2012; Rahbek, Carsten/D-9372-2013; Rahbek, Carsten/L-1129-2013; Colwell, Robert/C-7276-2015; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 NR 53 TC 168 Z9 179 U1 7 U2 71 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD JAN 22 PY 2007 VL 274 IS 1607 BP 165 EP 174 DI 10.1098/rspb.2006.3700 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 115WV UT WOS:000242765400002 PM 17148246 ER PT J AU Vigelius, M Melatos, A Chatterjee, S Gaensler, BM Ghavamian, P AF Vigelius, M. Melatos, A. Chatterjee, S. Gaensler, B. M. Ghavamian, P. TI Three-dimensional hydrodynamic simulations of asymmetric pulsar wind bow shocks SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; shock waves; pulsars : general; stars : winds, outflows ID RELATIVISTIC MHD SIMULATIONS; LOW-DENSITY PLASMA; CRAB-NEBULA; NEUTRON-STAR; SUPERNOVA-REMNANTS; OPTICAL-EMISSION; GUITAR NEBULA; JET; DISCOVERY; DYNAMICS AB We present three-dimensional, non-relativistic, hydrodynamic simulations of bow shocks in pulsar wind nebulae. The simulations are performed for a range of initial and boundary conditions to quantify the degree of asymmetry produced by latitudinal variations in the momentum flux of the pulsar wind, radiative cooling in the post-shock flow and density gradients in the interstellar medium (ISM). We find that the bow shock is stable even when travelling through a strong ISM gradient. We demonstrate how the shape of the bow shock changes when the pulsar encounters density variations in the ISM. We show that a density wall can account for the peculiar bow shock shapes of the nebulae around PSR J2124-3358 and PSR B0740-28. A wall produces kinks in the shock, whereas a smooth ISM density gradient tilts the shock. We conclude that the anisotropy of the wind momentum flux alone cannot explain the observed bow shock morphologies but it is instead necessary to take into account external effects. We show that the analytic (single layer, thin shell) solution is a good approximation when the momentum flux is anisotropic, fails for a steep ISM density gradient and approaches the numerical solution for efficient cooling. We provide analytic expressions for the latitudinal dependence of a vacuum-dipole wind and the associated shock shape, and compare the results to a split-monopole wind. We find that we are unable to distinguish between these two wind models purely from the bow shock morphology. C1 Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Vigelius, M (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. EM mvigeliu@physics.unimelb.edu.au RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 53 TC 26 Z9 26 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 21 PY 2007 VL 374 IS 3 BP 793 EP 808 DI 10.1111/j.1365-2966.2006.11193.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124XI UT WOS:000243405300004 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, J. Stuart B. Loeb, Abraham TI Smooth boundaries to cosmological HII regions from galaxy clustering SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : high-redshift; quasars : general; cosmology : theory ID REIONIZATION; REDSHIFT; UNIVERSE; QUASARS; HISTORY; MASS AB The H II regions around quasars and galaxies at redshifts beyond the epoch of reionization will provide prime targets for upcoming 21-cm campaigns using a new generation of low-frequency radio observatories. Here we show that the boundaries of these H II regions will not be sharp. Rather, the clustering of sources near massive galaxies results in a neutral fraction that rises gradually towards large radii from an interior value near zero. A neutral fraction corresponding to the global background value is typically reached at a distance of 2-5 times the radius of the H II region around the central massive galaxy. C1 Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyithe, JSB (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. EM swyithe@physics.unimelb.edu.au; loeb@cfa.harvard.edu OI Wyithe, Stuart/0000-0001-7956-9758 NR 19 TC 10 Z9 10 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 21 PY 2007 VL 374 IS 3 BP 960 EP 964 DI 10.1111/j.1365-2966.2006.11201.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124XI UT WOS:000243405300017 ER PT J AU Jonker, PG Nelemans, G Bassa, CG AF Jonker, P. G. Nelemans, G. Bassa, C. G. TI Detection of the radial velocity curve of the B5-A0 supergiant companion star of Cir X-1 ? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars : individual : Cir X-1; stars : neutron; X-rays : binaries ID X-RAY BINARIES; ACCRETING NEUTRON-STARS; CIRCINUS X-1; LOW-MASS; OPTICAL-SPECTRA; ZERO PHASE; ANGSTROM; SPECTROSCOPY; VARIABILITY; POPULATION AB In this paper, we report on phase-resolved I-band optical spectroscopic and photometric observations of Cir X-1 obtained with the Very Large Telescope. The spectra are dominated by Paschen absorption lines at nearly all orbital phases except near phase zero (coinciding with the X-ray dip) when the absorption lines are filled in by broad Paschen emission lines. The radial velocity curve of the absorption lines corresponds to an eccentric orbit (e = 0.45) whose period and time of periastron passage are consistent with the period and phase predicted by the most recent X-ray dip ephemeris. We found that the I-band magnitude decreases from 17.6 to similar to 16.8 near phase 0.9-1.0; this brightening coincides in phase with the X-ray dip. Even though it is likely that the absorption-line spectrum is associated with the companion star of Cir X-1, we cannot exclude the possibility that the spectrum originates in the accretion disc. However, if the spectrum belongs to the companion star, it must be a supergiant of spectral type B5-A0. If we assume that the compact object does not move through the companion star at periastron, the companion star mass is constrained to less than or similar to 10 M-circle dot for a 1.4-M-circle dot neutron star, whereas the inclination has to be greater than or similar to 13 degrees 7. Alternatively, the measured absorption lines and their radial velocity curve can be associated with the accretion disc surrounding a 1.4-M-circle dot neutron star and its motion around the centre of mass. An absorption-line spectrum from an accretion disc is typically found when our line of sight passes through the accretion disc rim implying a high inclination. In this scenario, the companion star mass is found to be similar to 0.4 M-circle dot. However, from radio observations it was found that the angle between the line of sight and the jet axis is smaller than 5 degrees. This would mean that the jet ploughs through the accretion disc in this scenario, making this solution less probable. C1 SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 ED Nijmegen, Netherlands. RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 NR 46 TC 33 Z9 33 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 21 PY 2007 VL 374 IS 3 BP 999 EP 1005 DI 10.1111/j.1365-2966.2006.11210.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124XI UT WOS:000243405300020 ER PT J AU Nagai, D Vikhlinin, A Kravtsov, AV AF Nagai, Daisuke Vikhlinin, Alexey Kravtsov, Andrey V. TI Testing X-ray measurements of galaxy clusters with cosmological simulations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation; methods : numerical ID MASS-TEMPERATURE RELATION; INTRACLUSTER MEDIUM; VISCOUS DISSIPATION; CHANDRA SAMPLE; DARK-MATTER; GAS; PROFILES; SPECTRA; TURBULENCE; VISCOSITY AB X-ray observations of galaxy clusters potentially provide powerful cosmological probes if systematics due to our incomplete knowledge of the ICM physics is understood and controlled. In this paper we present mock Chandra analyses of cosmological cluster simulations and assess X-ray measurements of galaxy cluster properties using a model and procedure essentially identical to that used in real data analysis. We show that reconstruction of three-dimensional ICM density and temperature profiles is excellent for relaxed clusters, but still reasonably accurate for unrelaxed systems. The total ICM mass is measured quite accurately (less than or similar to 6%) in all clusters, while the hydrostatic estimate of the gravitationally bound mass is biased low by about 5% -20% through the virial region, primarily due to additional pressure support provided by subsonic bulk motions in the ICM, ubiquitous in our simulations even in relaxed systems. Gas fraction determinations are therefore biased high; the bias increases toward cluster outskirts and depends sensitively on its dynamical state, but we do not observe significant trends of the bias with cluster mass or redshift. We also find that different average ICM temperatures, such as the X-ray spectroscopic T(spec) and gas-mass-weighted T(mg), are related to each other by a constant factor with a relatively small object-to-object scatter and no systematic trend with mass, redshift, or the dynamical state of clusters. We briefly discuss direct applications of our results for different cluster-based cosmological tests. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Inst, Moscow, Russia. Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Nagai, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM daisuke@caltech.edu NR 50 TC 297 Z9 297 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP 98 EP 108 DI 10.1086/509868 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400009 ER PT J AU Whittet, DCB Shenoy, SS Bergin, EA Chiar, JE Gerakines, PA Gibb, EL Melnick, GJ Neufeld, DA AF Whittet, D. C. B. Shenoy, S. S. Bergin, E. A. Chiar, J. E. Gerakines, P. A. Gibb, E. L. Melnick, G. J. Neufeld, D. A. TI The abundance of carbon dioxide ice in the quiescent intracloud medium SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : abundances; ISM : individual (Taurus dark cloud); infrared : ISM : lines and bands; ISM : molecules ID SPITZER-SPACE-TELESCOPE; TAURUS DARK CLOUD; INFRARED SPECTROGRAPH IRS; SERPENS MOLECULAR CLOUD; GAS-GRAIN CHEMISTRY; RHO-OPHIUCHI CLOUD; INTERSTELLAR-MEDIUM; HIGH-RESOLUTION; CO2 ICE; DUST AB We present new observations with the Infrared Spectrograph on board the Spitzer Space Telescope of the solid-CO2 absorption feature near 15 mu m in the spectra of eight field stars behind the Taurus complex of dark clouds. Solid CO2 is detected in six lines of sight. New results are combined with previous data to investigate the correlation of CO2 column density with those of other major ice constituents ( H2O and CO) and with extinction. CO2 is shown to display a "threshold extinction'' effect, i. e., a minimumextinction ( A(0)=4.3 +/- 1.0 mag) required for detection, behavior similar to that previously reported for H2O and CO. We find a particularly tight correlation through the origin between N( CO2) and N( H2O), confirming that these species form in tandem and coexist in the same ( polar) ice layer on the grains. The observed composition of the mantles is broadly consistent with the predictions of photochemical models with diffusive surface chemistry proposed by Ruffle & Herbst. Comparison of our results for Taurus with published data for Serpens indicates significant differences in ice composition consistent with enhanced CO2 production in the latter cloud. Our results also place constraints on the distribution of elemental oxygen between ices and other potential reservoirs. Assuming a constant N( H) to extinction ratio, we show that similar to 65% of the solar O abundance is accounted for by summing the contributions of ices (similar to 26%), refractory dust (similar to 30%) and gas- phase CO (similar to 9%). If the Sun is an appropriate standard for the interstellar medium, the " missing'' oxygen may reside in atomic O i gas and/ or ( undetected) O-2 within the ices. C1 Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. SETI Inst, Mountain View, CA USA. Univ Alabama, Dept Phys, Birmingham, AL 35233 USA. Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Whittet, DCB (reprint author), Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. 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 67 TC 89 Z9 89 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 JAN 20 PY 2007 VL 655 IS 1 BP 332 EP 341 DI 10.1086/509772 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400024 ER PT J AU Brooke, TY Huard, TL Bourke, TL Boogert, ACA Allen, LE Blake, GA Evans, NJ Harvey, PM Koerner, DW Mundy, LG Myers, PC Padgett, DL Sargent, AI Stapelfeldt, KR van Dishoeck, EF Chapman, N Cieza, L Dunham, MM Lai, SP Porras, A Spiesman, W Teuben, PJ Young, CH Wahhaj, Z Lee, CW AF Brooke, Timothy Y. Huard, Tracy L. Bourke, Tyler L. Boogert, A. C. Adwin Allen, Lori E. Blake, Geoffrey A. Evans, Neal J., II Harvey, Paul M. Koerner, David W. Mundy, Lee G. Myers, Philip C. Padgett, Deborah L. Sargent, Anneila I. Stapelfeldt, Karl R. van Dishoeck, Ewine F. Chapman, Nicholas Cieza, Lucas Dunham, Michael M. Lai, Shih-Ping Porras, Alicia Spiesman, William Teuben, Peter J. Young, Chadwick H. Wahhaj, Zahed Lee, Chang Won TI The Spitzer c2d survey of nearby dense cores. IV. Revealing the embedded cluster in B59 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : ISM; infrared : stars; ISM : clouds; stars : pre-main sequence ID MAIN-SEQUENCE STARS; YOUNG STELLAR POPULATION; AURIGA MOLECULAR CLOUD; SPACE-TELESCOPE; DARK CLOUD; INTERSTELLAR EXTINCTION; SOURCE COUNTS; PIPE NEBULA; EVOLUTION; OPHIUCHI AB Infrared images of the dark cloud core B59 were obtained with the Spitzer Space Telescope as part of the "Cores to Disks'' Legacy Science project. Photometry from 3.6Y70 mu m indicates at least 20 candidate low-mass young stars near the core, more than doubling the previously known population. Out of this group, 13 are located within similar to 0.1 pc in projection of the molecular gas peak, where a new embedded source is detected. Spectral energy distributions span the range from small excesses above photospheric levels to rising in the mid-infrared. One other embedded object, probably associated with the millimeter source B59-MMS1, with a bolometric luminosity L-bol similar to 2L(circle dot), has extended structure at 3.6 and 4.5 mu m, possibly tracing the edges of an outflow cavity. The measured extinction through the central part of the core is A(V) greater than or similar to 45 mag. The B59 core is producing young stars with a high efficiency. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. Smithsonian Astrophys Observ, Cambridge, MA USA. NOAO Gemini Sci Ctr, La Serena, Chile. CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Leiden Univ, Leiden, Netherlands. Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70310 USA. Korea Astron & Space Sci Inst, Taejon, South Korea. RP Brooke, TY (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA. EM tyb@astro.caltech.edu RI Stapelfeldt, Karl/D-2721-2012 NR 66 TC 43 Z9 43 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP 364 EP 374 DI 10.1086/510115 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400028 ER PT J AU Horan, D Atkins, RW Badran, HM Blaylock, G Bradbury, SM Buckley, JH Byrum, KL Celik, O Chow, YCK Cogan, P Cui, W Daniel, MK Perez, ID Dowdall, C Falcone, AD Fegan, DJ Fegan, SJ Finley, JP Fortin, P Fortson, LF Gillanders, GH Grube, J Gutierrez, KJ Hall, J Hanna, D Holder, J Hughes, SB Humensky, TB Kenny, GE Kertzman, M Kieda, DB Kildea, J Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G Moriarty, P Nagal, T Ong, RA Perkins, JS Petry, D Quinn, J Quinn, M Ragan, K Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Steele, D Swordy, SP Toner, JA Valcarcel, L Vassiliev, VV Wagner, RG Wakely, SP Weekes, TC White, RJ Williams, DA AF Horan, D. Atkins, R. W. Badran, H. M. Blaylock, G. Bradbury, S. M. Buckley, J. H. Byrum, K. L. Celik, O. Chow, Y. C. K. Cogan, P. Cui, W. Daniel, M. K. Perez, I. de la Calle Dowdall, C. Falcone, A. D. Fegan, D. J. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. F. Gillanders, G. H. Grube, J. Gutierrez, K. J. Hall, J. Hanna, D. Holder, J. Hughes, S. B. Humensky, T. B. Kenny, G. E. Kertzman, M. Kieda, D. B. Kildea, J. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. Moriarty, P. Nagal, T. Ong, R. A. Perkins, J. S. Petry, D. Quinn, J. Quinn, M. Ragan, K. Reynolds, P. T. Rose, H. J. Schroedter, M. Sembroski, G. H. Steele, D. Swordy, S. P. Toner, J. A. Valcarcel, L. Vassiliev, V. V. Wagner, R. G. Wakely, S. P. Weekes, T. C. White, R. J. Williams, D. A. TI Very high energy observations of gamma-ray burst locations with the whipple telescope SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays : bursts; gamma rays : observations ID COMPTON EMISSION; REFRESHED SHOCKS; EXTERNAL MATTER; LIGHT-CURVE; AFTERGLOWS; TEV; MODELS; FLARES; DISCOVERY; SEARCH AB Gamma-ray burst (GRB) observations at very high energies (VHE; E > 100 GeV) can impose tight constraints on some GRB emission models. Many GRB afterglow models predict a VHE component similar to that seen in blazars and plerions, in which the GRB spectral energy distribution has a double-peaked shape extending into the VHE regime. VHE emission coincident with delayed X-ray flare emission has also been predicted. GRB follow-up observations have had high priority in the observing program at the Whipple 10 m gamma-ray telescope, and GRBs will continue to be high-priority targets as the next-generation observatory, VERITAS, comes online. Upper limits on the VHE emission at late times (> similar to 4 hr) from seven GRBs observed with the Whipple Telescope are reported here. C1 Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ USA. Univ Utah, Dept Phys, Salt Lake City, UT USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Argonne Natl Lab, Argonne, IL 60439 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. Univ Coll Dublin, Sch Phys, Dublin 2, Ireland. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Univ Oxford, Dept Phys, Oxford, England. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL USA. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. McGill Univ, Dept Phys, Montreal, PQ H3A 2T5, Canada. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA USA. Galway Mayo Inst Technol, Dept Phys & Life Sci, Galway, Ireland. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. RP Horan, D (reprint author), Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. RI Hall, Jeter/E-9294-2015; Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Lang, Mark/0000-0003-4641-4201 NR 110 TC 18 Z9 18 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP 396 EP 405 DI 10.1086/509567 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400031 ER PT J AU Besla, G Wu, YQ AF Besla, Gurtina Wu, Yanqin TI Formation of narrow dust rings in circumstellar debris disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; hydrodynamics; infrared : stars; instabilities ID MAIN-SEQUENCE STARS; BETA-PICTORIS DISK; VEGA-EXCESS STARS; HR 4796A; PLANETARY-SYSTEMS; EPSILON-ERIDANI; GAS TEMPERATURE; RADIATION PRESSURE; AU MICROSCOPII; EMISSION AB Narrow dust rings observed around some young stars (e.g., HR 4796A) need to be confined. We present a possible explanation for the formation and confinement of such rings in optically thin circumstellar disks, without invoking shepherding planets. If an enhancement of dust grains (e.g., due to a catastrophic collision) occurs somewhere in the disk, photoelectric emission from the grains can heat the gas to temperatures well above that of the dust. The gas orbits with super (sub)-Keplerian speeds inward (outward) of the associated pressure maximum. This tends to concentrate the grains into a narrow region. The rise in dust density leads to further heating and a stronger concentration of grains. A narrow dust ring forms as a result of this instability. We show that this mechanism not only operates around early-type stars that have high UV fluxes, but also around stars with spectral types as late as K. This implies that this process is generic and may have occurred during the lifetime of each circumstellar disk. We examine the stringent upper limit on the H(2) column density in the HR 4796A disk and find it to be compatible with the presence of a significant amount of hydrogen gas in the disk. We also compute the O I and C II infrared line fluxes expected from various debris disks and show that these will be easily detectable by the upcoming Herschel mission. Herschel will be instrumental in detecting and characterizing gas in these disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. RP Besla, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 83 TC 25 Z9 25 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP 528 EP 540 DI 10.1086/509495 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400042 ER PT J AU Gaudi, BS Winn, JN AF Gaudi, B. Scott Winn, Joshua N. TI Prospects for the characterization and confirmation of transiting exoplanets via the Rossiter-McLaughlin effect SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : rotation ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EXTRASOLAR PLANETARY SYSTEMS; DOPPLER FOLLOW-UP; DIFFERENTIAL ROTATION; GIANT PLANETS; HOT JUPITERS; GALACTIC BULGE; DYNAMICAL INSTABILITIES; SOLAR ROTATION AB The Rossiter-McLaughlin (RM) effect is the distortion of stellar spectral lines that occurs during eclipses or transits, due to stellar rotation. We assess the future prospects for using the RM effect to measure the alignment of planetary orbits with the spin axes of their parent stars, and to confirm exoplanetary transits. We compute the achievable accuracy for the parameters of interest, in general and for the five known cases of transiting exoplanets with bright host stars. We determine the requirements for detecting the effects of differential rotation. For transiting planets with small masses or long periods (as will be detected by forthcoming satellite missions), the velocity anomaly produced by the RM effect can be much larger than the orbital velocity of the star. For a terrestrial planet in the habitable zone of a Sunlike star found by the Kepler mission, it will be difficult to use the RM effect to confirm transits with current instruments, but it still may be easier than measuring the spectroscopic orbit. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. RP Gaudi, BS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sgaudi@cfa.harvard.edu; jwinn@mit.edu RI Gaudi, Bernard/I-7732-2012 NR 80 TC 150 Z9 150 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP 550 EP 563 DI 10.1086/509910 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400044 ER PT J AU Knutson, HA Charbonneau, D Noyes, RW Brown, TM Gilliland, RL AF Knutson, Heather A. Charbonneau, David Noyes, Robert W. Brown, Timothy M. Gilliland, Ronald L. TI Using stellar limb-darkening to refine the properties of HD 209458b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; planetary systems; stars : individual ( HD 209458); techniques : photometric ID EXTRASOLAR GIANT PLANET; TRANSITING PLANET; INFRARED OBSERVATIONS; TRANSMISSION SPECTRA; SECONDARY ECLIPSE; HOT JUPITERS; STAR; SPECTROSCOPY; PARAMETERS; PHOTOMETRY AB We use multiband photometry to refine estimates for the planetary radius and orbital inclination of the transiting planet system HD 209458. We gathered 1066 spectra over four distinct transits with the STIS spectrometer on the Hubble Space Telescope using two gratings with a resolution R = 1500 and a combined wavelength range of 290-1030 nm. We divide the spectra into 10 spectrophotometric bandpasses, five for each grating, of equal wavelength span within each grating, and fit a transit curve over all bandpasses simultaneously. In our fit we use theoretical values for the stellar limb-darkening to further constrain the planetary radius. We find that the radius of HD 209458b is (1.320 +/- 0.025) R-Jup, which is a factor of 2 more precise than current estimates. We also obtain improved estimates for the orbital period P and time of center of transit T-C. Although in principle the photon-limited precision of the STIS data should allow us to measure the timing of individual transits to a precision of 2-7 s, we find that uncertainties in the stellar limb-darkening coefficients and residual noise in the data degrade these measurements to a typical precision of +/- 14 s. Within this level of error, we find no significant variations in the timing of the eight events examined in this work. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Las Cumbres Observ, Goleta, CA USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Knutson, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hknutson@cfa.harvard.edu; dcharbonneau@cfa.harvard.edu; noyes@cfa.harvard.edu; tbrown@lcogt.net; gillil@stsci.edu OI Charbonneau, David/0000-0002-9003-484X NR 54 TC 170 Z9 169 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP 564 EP 575 DI 10.1086/510111 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400045 ER PT J AU Bemporad, A Raymond, J Poletto, G Romoli, M AF Bemporad, A. Raymond, J. Poletto, G. Romoli, M. TI Comprehensive study of the initiation and early evolution of a coronal mass ejection from ultraviolet and white-light data SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : UV radiation ID SOLAR CORONA; MAGNETIC RECONNECTION; CURRENT SHEET; SOHO OBSERVATIONS; UVCS-SOHO; CME; SPECTROMETER; RELAXATION; DENSITY; FIELDS AB In this work we analyze simultaneous UV and white-light (WL) observations of a slow CME that occurred on 2000 January 31. Unlike most CMEs studied in the UV so far, this event was not associated with a flare or filament eruption. Based on vector magnetograph data and magnetic field models, we find that field disruption in an active region (AR) was driven by flux emergence and shearing motions, leading to the CME and to post-CME arcades seen in the EUV. WL images, acquired by the Mark IV coronagraph at the Mauna Loa Observatory, allowed us to identify the CME front, bubble, and core shortly (about 1 hr) after the CME ejection. From polarized brightness (pB) Mauna Loa data we estimated the mass and electron densities of the CME. The CME mass increases with time, indicating that about 2/3 of the mass originates above 1.6 R circle dot. Analysis of the UV spectra, acquired by the Solar and Heliospheric Observatory Ultraviolet Coronagraph Spectrometer (SOHO UVCS) at 1.6 and 1.9 R circle dot, allowed us to derive the electron temperature distribution across the CME. The temperature maximizes at the CME core and increases between 1.6 and 1.9 R circle dot. This event was unusual, in that the leading edge and the CME core were hotter than the ambient corona. We discuss magnetic heating and adiabatic compression as explanations for the high temperatures in the core and leading edge, respectively. C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron & Sci Spazio, Florence, Italy. RP Bemporad, A (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. RI Romoli, Marco/H-6859-2012; OI Bemporad, Alessandro/0000-0001-5796-5653 NR 46 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP 576 EP 590 DI 10.1086/509569 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400046 ER PT J AU Riley, P Lionello, R Mikic, Z Linker, J Clark, E Lin, J Ko, YK AF Riley, Pete Lionello, Roberto Mikic, Zoran Linker, Jon Clark, Eric Lin, Jun Ko, Yuan-Kuen TI "Bursty'' reconnection following solar eruptions: MHD simulations and comparison with observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : corona; Sun : coronal mass ejections (CMEs); Sun : magnetic fields; solar wind ID CORONAL MASS EJECTIONS; MAGNETIC RECONNECTION; HELMET STREAMER; ARCADES; DISRUPTION; SHEET AB Posteruptive arcades are frequently seen in the aftermath of coronal mass ejections (CMEs). The formation of these loops at successively higher altitudes, coupled with the classic "two-ribbon'' flare seen in H alpha, are interpreted as reconnection of the coronal magnetic field that has been dragged outward by the CME. White-light observations of "rays,'' which have been interpreted as being coincident with the current sheet at the reconnection site underneath the erupting CME, also provide evidence for its occurrence. "Blobs'' occasionally seen within these rays suggest an even richer level of structure. In this report, we present numerical simulations that reproduce both the observed rays and the formation and evolution of the blobs. We compare their properties with SOHO/LASCO observations of similar structures, and relate their formation to standard theories of reconnection. C1 Sci Applicat Int Corp, San Diego, CA 92121 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Riley, P (reprint author), Sci Applicat Int Corp, San Diego, CA 92121 USA. EM pete.riley@saic.com; lionelr@saic.com; mikicz@saic.com; linkerj@saic.com; stephen.e.clark@saic.com; jlin@cfa.harvard.edu; yko@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 27 TC 38 Z9 44 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 JAN 20 PY 2007 VL 655 IS 1 BP 591 EP 597 DI 10.1086/509913 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400047 ER PT J AU Cirtain, JW Del Zanna, G DeLuca, EE Mason, HE Martens, PCH Schmelz, JT AF Cirtain, J. W. Del Zanna, G. DeLuca, E. E. Mason, H. E. Martens, P. C. H. Schmelz, J. T. TI Active region loops: Temperature measurements as a function of time from joint TRACE and SOHO CDS observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : UV radiation ID TRANSITION-REGION; CORONAL-EXPLORER; SOLAR CORONA; TELESCOPE; FILTER; SPECTROMETER; ATMOSPHERE; EIT AB In this paper, we aim to quantitatively investigate the structure and time variation of quiescent active region loop structures. We coordinated a joint program of observations (JOP 146) using TRACE, to obtain high-cadence EUV images, and SOHO CDS, to obtain spectroscopic data. Loop intensities are used to determine temperature as a function of time for a single loop, taking full account of the background emission. In many locations, the emission measure loci are consistent with an isothermal structure. However, the results indicate significant changes in the loop temperature (between 1 and 2 MK) over the 6 hr observing period. It is possible that the loop structures are composed of multiple, independently heated strands with sizes less than the resolution of the imager and spectrometer. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cirtain, JW (reprint author), UCL, Dept Space & Climate Phys, Mullard Space Sci Lab, Surrey, England. EM jcirtain@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 NR 25 TC 29 Z9 29 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 JAN 20 PY 2007 VL 655 IS 1 BP 598 EP 605 DI 10.1086/509769 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400048 ER PT J AU Su, YN Golub, L Van Ballegooijen, AA AF Su, Yingna Golub, Leon Van Ballegooijen, Adriaan A. TI A statistical study of shear motion of the footpoints in two-ribbon flares SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : flares; Sun : magnetic fields; Sun : UV radiation ID CORONAL MASS EJECTIONS; EMERGING MAGNETIC-FLUX; SOLAR-FLARES; RECONNECTION; MODEL; MORPHOLOGIES; PROMINENCES; ERUPTIONS; IMAGES; ROPE AB We present a statistical investigation of shear motion of the ultraviolet (UV) or extreme-ultraviolet (EUV) footpoints in two-ribbon flares, using the high spatial resolution data obtained in 1998-2005 by TRACE. To do this study, we have selected 50 well-observed X and M class two-ribbon flares as our sample. All 50 of these flares are classified into three types based on the motions of the footpoints with respect to the magnetic field (SOHO MDI). The relation between our classification scheme and the traditional classification scheme (i.e., "ejective'' and "confined'' flares) is discussed. We have found that 86% (43 out of 50) of these flares show both strong-to-weak shear change of footpoints and ribbon separation (type I flares), and 14% of the flares show no measurable shear change of conjugate footpoints, including two flares with very small ribbon separation (type II flares) and five flares having no ribbon separation at all through the entire flare process (type III flares). Shear motion of footpoints is thus a common feature in two-ribbon flares. A detailed analysis of the type I flares shows (1) for a subset of 20 flares, the initial and final shear angles of the footpoints are mainly in the range 50 degrees-80 degrees and 15 degrees-55 degrees, respectively; and (2) in 10 of the 14 flares having both measured shear angle and corresponding hard X-ray observations, the cessation of shear change is 0-2 minutes earlier than the end of the impulsive phase, which may suggest that the change from impulsive to gradual phase is related to magnetic shear change. C1 Purple Mt Observ, Nanjing, Peoples R China. RP Su, YN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ynsu@head.cfa.harvard.edu RI Su, Yingna/J-1674-2012; OI van Ballegooijen, Adriaan/0000-0002-5622-3540; Golub, Leon/0000-0001-9638-3082 NR 36 TC 36 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 JAN 20 PY 2007 VL 655 IS 1 BP 606 EP 614 DI 10.1086/510065 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JN UT WOS:000243725400049 ER PT J AU Gupta, H Brunken, S Tamassia, F Gottlieb, CA McCarthy, MC Thaddeus, P AF Gupta, H. Brunken, S. Tamassia, F. Gottlieb, C. A. McCarthy, M. C. Thaddeus, P. TI Rotational spectra of the carbon chain negative ions C4H- and C8H- SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; line : identification; molecular data; molecular processes; radio lines : ISM ID LINE SURVEY; LABORATORY DETECTION; RADICALS; TRANSITION; IRC+10216; CLUSTERS; ANIONS; C6H; GHZ; C3N AB The rotational spectra of the butadiyne anion C4H- and the octatetrayne anion C8H- have been detected in the laboratory. Precise spectroscopic constants for these closed-shell molecules have been obtained, which enable their rotational spectra to be calculated to high accuracy throughout the radio band. Deep astronomical searches can now be undertaken in essentially any molecular source, including TMC-1 and IRC + 10216, where the negative ion C6H- has recently been detected. The large dipole moments and high binding energies of both anions make them good candidates for astronomical detection. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Texas, Inst Theoret Chem, Dept Chem & Biochem, Austin, TX 78712 USA. Univ Bologna, Dipartimento Chim Fis & Inorgan, I-40136 Bologna, Italy. RP Gupta, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hgupta@cfa.harvard.edu; sbruenken@cfa.harvard.edu; tamassia@ms.fci.unibo.it; cgottlieb@cfa.harvard.edu; mccarthy@cfa.harvard.edu; pthaddeus@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010 OI Brunken, Sandra/0000-0001-7175-4828 NR 21 TC 62 Z9 63 U1 2 U2 9 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2007 VL 655 IS 1 BP L57 EP L60 DI 10.1086/511766 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129JO UT WOS:000243725500015 ER PT J AU Hu, RM Martin, RV Fairlie, TD AF Hu, R. -M. Martin, R. V. Fairlie, T. D. TI Global retrieval of columnar aerosol single scattering albedo from space-based observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RESOLUTION IMAGING SPECTRORADIOMETER; SEA-SALT AEROSOLS; OPTICAL-PROPERTIES; BLACK CARBON; TROPOSPHERIC AEROSOLS; SULFATE AEROSOLS; MODEL GOCART; ART.; CLIMATE; ABSORPTION AB We retrieve the global distribution of columnar single scattering albedo (omega(0)) by taking advantage of the high sensitivity of satellite measurements at ultraviolet channels by the Total Ozone Mapping Spectrometer (TOMS) to both aerosol optical depth and omega(0) and the high sensitivity of satellite measurements at visible channels by the Moderate Resolution Imaging Spectroradiometer (MODIS) to aerosol optical depth. A radiative transfer model (LIDORT) is used to calculate the local omega(0) that reproduces the TOMS aerosol index, when constrained by MODIS aerosol optical depth and by relative vertical profiles from a global chemical transport model (GEOS-CHEM). The simulated aerosol profiles are evaluated with lidar measurements of aerosol extinction. The retrieved omega(0) at 360 nm is near 1 over the remote ocean, in contrast with values of 0.75 to 0.9 over regions dominated by biomass burning and mineral dust aerosol. The retrieval uncertainty is 15%. We validate our retrieval with measurements from the Aerosol Robotic Network (AERONET); the correlation coefficient, slope, and intercept are 0.75, 0.99, and 0.02 respectively. C1 Dalhousie Univ, Dept Phys & Astmospher Sci, Halifax, NS, Canada. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. NASA Langley Res Ctr, Hampton, VA USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Engn, Cambridge, MA 02138 USA. RP Hu, RM (reprint author), Dalhousie Univ, Dept Phys & Astmospher Sci, Halifax, NS, Canada. EM hu@fizz.phys.dal.ca RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; NR 73 TC 14 Z9 15 U1 0 U2 4 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 JAN 20 PY 2007 VL 112 IS D2 AR D02204 DI 10.1029/2005JD006832 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 131DY UT WOS:000243849600001 ER PT J AU Hopfner, M von Clarmann, T Fischer, H Funke, B Glatthor, N Grabowski, U Kellmann, S Kiefer, M Linden, A Milz, M Steck, T Stiller, GP Bernath, P Blom, CE Blumenstock, T Boone, C Chance, K Coffey, MT Friedl-Vallon, F Griffith, D Hannigan, JW Hase, F Jones, N Jucks, KW Keim, C Kleinert, A Kouker, W Liu, GY Mahieu, E Mellqvist, J Mikuteit, S Notholt, J Oelhaf, H Piesch, C Reddmann, T Ruhnke, R Schneider, M Strandberg, A Toon, G Walker, KA Warneke, T Wetzel, G Wood, S Zander, R AF Hoepfner, M. von Clarmann, T. Fischer, H. Funke, B. Glatthor, N. Grabowski, U. Kellmann, S. Kiefer, M. Linden, A. Milz, M. Steck, T. Stiller, G. P. Bernath, P. Blom, C. E. Blumenstock, Th. Boone, C. Chance, K. Coffey, M. T. Friedl-Vallon, F. Griffith, D. Hannigan, J. W. Hase, F. Jones, N. Jucks, K. W. Keim, C. Kleinert, A. Kouker, W. Liu, G. Y. Mahieu, E. Mellqvist, J. Mikuteit, S. Notholt, J. Oelhaf, H. Piesch, C. Reddmann, T. Ruhnke, R. Schneider, M. Strandberg, A. Toon, G. Walker, K. A. Warneke, T. Wetzel, G. Wood, S. Zander, R. TI Validation of MIPAS ClONO2 measurements SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID LIMB EMISSION-SPECTRA; SOLAR OCCULTATION SPECTRA; CHLORINE NITRATE CLONO2; STRATOSPHERIC CHLORINE; MICHELSON INTERFEROMETER; REACTIVE NITROGEN; ANTARCTIC VORTEX; HIGH-RESOLUTION; APRIL 1993; Q-BRANCH AB Altitude profiles of ClONO2 retrieved with the IMK (Institut fur Meteorologie und Klimaforschung) science-oriented data processor from MIPAS/Envisat (Michelson Interferometer for Passive Atmospheric Sounding on Envisat) mid-infrared limb emission measurements between July 2002 and March 2004 have been validated by comparison with balloon-borne (Mark IV, FIRS2, MIPAS-B), airborne (MIPAS-STR), ground-based (Spitsbergen, Thule, Kiruna, Harestua, Jungfraujoch, Izana, Wollongong, Lauder), and spaceborne (ACE-FTS) observations. With few exceptions we found very good agreement between these instruments and MIPAS with no evidence for any bias in most cases and altitude regions. For balloon-borne measurements typical absolute mean differences are below 0.05 ppbv over the whole altitude range from 10 to 39 km. In case of ACE-FTS observations mean differences are below 0.03 ppbv for observations below 26 km. Above this altitude the comparison with ACE-FTS is affected by the photochemically induced diurnal variation of ClONO2. Correction for this by use of a chemical transport model led to an overcompensation of the photochemical effect by up to 0.1 ppbv at altitudes of 30-35 km in case of MIPAS-ACE-FTS comparisons while for the balloon-borne observations no such inconsistency has been detected. The comparison of MIPAS derived total column amounts with ground-based observations revealed no significant bias in the MIPAS data. Mean differences between MIPAS and FTIR column abundances are 0.11 +/- 0.12 x 10(14) cm(-2) (1.0 +/- 1.1%) and -0.09 +/- 0.19 x 10(14) cm(-2) (-0.8 +/- 1.7%), depending on the coincidence criterion applied. chi(2) tests have been performed to assess the combined precision estimates of MIPAS and the related instruments. When no exact coincidences were available as in case of MIPAS-FTIR or MIPAS-ACE-FTS comparisons it has been necessary to take into consideration a coincidence error term to account for chi(2) deviations. From the resulting chi(2) profiles there is no evidence for a systematic over/underestimation of the MIPAS random error analysis. C1 Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, Karlsruhe, Germany. Inst Astrofis Andalucia, E-18080 Granada, Spain. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. Univ Wollongong, Dept Chem, Wollongong, NSW, Australia. Harvard Smithsonian Ctr Astrophys, Opt & Infrared Astron Div, Cambridge, MA 02138 USA. Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. Chalmers, Dept Radio & Space Sci, S-41296 Gothenburg, Sweden. Univ Bremen, Inst Umweltphys, D-2800 Bremen 33, Germany. CALTECH, Jet Prop Lab, Pasadena, CA USA. Natl Inst Water & Atmospher Res, Lauder, New Zealand. RP Hopfner, M (reprint author), Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, Karlsruhe, Germany. EM michael.hoepfner@imk.fzk.de RI Milz, Mathias/C-9899-2011; Bernath, Peter/B-6567-2012; Ruhnke, Roland/J-8800-2012; Blumenstock, Thomas/K-2263-2012; Kleinert, Anne/A-7048-2013; Wetzel, Gerald/A-7065-2013; Hopfner, Michael/A-7255-2013; Stiller, Gabriele/A-7340-2013; Hase, Frank/A-7497-2013; Felix Friedl-Vallon, Felix/A-7741-2013; Oelhaf, Hermann/A-7895-2013; von Clarmann, Thomas/A-7287-2013; Reddmann, Thomas/A-7681-2013; Glatthor, Norbert/B-2141-2013; Kiefer, Michael/A-7254-2013; Schneider, Matthias/B-1441-2013; Funke, Bernd/C-2162-2008; Barthlott, Sabine/B-1439-2013; Jones, Nicholas/G-5575-2011; Notholt, Justus/P-4520-2016; OI Bernath, Peter/0000-0002-1255-396X; Hopfner, Michael/0000-0002-4174-9531; Stiller, Gabriele/0000-0003-2883-6873; von Clarmann, Thomas/0000-0003-2219-3379; Reddmann, Thomas/0000-0003-1733-7016; Funke, Bernd/0000-0003-0462-4702; Barthlott, Sabine/0000-0003-0258-9421; Jones, Nicholas/0000-0002-0111-2368; Notholt, Justus/0000-0002-3324-885X; Chance, Kelly/0000-0002-7339-7577; Mahieu, Emmanuel/0000-0002-5251-0286 NR 54 TC 32 Z9 33 U1 1 U2 4 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD JAN 18 PY 2007 VL 7 BP 257 EP 281 DI 10.5194/acp-7-257-2007 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 129RN UT WOS:000243747400002 ER PT J AU John, R Dalling, JW Harms, KE Yavitt, JB Stallard, RF Mirabello, M Hubbell, SP Valencia, R Navarrete, H Vallejo, M Foster, RB AF John, Robert Dalling, James W. Harms, Kyle E. Yavitt, Joseph B. Stallard, Robert F. Mirabello, Matthew Hubbell, Stephen P. Valencia, Renato Navarrete, Hugo Vallejo, Martha Foster, Robin B. TI Soil nutrients influence spatial distributions of tropical tree species SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE community assembly; niche differentiation; tropical forest ID RAIN-FOREST TREES; HABITAT SPECIALIZATION; DEPENDENT RECRUITMENT; ECUADORIAN AMAZONIA; DIPTEROCARP FOREST; DENSITY-DEPENDENCE; NEOTROPICAL FOREST; EDAPHIC FACTORS; DIVERSITY; ECOLOGY AB The importance of niche vs. neutral assembly mechanisms in structuring tropical tree communities remains an important unsettled question in community ecology [Bell G (2005) Ecology 86:17571770]. There is ample evidence that species distributions are determined by soils and habitat factors at landscape (< 10(4) km(2)) and regional scales. At local scales (< 1 km(2)), however, habitat factors and species distributions show comparable spatial aggregation, making it difficult to disentangle the importance of niche and dispersal processes. In this article, we test soil resource-based niche assembly at a local scale, using species and soil nutrient distributions obtained at high spatial resolution in three diverse neotropical forest plots in Colombia (La Planada), Ecuador (Yasuni), and Panama (Barro Colorado Island). Using spatial distribution maps of > 0.5 million individual trees of 1,400 species and 10 essential plant nutrients, we used Monte Carlo simulations of species distributions to test plant-soil associations against null expectations based on dispersal assembly. We found that the spatial distributions of 36-51% of tree species at these sites show strong associations to soil nutrient distributions. Neutral dispersal assembly cannot account for these plant-soil associations or the observed niche breadths of these species. These results indicate that belowground resource availability plays an important role in the assembly of tropical tree communities at local scales and provide the basis for future investigations on the mechanisms of resource competition among tropical tree species. C1 Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Trop Res Inst, Balboa, Panama. Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. US Geol Survey, Div Water Resources, Boulder, CO 80303 USA. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Pontifical Catolic Univ Ecuador, Dept Biol Sci, Quito, Ecuador. Inst Alexander Von Humboldt, Bogota, Colombia. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, 505 Goodwin Ave, Urbana, IL 61801 USA. EM dallingj@life.uiuc.edu RI Stallard, Robert/H-2649-2013 OI Stallard, Robert/0000-0001-8209-7608 NR 49 TC 364 Z9 409 U1 17 U2 165 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 16 PY 2007 VL 104 IS 3 BP 864 EP 869 DI 10.1073/pnas.0604666104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 129WP UT WOS:000243761100034 PM 17215353 ER PT J AU Buffington, ML Van Noort, S AF Buffington, M. L. Van Noort, S. TI A world revision of the Pycnostigminae (Cynipoidea : Figitidae) with descriptions of seven new species SO ZOOTAXA LA English DT Article DE Pycnostigmus; Tylosema; Trjapitziniola; Pycnostigminae; Figitidae; Cynipoidea; Hymenoptera; new species; redescription ID SOUTH-AFRICA; CAPE FLORA; HYMENOPTERA; PHYLOGENY; EVOLUTION AB Pycnostigmus rostratus Cameron, 1905, is redescribed and four new species of Pycnostigmus are described: P. mastersonae Buffington & van Noort, new species; P. incognito Buffington & van Noort, new species; P. fossilensis Buffington & van Noort, new species; and P. hoerikwaggoensis Buffington & van Noort, new species. Pycnostigmus mastersonae is the only known species of Cynipoidea with a metallic sheen on the head and mesosoma. A redescription of Tylosema nigerrimum Kieffer, 1905, is provided as well as the description of two new species: Tylosema dayae Buffington & van Noort, new species and Tylosema ronquisti Buffington & van Noort, new species. The discovery of two new species of Tylosema in South Africa is noteworthy since the only previously known species, T. nigerrimum Kieffer, is from Algeria. A redescription of Trjapitziniola popovi (Belizin 1951) is provided as well as the description of one new species: Trjapitziniola vanharteni Buffington & van Noort, new species. Trjapitziniola vanharteni was collected in the United Emirates Republic, which extends the distribution of Trjapitziniola well into the Arabian Penninsula. An online key to World species of Pycnostigminae and images are available at www.waspweb.org/Cynipoidea/Figitidae/Pycnostigminae/index.htm, and images of all species contained within this paper are available from http://morphbank.net. C1 Smithsonian NMNH, USDA, Systemat Entomol Lab, Washington, DC 20013 USA. Iziko S African Museum, Nat Hist Div, ZA-8000 Cape Town, South Africa. RP Buffington, ML (reprint author), Smithsonian NMNH, USDA, Systemat Entomol Lab, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM mbuffington@sel.barc.usda.gov RI van Noort, Simon/C-4006-2017 OI van Noort, Simon/0000-0001-6930-9741 NR 34 TC 14 Z9 14 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 15 PY 2007 IS 1392 BP 1 EP 30 PG 30 WC Zoology SC Zoology GA 125HR UT WOS:000243433500001 ER PT J AU Ates, C Pohl, T Pattard, T Rost, JM AF Ates, C. Pohl, T. Pattard, T. Rost, J. M. TI Antiblockade in Rydberg excitation of an ultracold lattice gas SO PHYSICAL REVIEW LETTERS LA English DT Article AB It is shown that the two-step excitation scheme typically used to create an ultracold Rydberg gas can be described with an effective two-level rate equation, greatly reducing the complexity of the optical Bloch equations. This allows us to efficiently solve the many-body problem of interacting cold atoms with a Monte Carlo technique. Our results reproduce the observed excitation blockade effect. However, we demonstrate that an Autler-Townes double peak structure in the two-step excitation scheme, which occurs for moderate pulse lengths as used in the experiment, can give rise to an antiblockade effect. It is most pronounced for atoms arranged on a lattice. Since the effect is robust against a large number of lattice defects it should be experimentally realizable with an optical lattice created by CO2 lasers. C1 Max Planck Inst Phys Complex Syst, D-01187 Dresden, Germany. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Ates, C (reprint author), Max Planck Inst Phys Complex Syst, Nothnitzer Str 38, D-01187 Dresden, Germany. RI Pohl, Thomas/B-5133-2013; OI Pattard, Thomas/0000-0002-2276-5173; Rost, Jan M./0000-0002-8306-1743 NR 11 TC 75 Z9 75 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 12 PY 2007 VL 98 IS 2 AR 023002 DI 10.1103/PhysRevLett.98.023002 PG 4 WC Physics, Multidisciplinary SC Physics GA 127LF UT WOS:000243586700018 PM 17358602 ER PT J AU Romaine, S Bruni, R Gorenstein, P Zhong, Z AF Romaine, S. Bruni, R. Gorenstein, P. Zhong, Z. TI Measurements of the hard-x-ray reflectivity of iridium SO APPLIED OPTICS LA English DT Article ID REFLECTANCE MEASUREMENTS; OPTICAL-CONSTANTS AB In connection with the design of a hard-x-ray telescope for the Constellation X-Ray Observatory we measured the reflectivity of an iridium-coated zerodur substrate as a function of angle at 55, 60, 70, and 80 keV at the National Synchrotron Light Source of Brookhaven National Laboratory. The optical constants were derived from the reflectivity data. The real component of the index of refraction is in excellent agreement with theoretical values at all four energies. However, the imaginary component, which is related to the mass attenuation coefficient, is 50% to 70% larger at 55, 60, and 70 keV than theoretical values. (c) 2007 Optical Society of America. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Brookhaven Natl Lab, Natl Synchrotron Light Source, Upton, NY 11973 USA. RP Romaine, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS83, Cambridge, MA 02138 USA. EM sromaine@cfa.harvard.edu NR 13 TC 4 Z9 4 U1 0 U2 2 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 JAN 10 PY 2007 VL 46 IS 2 BP 185 EP 189 DI 10.1364/AO.46.000185 PG 5 WC Optics SC Optics GA 123GD UT WOS:000243283500008 PM 17268563 ER PT J AU Hopkins, PF Richards, GT Hernquist, L AF Hopkins, Philip F. Richards, Gordon T. Hernquist, Lars TI An observational determination of the bolometric quasar luminosity function SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : observations; galaxies : active; galaxies : evolution; galaxies : luminosity function, mass function; infrared : galaxies; quasars : general; ultraviolet : galaxies; X-rays : galaxies ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; HARD X-RAY; SUPERMASSIVE BLACK-HOLES; HIGH-REDSHIFT QUASARS; SPECTRAL ENERGY-DISTRIBUTIONS; EARLY-TYPE GALAXIES; LY-ALPHA FOREST; UNIFIED SCHEMES; COSMOLOGICAL EVOLUTION AB We combine a large set of quasar luminosity function (QLF) measurements from the rest-frame optical, soft and hard X-ray, and near- and mid-IR bands to determine the bolometric QLF in the redshift interval z = 0-6. Accounting for the observed distributions of quasar column densities and variation of SED shapes, as well as their dependence on luminosity, makes it possible to integrate the observations in a reliable manner and provides a baseline in redshift and luminosity larger than that of any individual survey. We infer the QLF break luminosity and faint-end slope out to z similar to 4.5 and confirm at high significance (greater than or similar to 10 sigma) previous claims of a flattening in both the faint- and bright-end slopes with redshift. With the best-fit estimates of the column density distribution and quasar SED, which both depend on luminosity, a single bolometric QLF self-consistently reproduces the observed QLFs in all bands and at all redshifts for which we compile measurements. Ignoring this luminosity dependence does not yield a self-consistent bolometric QLF and there is no evidence for any additional dependence on redshift. We calculate the expected relic black hole mass function and mass density, cosmic X-ray background, and ionization rate as a function of redshift and find that they are consistent with existing measurements. The peak in the total quasar luminosity density is well constrained at z = 2.15 +/- 0.05. We provide a number of fitting functions to the bolometric QLF and its manifestations in various bands, as well as a script to return the QLF at arbitrary frequency and redshift from these fits. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 176 TC 559 Z9 563 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2007 VL 654 IS 2 BP 731 EP 753 DI 10.1086/509629 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124PU UT WOS:000243382900004 ER PT J AU Sakamoto, K Ho, PTP Mao, RQ Matsushita, S Peck, AB AF Sakamoto, Kazushi Ho, Paul T. P. Mao, Rui-Qing Matsushita, Satoki Peck, Alison B. TI Detection of CO hot spots associated with young clusters in the southern starburst galaxy NGC 1365 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 1365); galaxies : ISM; galaxies : starburst; galaxies : star clusters ID HUBBLE-SPACE-TELESCOPE; BARRED SPIRAL GALAXY; MOLECULAR GAS PROPERTIES; SEYFERT-GALAXIES; NGC 1365; STAR-CLUSTERS; RADIO-CONTINUUM; GALACTIC-CENTER; CENTRAL REGIONS; INTERSTELLAR-MEDIUM AB We have used the Submillimeter Array for the first interferometric CO imaging toward the starburst-Seyfert nucleus of the southern barred spiral galaxy NGC 1365, which is one of the four galaxies within 30 Mpc that have L8-1000 mu m >= 10(11) L-.. Our mosaic maps of (CO)-C-12, (CO)-C-13, and (CO)-O-18 (J = 2-1) emission at up to 2 '' ( 200 pc) resolutions have revealed a circumnuclear gas ring and several CO clumps in the central 3 kpc. The molecular ring shows morphological and kinematical signs of bar-driven gas dynamics, and the region as a whole is found to follow the star formation laws of Kennicutt. We have found that some of the gas clumps and peaks in CO brightness temperature, which we collectively call CO hot spots, coincide with the radio and mid-infrared sources previously identified as dust-enshrouded super star clusters. This hot spot-cluster association suggests that either the formation of the most massive clusters took place in large molecular gas concentrations ( of Sigma(mol) similar to 10(3) M-. pc(-2) in 200 pc scales) or the clusters have heated their ambient gas to cause or enhance the CO hot spots. The active nucleus is in the region of weak CO emission and is not associated with distinctive molecular gas properties. C1 Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96720 USA. Natl Astron Observ Japan, Tokyo, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Chinese Acad Sci, Purple Mt Observ, Nanjing, Peoples R China. RP Sakamoto, K (reprint author), Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96720 USA. EM sakamoto.kazushi@nao.ac.jp NR 97 TC 16 Z9 16 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2007 VL 654 IS 2 BP 782 EP 798 DI 10.1086/509775 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124PU UT WOS:000243382900007 ER PT J AU Bloom, JS Perley, DA Chen, HW Butler, N Prochaska, JX Kocevski, D Blake, CH Szentgyorgyi, A Falco, EE Starr, DL AF Bloom, J. S. Perley, D. A. Chen, H. -W. Butler, N. Prochaska, J. X. Kocevski, D. Blake, C. H. Szentgyorgyi, A. Falco, E. E. Starr, D. L. TI A putative early-type host galaxy for GRB 060502B: Implications for the progenitors of short-duration hard-spectrum bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; galaxies : elliptical and lenticular, cD; gamma rays : bursts ID GAMMA-RAY BURSTS; LARGE-SCALE ENVIRONMENTS; NEUTRON-STAR BINARIES; SKY SURVEY; AFTERGLOW; GRB-050709; CATALOG; CONSTRAINTS; DISTRIBUTIONS; LUMINOSITY AB Starting with the first detection of an afterglow from a short-duration hard-spectrum gamma-ray burst (SHB) by Swift last year, a growing body of evidence has suggested that SHBs are associated with an older and lower redshift galactic population than long-soft GRBs and, in a few cases, with large (greater than or similar to 10 kpc) projected offsets from the centers of their putative host galaxies. Here we present observations of the field of GRB 060502B, a SHB detected by Swift and localized by the X-Ray Telescope (XRT). We find a massive red galaxy at a redshift of z = 0.287 at an angular distance of 17: 100 from our revised XRT position. Using associative and probabilistic arguments, we suggest that this galaxy hosted the progenitor of GRB 060502B. If true, this offset would correspond to a physical displacement of 73 +/- 19 kpc in projection, about twice the largest offset inferred for any SHB to date and almost an order of magnitude larger than a typical long-soft burst offset. Spectra and modeling of the star formation history of this possible host show it to have undergone a large ancient starburst. If the progenitor of GRB060502B was formed in this starburst episode, the time of the GRB explosion since birth is tau approximate to 1.3 +/- 0.2 Gyr and the minimum kick velocity of the SHB progenitor is v(kick,min) = 55 +/- 15 km s(-1). C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloom, JS (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 60 TC 52 Z9 53 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2007 VL 654 IS 2 BP 878 EP 884 DI 10.1086/509114 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124PU UT WOS:000243382900014 ER PT J AU Torres, G AF Torres, Guillermo TI The planet host star gamma Cephei: Physical properties, the binary orbit, and the mass of the substellar companion SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; binaries : visual; planetary systems; stars : individual (gamma Cephei); stars : late-type ID STANDARD VELOCITY STARS; INTERMEDIATE ASTROMETRIC DATA; RADIAL-VELOCITIES; SPECTROSCOPIC BINARIES; NEARBY STARS; K-GIANTS; SPECTROGRAPHIC OBSERVATIONS; CHEMICAL ABUNDANCES; DYNAMICAL STABILITY; OXYGEN ABUNDANCES AB The bright, K1 IIIYIV star gamma Cep has been reported previously to have a possibly substellar companion in a similar to 2.5 yr orbit, as well as an unseen stellar companion at a larger separation. We determine for the first time the three-dimensional orbit of the latter, accounting also for the perturbation from the closer object. We combine new and existing radial velocity measurements with intermediate astrometric data from the Hipparcos mission ( abscissa residuals), as well as ground-based positional observations going back more than a century. The orbit of the secondary star is eccentric (e = 0.4085 +/- 0.0065) and has a period P = 66.8 +/- 1.4 yr. We establish the primary star to be on the first ascent of the giant branch and to have a mass of 1.18 +/- 0.11 M-., an effective temperature of 4800 +/- 100 K, and an age around 6.6 Gyr ( for an assumed metallicity [Fe/H] = +0.01 +/- 0.05). The unseen secondary star is found to be an M4 dwarf with a mass of 0.362 +/- 0.022 M-. and is expected to be similar to 6.4 mag fainter than the primary in K. The minimum mass of the putative planetary companion is M-p sin i = 1.43 +/- 0.13 M-Jup. Based on high-precision Hipparcos observations, we are able to place a dynamical upper limit on this mass of 13.3 M-Jup at the 95% confidence level, and 16.9 M-Jup at the 99.73% (3 sigma) confidence level, thus confirming that it is indeed substellar in nature. The orbit of this object is only 9.8 times smaller than the orbit of the secondary star ( the smallest ratio among exoplanet host stars in multiple systems), but it is stable if coplanar with the binary. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu NR 80 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 JAN 10 PY 2007 VL 654 IS 2 BP 1095 EP 1109 DI 10.1086/509715 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124PU UT WOS:000243382900033 ER PT J AU Abrahamsson, E Krems, RV Dalgarno, A AF Abrahamsson, E. Krems, R. V. Dalgarno, A. TI Fine-structure excitation of OI and CI by impact with atomic hydrogen SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; atomic processes; methods : numerical; molecular processes; scattering ID PHYSICAL CONDITIONS; NEUTRAL CARBON; EMISSION; REGIONS; OXYGEN; GAS; CO AB Using accurate interaction potentials, we perform refined calculations of rate coefficients for the fine-structure excitations in collisions of O(P-3) and C(P-3) with atomic hydrogen. The results are presented in the form of analytical functions approximating the rate coefficients over a wide range of temperatures. We examine the sensitivity of the collision dynamics to variations of the interaction potentials and the couplings to electronically excited states. C1 Univ British Columbia, Dept Chem, Vancouver, BC, Canada. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Abrahamsson, E (reprint author), Univ British Columbia, Dept Chem, Vancouver, BC, Canada. EM rkrems@chem.ubc.ca NR 19 TC 36 Z9 36 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2007 VL 654 IS 2 BP 1171 EP 1174 DI 10.1086/509631 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124PU UT WOS:000243382900040 ER PT J AU Worden, J Liu, X Bowman, K Chance, K Beer, R Eldering, A Gunson, M Worden, H AF Worden, John Liu, Xiong Bowman, Kevin Chance, Kelly Beer, Reinhard Eldering, Annmarie Gunson, Michael Worden, Helen TI Improved tropospheric ozone profile retrievals using OMI and TES radiances SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EMISSION SPECTROMETER; MODEL; SATELLITE AB We perform a study for characterizing the vertical resolution of tropospheric ozone profile retrievals from the combination of simulated ultraviolet (UV) and thermal infrared (TIR) observations that are representative of the EOS Aura Ozone Monitoring Instrument (OMI) and the Tropospheric Emission Spectrometer (TES). Under the low thermal contrast conditions used for this simulation, we find that estimating ozone profiles by combining UV and TIR radiances results in a factor of two or more improvement in the ability to resolve boundary layer ozone, as compared with either instrument alone. In addition, there is a substantial improvement in the vertical resolution of ozone in the free troposphere (between 20% and 60%) as compared to the TES vertical resolution. This study points towards the importance of combining multiple spectral regions for dramatically improving the sounding of tropospheric trace gases. C1 CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Worden, J (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, 4800 OAk Grove Dr,MS 183-301, Pasadena, CA 91109 USA. EM john.worden@jpl.nasa.gov RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 NR 21 TC 41 Z9 41 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JAN 10 PY 2007 VL 34 IS 1 AR L01809 DI 10.1029/2006GL027806 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 126QG UT WOS:000243528900003 ER PT J AU Montanez, IP Tabor, NJ Niemeier, D DiMichele, WA Frank, TD Fielding, CR Isbell, JL Birgenheier, LP Rygel, MC AF Montanez, Isabel P. Tabor, Neil J. Niemeier, Deb DiMichele, William A. Frank, Tracy D. Fielding, Christopher R. Isbell, John L. Birgenheier, Lauren P. Rygel, Michael C. TI CO2-forced climate and vegetation instability during late paleozoic deglaciation SO SCIENCE LA English DT Article ID ATMOSPHERIC CARBON-DIOXIDE; ISOTOPIC COMPOSITION; ORGANIC-MATTER; NORTH-AMERICA; GLACIATION; CO2; RECORD; OXYGEN; PALEOCLIMATE; TRANSITION AB The late Paleozoic deglaciation is the vegetated Earth's only recorded icehouse-to-greenhouse transition, yet the climate dynamics remain enigmatic. By using the stable isotopic compositions of soil-formed minerals, fossil-plant matter, and shallow-water brachiopods, we estimated atmospheric partial pressure of carbon dioxide (pCO(2)) and tropical marine surface temperatures during this climate transition. Comparison to southern Gondwanan glacial records documents covariance between inferred shifts in pCO(2), temperature, and ice volume consistent with greenhouse gas forcing of climate. Major restructuring of paleotropical flora in western Euramerica occurred in step with climate and pCO(2) shifts, illustrating the biotic impact associated with past CO2-forced turnover to a permanent ice-free world. C1 Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. So Methodist Univ, Dept Geol Sci, Dallas, TX 75275 USA. Univ Calif Davis, Dept Civil & Environm Engn, Davis, CA 95616 USA. Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Nebraska, Dept Geosci, Lincoln, NE 68588 USA. Univ Wisconsin, Dept Geosci, Milwaukee, WI 53201 USA. RP Montanez, IP (reprint author), Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. EM montanez@geology.ucdavis.edu RI DiMichele, William/K-4301-2012 NR 47 TC 228 Z9 235 U1 9 U2 60 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 5 PY 2007 VL 315 IS 5808 BP 87 EP 91 DI 10.1126/science.1134207 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 122WU UT WOS:000243259100041 PM 17204648 ER PT J AU Pawson, DL AF Pawson, David L. TI Narcissia ahearnae, a new species of sea star from the Western Atlantic (Echinodermata : Asteroidea : Valvatida) SO ZOOTAXA LA English DT Article DE Narcissia ahearnae; Asteroidea; Valvatida; Ophidiasteridae AB Narcissia ahearnae, new species, is described from off the east coast of Florida and the Bahamas, in depths of 53-135 m. It is distinctive in having conspicuous undulating carinal ridges extending from the center of the disc along the upper surfaces of the arms. C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Pawson, DL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Mail Stop MRC163, Washington, DC 20013 USA. EM pawsond@si.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 4 PY 2007 IS 1386 BP 53 EP 58 PG 6 WC Zoology SC Zoology GA 123CY UT WOS:000243275100006 ER PT J AU Willard, DA Phillips, TL Lesnikowska, AD DiMichele, WA AF Willard, Debra A. Phillips, Tom L. Lesnikowska, Alicia D. DiMichele, William A. TI Paleoecology of the Late Pennsylvanian-age Calhoun coal bed and implications for long-term dynamics of wetland ecosystems SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article DE Late Pennsylvanian; coal; coal-ball; paleoecology; palynology; ecosystem stability ID PALEOCLIMATE CONTROLS; SWAMP VEGETATION; ILLINOIS BASIN; DUQUESNE COAL; OHIO USA; ASSEMBLAGES; PATTERNS; PLANTS; PERSISTENCE AB Quantitative plant assemblage data from coal balls, miospores, megaspores, and compression floras from the Calhoun coal bed (Missourian) of the Illinois Basin (USA) are used to interpret spatial and temporal changes in plant communities in the paleo-peat swamp. Coal-ball and miospore floras froth the Calhoun coal bed are dominated strongly by tree ferns, and pteridosperms and sigillarian lycopsids are subdominant, depending on geographic location within the coal bed. Although the overall composition of Calhoun peat-swamp assemblages is consistent both temporally and spatially, site-to-site differences and short-term shifts in species dominance indicate local topographic and hydrologic control on species composition within the broader context of the swamp. Statistical comparison of the Calhoun miospore assemblages with those from other Late Pennsylvanian coal beds suggests that the same basic species pool was represented in each peat-swamp landscape and that the relative patterns of dominance and diversity were persistent from site to site. Therefore, it appears that the relative patterns of proportional dominance stayed roughly the same from one coal bed to the next during Late Pennsylvanian glacially-driven climatic oscillations. Published by Elsevier B.V. C1 US Geol Survey, Reston, VA USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Inst, NMNH, Dept Paleobiol, Washington, DC 20560 USA. RP Willard, DA (reprint author), US Geol Survey, 926A Natl Ctr, Reston, VA USA. EM dwillard@usgs.gov RI DiMichele, William/K-4301-2012 NR 48 TC 21 Z9 21 U1 1 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD JAN 2 PY 2007 VL 69 IS 1-2 BP 21 EP 54 DI 10.1016/j.coal.2006.03.011 PG 34 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 130QQ UT WOS:000243814500002 ER PT B AU Ramsay, G Brocksopp, C Groot, PJ Hakala, P Lehto, H Marsh, TR Napiwotzki, R Nelemans, G Potter, S Slee, B Steeghs, D Wu, K AF Ramsay, G. Brocksopp, C. Groot, P. J. Hakala, P. Lehto, H. Marsh, T. R. Napiwotzki, R. Nelemans, G. Potter, S. Slee, B. Steeghs, D. Wu, K. BE Napiwotzki, R Burleigh, MR TI Recent observational progress in AM CVn binaries SO 15TH EUROPEAN WORKSHOP ON WHITE DWARFS, PROCEEDINGS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 15th European Workshop on White Dwarfs CY AUG 07-11, 2006 CL Univ Leicester, Leicester, ENGLAND HO Univ Leicester ID XMM-NEWTON OBSERVATIONS; TEMPORAL SURVEY RATS; RX J1914+24; SYSTEMS; EMISSION AB We present the results of some recent research on AM CVn systems. We present: X-ray/UV observations made using XMM-Newton; the Xray grating spectrum of RX J1914+24 preliminary results of a search for radio emission from AM CVn binaries, and discuss the strategy and first results of the RATS project, whose main aim is to discover AM CVn systems. C1 [Ramsay, G.; Brocksopp, C.; Wu, K.] UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Groot, P. J.; Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, Nijmegen, Netherlands. [Hakala, P.; Lehto, H.] Univ Turku, Tuorla Observ, Turku, Finland. [Marsh, T. R.] Univ Warwick, Dept Phys, Coventry, W Midlands, England. [Napiwotzki, R.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield, Herts, England. [Potter, S.] S African Astronom, Cape Town, South Africa. [Slee, B.] Australia Telescope Natl Facil, Sydney, NSW, Australia. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Ramsay, G (reprint author), UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X NR 13 TC 6 Z9 6 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-239-6 J9 ASTR SOC P PY 2007 VL 372 BP 425 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGV80 UT WOS:000250828100084 ER PT S AU Blundell, R AF Blundell, Raymond GP IEEE TI The submillimeter array SO 2007 IEEE/MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST, VOLS 1-6 SE IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST LA English DT Proceedings Paper CT IEEE/MTT-S International Microwave Symposium CY JUN 03-08, 2007 CL Honolulu, HI SP IEEE MTTS DE submillimeter wave antennas; submillimeter wave instrumentation; submillimeter wave astronomy AB The Submillimeter Array, a collaboration between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics of Taiwan, is a pioneering radio-interferometer made up of eight 6-meter diameter antennas designed for high angular resolution astronomical observations of the cool universe throughout the major atmospheric windows from about 200 to 900 GHz. Each antenna houses a single cryostat, with an integrated cryocooler that can cool eight heterodyne receivers to 4 K. Four receiver bands are available: 180-250 GHz, 266-355 GHz, 320-420 GHz, and 600-700 GHz, and simultaneous observations are possible in any pair of high and low frequency receiver bands. C1 [Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blundell, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Blundell, Richard/C-1552-2008 OI Blundell, Richard/0000-0003-1588-2299 NR 4 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-645X BN 978-1-4244-0687-6 J9 IEEE MTT-S PY 2007 BP 1849 EP 1852 PG 4 WC Engineering, Electrical & Electronic; Optics; Telecommunications SC Engineering; Optics; Telecommunications GA BGV76 UT WOS:000250827404085 ER PT B AU Faisal, FHM Abdurrouf, A Miyazaki, K Miyaji, G AF Faisal, F. H. M. Abdurrouf, A. Miyazaki, K. Miyaji, G. GP IEEE TI A theory of molecular high harmonic generation from coherently rotating molecules and interpretation of recent pump-probe experiments SO 2007 PACIFIC RIM CONFERENCE ON LASERS AND ELECTRO-OPTICS, VOLS 1-4 LA English DT Proceedings Paper CT Pacific Rim Conference on Lasers and Electro-Optics CY AUG 26-31, 2007-2008 CL Seoul, SOUTH KOREA ID ALIGNMENT AB A general theory of molecular high harmonic generation in intense femtosecond pump-probe experiments is presented. It provides explicit analytical expressions correlating the harmonic signals with the dynamical alignment of linear molecules. Recent experimental data from purnp-probe experiments are analyzed and a unified interpretation of the diverse observations is given. C1 [Faisal, F. H. M.; Abdurrouf, A.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany. [Faisal, F. H. M.] ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miyazaki, K.; Miyaji, G.] Kyoto Univ, Inst Adv Energy, Kyoto 6110011, Japan. RP Faisal, FHM (reprint author), Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany. EM ffaisal@harvard.cfa.edu FU NSF; ITAMP at Harvard University; Smithsonian Astrophysical Observatory FX This work was partially supported by NSF through a grant for ITAMP at Harvard University and Smithsonian Astrophysical Observatory. NR 6 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-1173-3 PY 2007 BP 778 EP + PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BHW12 UT WOS:000256956600392 ER PT S AU Szentgyorgyi, AH Furesz, G AF Szentgyorgyi, A. H. Furesz, G. BE Kurtz, S Franco, J Hong, S GarciaSegura, G Santillan, A Kim, J Han, I TI Precision radial velocities for the Kepler era SO 3rd Mexico-Korea Conference on Astrophysics: Telescopes of the Future and San Pedro Martir SE REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA, SERIE DE CONFERENCIAS LA English DT Proceedings Paper CT 3rd Mexico-Korea Conference on Astrophysics - Telescopes of the Future and San Pedro Martir CY NOV 08-11, 2005 CL Mexico City, MEXICO DE instrumentation : spectrographs; techniques : radial velocity; stars : planetary systems : protoplanetary disks ID SPECTROGRAPH AB The Kepler Mission will provide photometry for 100,000 dwarfs to m similar to 14 in search of terrestrial-sized exoplanets in a northern field 107 degrees square. This search requires massive photometric and spectroscopic reconnaissance both to identify the dwarfs from the millions of stars in the field and post facto to weed out impostor binaries and blends that mimic transiting earth-size exoplanets. In this paper we discuss several new instruments that the Smithsonian Astrophysical Observatory has recently commissioned or is building that are cornerstones of this spectroscopic follow-up: the Hectochelle and TRES. C1 Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, Cambridge, MA 02138 USA. RP Szentgyorgyi, AH (reprint author), Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, M-S 20,60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 13 Z9 13 U1 0 U2 1 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 BN 978-970-32-3273-4 J9 REV MEX AST ASTR PY 2007 VL 28 BP 129 EP 133 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGT50 UT WOS:000250418400025 ER PT S AU Bogdanov, S Grindlay, JE AF Bogdanov, Slavko Grindlay, Jonathan E. BE Bassa, CG Wang, Z Cumming, A Kaspi, VM TI An X-ray view of radio millisecond pulsars SO 40 YEARS OF PULSARS: MILLISECOND PULSARS, MAGNETARS AND MORE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT AIP Conference: 40 Years of Pulsars CY AUG 12-17, 2007 CL Montreal, CANADA SP McGill Univ, Phys Dept, McGill Univ, Fac Sci, Canadian Inst Theoret Astrophys, Canadian Inst Adv Res DE neutron stars; millisecond pulsars; X-rays ID XMM-NEWTON OBSERVATIONS; 47 TUCANAE; EMISSION; CHANDRA; 47-TUCANAE; J0437-4715; RADIATION; B1957+20; NGC-6397 AB In recent years, X-ray observations with Chandra and XMM-Newton have significantly increased our understanding of rotation-powered (radio) millisecond pulsars (MSPs). Deep Chandra studies of several globular clusters have detected X-ray counterparts to a host of MSPs, including 19 in 47 Tuc alone. These surveys have revealed that most MSPs exhibit thermal emission from their heated magnetic polar caps. Realistic models of this thermal X-ray emission have provided important insight into the basic physics of pulsars and neutron stars. In addition, intrabinary shock X-ray radiation observed in "black-widow" and peculiar globular cluster "exchanged" binary MSPs give interesting insight into MSP winds and relativistic shock. Thus, the X-ray band contains valuable information regarding the basic properties of MSPs that are not accesible by radio timing observations. C1 [Bogdanov, Slavko; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bogdanov, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 32 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0502-8 J9 AIP CONF PROC PY 2007 VL 983 BP 64 EP 68 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHL21 UT WOS:000254022400010 ER PT S AU Ho, WCG Mow, K AF Ho, Wynn C. G. Mow, Kaya BE Bassa, CG Wang, Z Cumming, A Kaspi, VM TI Modeling phase-resolved observations of the surfaces of magnetic neutron stars SO 40 YEARS OF PULSARS: MILLISECOND PULSARS, MAGNETARS AND MORE SE AIP Conference Proceedings LA English DT Proceedings Paper CT AIP Conference: 40 Years of Pulsars CY AUG 12-17, 2007 CL Montreal, CANADA SP McGill Univ, Phys Dept, McGill Univ, Fac Sci, Canadian Inst Theoret Astrophys, Canadian Inst Adv Res DE stars : atmospheres; stars : magnetic fields; stars : neutron; stars : rotation; X-rays : stars ID EQUATION-OF-STATE; ATMOSPHERE MODELS; HYDROGEN ATMOSPHERES; SPECTRAL FEATURES; THERMAL EMISSION; XMM-NEWTON; X-RAYS; FIELDS; POLARIZATION; RADIATION AB Recent observations by XMM-Newton detected rotational pulsations in the total brightness and spectrum of several neutron stars. To properly interpret the data, accurate modeling of neutron star emission is necessary. Detailed analysis of the shape and strength of the rotational variations allows a measurement of the surface composition and magnetic field, as well as constrains the nuclear equation of state. We discuss our models of the spectra and light curves of two of the most observed neutron stars, RX J1856.5-3754 and 1E 1207.4-5209, and discuss some implications of our results and the direction of future work. C1 [Ho, Wynn C. G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Mow, Kaya] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Ho, WCG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 50 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0502-8 J9 AIP CONF PROC PY 2007 VL 983 BP 340 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHL21 UT WOS:000254022400080 ER PT S AU Heinke, CO Deloye, CJ Jonker, PG Taam, RE Wijnands, R AF Heinke, C. O. Deloye, C. J. Jonker, P. G. Taam, R. E. Wijnands, R. BE Bassa, CG Wang, Z Cumming, A Kaspi, VM TI SAX J1808.4-3657 in Quiescence: A keystone for neutron star science SO 40 YEARS OF PULSARS: MILLISECOND PULSARS, MAGNETARS AND MORE SE AIP Conference Proceedings LA English DT Proceedings Paper CT AIP Conference: 40 Years of Pulsars CY AUG 12-17, 2007 CL Montreal, CANADA SP McGill Univ, Phys Dept, McGill Univ, Fac Sci, Canadian Inst Theoret Astrophys, Canadian Inst Adv Res DE neutron stars; X-ray binaries; nuclear matter; pulsars ID ACCRETING MILLISECOND PULSAR; ACTIVE RADIO PULSAR; OPTICAL COUNTERPART; EMISSION; SAX-J1808.4-3658 AB The accreting millisecond pulsar SAX J1809.4-3658 may be a transition object between accreting X-ray binaries and millisecond radio pulsars. We have constrained the thermal radiation from its surface through XMM-Newton X-ray observations, providing strong evidence for neutrino cooling processes from the neutron star core. We have also undertaken simultaneous X-ray and optical (Gemini) observations, shedding light on whether the strong heating of the companion star in quiescence may be due to X-ray irradiation, or to a radio pulsar turning on when accretion stops. C1 [Heinke, C. O.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Heinke, C. O.; Deloye, C. J.; Taam, R. E.] Northwestern Univ, Dept Phys, Evanston, IL 60208 USA. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Heinke, CO (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. FU Northwestern University; NASA XMM [NNX06AH62G]; Netherlands Organization for Scientific Research; NASA through the Chandra X-ray Center [TM7-800]; ESA Member States FX We thank S. Sengupta for continuing conversations. COH thanks A. Bonanos for assistance with the ISIS software. We thank M. Prakash, D. Page, K. Levenfish, D. Yakovlev and D. Chakrabarty for discussions. COH acknowledges the Lindheimer Postdoctoral Fellowship at Northwestern University. COH and CJD acknowledge support from NASA XMM grant NNX06AH62G. PGJ acknowledges support from the Netherlands Organization for Scientific Research. CJD acknowledges support from NASA through the Chandra X-ray Center, grant number TM7-800. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: The National Science Foundation (United States), the Particle Physics and Astronomy Research Council (United Kingdom), The National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brzil), and CONICET (Argentina). NR 21 TC 1 Z9 1 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0502-8 J9 AIP CONF PROC PY 2007 VL 983 BP 526 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHL21 UT WOS:000254022400114 ER PT S AU Kildea, J AF Kildea, J. CA Veritas Collaboration BE Bassa, CG Wang, Z Cumming, A Kaspi, VM TI VERITAS observations of pulsars SO 40 YEARS OF PULSARS: MILLISECOND PULSARS, MAGNETARS AND MORE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT AIP Conference: 40 Years of Pulsars CY AUG 12-17, 2007 CL Montreal, CANADA SP McGill Univ, Phys Dept, McGill Univ, Fac Sci, Canadian Inst Theoret Astrophys, Canadian Inst Adv Res DE pulsars; VERITAS; EGRET; GLAST; TeV; Cherenkov; Polar Cap; Outer Gap ID TELESCOPE; EMISSION AB The EGRET detector on board the Compton Gamma-Ray Observatory detected pulsed emission from seven pulsars up to energies around 10 GeV. Despite numerous attempts, no pulsed emission has been observed by ground-based gamma-ray telescopes operating above similar to 100 GeV. A pulsed emission cut-off necessarily lies between. Any detection of this cut-off has important implications for the models that attempt to explain pulsar emission. With the current generation of ground-based gamma-ray telescopes extending in energy below 100 GeV and with GLAST promising observations above 10 GeV, pulsars are promising targets for future gamma-ray observation. We discuss here the VERITAS program for pulsar observations, its progress to date, and methods to improve the sensitivity of VERITAS for gamma rays below 100 GeV. C1 [Kildea, J.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Kildea, J (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0502-8 J9 AIP CONF PROC PY 2007 VL 983 BP 618 EP 620 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHL21 UT WOS:000254022400136 ER PT S AU Forman, W Jones, C Churazov, E AF Forman, W. Jones, C. Churazov, E. GP ESA BE Grebenev, S Sunyaev, R Winkler, C TI Shocks, bubbles, and filaments: The effects of supermassive black hole outbursts SO 6TH INTEGRAL WORKSHOP: THE OBSCURED UNIVERSE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 6th Integral Workshop on the Obscured Universe CY JUL 02-08, 2006 CL Space Res Inst, Moscow, RUSSIA SP Space Res Inst, European Space Agcy, Russian Acad Sci, Russian Basic Res Fdn HO Space Res Inst DE galaxy; X-ray; M87 ID M87; CLUSTER; GALAXIES; FLOW; JET; GAS AB We summarize the results derived from a 500 ksec Chandra observation of M87. At hard energies (3.5-7.5 keV), we detect a nearly circular shell of outer radius 2.8' (13 kpc). This ring of hard X-ray emission provides a clear signature of a weak shock, driven by an outburst from the supermassive black hole at the center of M87. We find that the observed density and temperature jumps are consistent with a Mach M similar to 1.2 shock (for monoatomic gas with gamma = 5/3). From a series of models, we find that the outburst energy required to drive the shock is 5 x 10(57) ergs and that the outburst occurred similar to 14 x 10(6) years ago. At soft energies (0.5-1.0 keV), we detect a complex filamentary web. This filamentary structure is particularly striking in the eastern arm where we suggest the filaments are the outer edges of a series of buoyant bubbles filled with relativistic plasma, produced by the central supermassive black hole, in a succession of small outbursts. The M87 outburst is intermediate in energy and radial scale between outbursts from supermassive black holes in "normal" galaxies with typical outbursts of similar to 10(57) ergs and several spectacular outbursts detected from central galaxies in rich clusters with outburst energies up to 10(62) ergs. Over a wide range, active nuclei are able to provide significant energy to the radiatively cooling gas in galaxy, group, and cluster atmospheres. C1 [Forman, W.; Jones, C.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Forman, W (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Churazov, Eugene/A-7783-2013 NR 19 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 J9 ESA SP PUBL PY 2007 VL 622 BP 187 EP 190 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHK58 UT WOS:000253876500029 ER PT J AU Molenda-Zakowicz, J Frasca, A Latham, DW Jerzykiewicz, M AF Molenda-Zakowicz, J. Frasca, A. Latham, D. W. Jerzykiewicz, M. TI Spectroscopic study of Kepler asteroseismic targets SO ACTA ASTRONOMICA LA English DT Article DE binaries : spectroscopic; binaries : eclipsing; stars : fundamental parameters; stars : individual : FL Lyr HIP 94734; V2077 Cyg ID PROPER-MOTION STARS; ELODIE ECHELLE SPECTRA; PARAMETERS T-EFF; ONLINE DETERMINATION; STELLAR EVOLUTION; LOG G; BINARIES; FE/H; METALLICITIES; OSCILLATIONS AB Reported are spectroscopic observations of 15 candidates for Kepler primary asteroseismic targets and 14 other stars in the Kepler field, carried out at three observatories. For all these stars, the radial velocities, effective temperature, surface gravity, metallicity, and the projected rotational velocity are derived from two separate sets of data by means of two independent methods. In addition, MK type is estimated from one of these sets of data. Three stars, HIP 94335, HIP 94734, and HIP 94743, are found to have variable radial-velocity. For HIP 94335 = FL Lyr, a well-known Algol-type eclipsing variable and a double-lined spectroscopic binary, the orbital elements computed from our data agree closely with those of Popper et al. For HIP 94734 and HIP 94743 = V2077 Cyg, which we discover to be single-lined systems, orbital elements are derived. In addition, from our value of the orbital period and the Hipparcos epoch photometry, HIP 94743 is demonstrated to be a detached eclipsing binary. C1 [Molenda-Zakowicz, J.; Jerzykiewicz, M.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Frasca, A.] Catania Astrophys Observ, I-95123 Catania, Italy. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Molenda-Zakowicz, J (reprint author), Univ Wroclaw, Astron Inst, Kopernika 11, PL-51622 Wroclaw, Poland. EM molenda@astro.uni.wroc.pl; afr@oact.inaf.it; dlatham@cfa.harvard.edu; mjerz@astro.uni.wroc.pl OI Frasca, Antonio/0000-0002-0474-0896 NR 25 TC 13 Z9 13 U1 0 U2 1 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2007 VL 57 IS 4 BP 301 EP 321 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259QP UT WOS:000252954100002 ER PT S AU Novikova, I Gorshkov, AV Phillips, DF Xiao, Y Klein, M Walsworth, RL AF Novikova, Irina Gorshkov, Alexey V. Phillips, David F. Xiao, Yanhong Klein, Mason Walsworth, Ronald L. BE Hasan, ZU Craig, AE Shahriar, SM Coufal, HJ TI Optimization of slow and stored light in atomic vapor - art. no. 64820M SO Advanced Optical and Quantum Memories and Computing IV SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced Optical and Quantum Memories and Computing IV CY JAN 24-25, 2007 CL San Jose, CA SP SPIE DE electromagnetically; induced transparency; slow light; stored light; vapor cell; buffer gas ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; QUANTUM COMMUNICATION; STORAGE; ENSEMBLES; PULSES AB We present a preliminary experimental study of optimized sloq and stored light pulses in Rb vapor cells, We study the efficiency of light storage as a function of pulse duration, storage time, retrieval field intensity, etc. We demonstrate a procedure based on time reversal for the optimization of the efficiency for storage of fight in atomic ensembles suggested in a recent theoretical paper [A. V. Gorshkov Pt al., e-print archive quant-ph/0604037 (2006)]. Experimental results are in a good qualitative agreement with theoretical calculations based oil a simplified three-level model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Novikova, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gorshkov, Alexey/A-9848-2008 OI Gorshkov, Alexey/0000-0003-0509-3421 NR 24 TC 1 Z9 1 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-6595-5 J9 P SOC PHOTO-OPT INS PY 2007 VL 6482 BP M4820 EP M4820 AR 64820M DI 10.1117/12.716400 PG 11 WC Optics SC Optics GA BGF12 UT WOS:000246396000013 ER PT J AU Gorenstein, P AF Gorenstein, Paul TI Diffractive-refractive X-ray optics for very high angular resolution X-ray astronomy SO ADVANCES IN SPACE RESEARCH LA English DT Article DE x-rays; diffractive optics; high angular resolution ID HIGH-ENERGY ASTRONOMY; TELESCOPES AB The 0.5 arcsec angular resolution of the Chandra X-ray Observatory is possibly the best that a grazing incidence telescope with substantial collecting area will ever attain. We describe a telescope consisting of a diffractive and refractive doublet that transmits rather than reflects X-rays. Therefore, its angular resolution is relatively insensitive to figure errors and surface roughness, the factors that limit grazing incidence telescopes. When the focal length of the refractive component is minus twice that of the diffractive the chromatic aberration that is inherent in the diffractive and refractive components individually will compensate each other within a limited but not insignificant energy band. We consider a system with a long focal length, about 5000 km, to allow the refractive lens to be thin and transmit X-rays. The long focal length requires very long distance formation flying between an optics spacecraft and a detector spacecraft that must be aligned to better than a few centimeters. Solar orbit is a likely site. We simulate an imaging system where chromatic aberration is corrected to first order at 6 keV. The angular resolution is expected to be better than 0.3 miliarcsec within a 10% bandwidth. The components are lightweight, and can probably be made in a machine shop. Published by Elsevier Ltd on behalf of COSPAR. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM goren@cfa.harvard.edu NR 5 TC 3 Z9 3 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2007 VL 40 IS 8 BP 1276 EP 1280 DI 10.1016/j.asr.2007.06.003 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 268OU UT WOS:000253589900017 ER PT J AU Schlegel, EM Singh, KP Rana, V Barrett, P AF Schlegel, E. M. Singh, K. P. Rana, V. Barrett, P. TI X-ray line emission from cataclysmic variables SO ADVANCES IN SPACE RESEARCH LA English DT Article DE cataclysmic variables; x-ray lines; grating spectra ID INTERMEDIATE POLARS; ACCRETION; ECLIPSES; REGION AB We discuss the X-ray line emission as observed with the HETG on Chandra of a sample of CV spectra. A portion of the data have been fit with global models by Mukai et al. [Mukai, K. et al. Two types of X-ray spectra in cataclysmic variables. ApJ 586, L77-L80, 2003]; we analyze the same spectra using a line-by-line fit. The results are similar to those reported by Mauche et al. on EX Hya, but additionally cover the other CVs. A broad range of temperatures is indicated based on the H/He-like ratio of O, Mg, S, and Fe. (c) 2007 Published by Elsevier Ltd on behalf of COSPAR. C1 [Schlegel, E. M.] Smithsonian Astrophys Observ, Cambridge, MA USA. [Singh, K. P.; Rana, V.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Barrett, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schlegel, E. M.] Univ Texas San Antonio, San Antonio, TX 78249 USA. [Barrett, P.] USN Observ, Washington, DC USA. RP Schlegel, EM (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA. EM eschlegel@cfa.harvard.edu; barrett.paul@usno.navy.mil NR 13 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2007 VL 40 IS 8 BP 1299 EP 1302 DI 10.1016/j.asr.2006.10.024 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 268OU UT WOS:000253589900021 ER PT J AU Ho, WCG Chang, P Kaplan, DL Mori, K Potelchin, AY van Adelsber, M AF Ho, Wynn C. G. Chang, Philip Kaplan, David L. Mori, Kaya Potelchin, Alexander Y. van Adelsber, Matthew TI Modeling atmosphere emission from magnetic neutron stars SO ADVANCES IN SPACE RESEARCH LA English DT Article DE magnetic fields; radiative transfer; stars : atmospheres; stars : magnetic fields; stars : neutron; X-rays : stars ID X-RAY-SPECTRUM; BROAD ABSORPTION FEATURE; EQUATION-OF-STATE; XMM-NEWTON; VACUUM POLARIZATION; THERMAL EMISSION; RX J1856.5-3754; ULTRARELATIVISTIC ELECTRONS; HYDROGEN ATMOSPHERES; CHANDRA OBSERVATIONS AB Since their discovery, neutron stars have been recognized to be unique natural laboratories for helping our understanding of fundamental physics, including nuclear and particle physics and the theory of gravity. The excellent sensitivity of the new X-ray telescopes, e.g., Chandra and XMM-Newton, is ideal for the study of cooling, isolated neutron stars, which emit at these energies. In order to exploit the wealth of information contained in the data, a thorough knowledge of the emission properties of neutron stars is necessary. We describe our work on constructing atmosphere models, which determine the observed spectra from neutron stars. In particular, we discuss the effects of vacuum polarization and bound atoms on the atmosphere structure and spectra. We show that our partially ionized hydrogen atmosphere model spectra can fit the multi-wavelength spectrum of the neutron star RX J 1856.5-3754. On the other hand, mid-Z element atmospheres may fit other isolated neutron stars, such as 1E 1207.4-5209. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Ho, Wynn C. G.; Kaplan, David L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Chang, Philip] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mori, Kaya] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Potelchin, Alexander Y.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [van Adelsber, Matthew] Cornell Univ, Ctr Radiophys & Space Res, Dept Astron, Ithaca, NY 14853 USA. RP Ho, WCG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wynnho@slac.stanford.edu RI Potekhin, Alexander/B-9747-2014 OI Potekhin, Alexander/0000-0001-9955-4684 NR 94 TC 2 Z9 2 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2007 VL 40 IS 10 BP 1432 EP 1440 DI 10.1016/j.asr.2007.04.011 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 268OW UT WOS:000253590100002 ER PT J AU Lorenzini, EC Shapiro, II Glashow, S Cheimets, P Bombardelli, C Iafolla, V Nozzoli, S AF Lorenzini, E. C. Shapiro, I. I. Glashow, S. Cheimets, P. Bombardelli, C. Iafolla, V. Nozzoli, S. TI Advances in the development of the experiment to test the equivalence principle in an Einstein elevator SO ADVANCES IN SPACE RESEARCH LA English DT Article DE equivalence principle; Einstein elevator; stratospheric balloon; fundamental physics AB We describe specific advances in the analysis and development of an experiment to test the Weak Equivalence Principle in free fall inside a capsule (Einstein elevator) released from a stratospheric balloon. The accuracy goal of the experiment is a few parts in 10(15). The attainment of this accuracy would improve the present results in testing the Equivalence Principle by two orders of magnitude. The measurement technique calls for a detector with two sensing masses of different materials, spinning about the detector horizontal axis, to free fall inside the capsule/cryostat for about 25 s. We focus here on the effects on the measurement accuracy of gravity gradients produced by nearby masses, which are non-corotating with the detector. The results of our study on gravity gradients generated by the distributed mass of the capsule/cryostat yield requirements on: (a) the size of the cryostat; (b) the tolerable verticality error of the capsule during the fall; and (c) the centering of the center of masses of the detector's sensing masses. These analyses on the mass distribution of the experiment carrier have moved the project towards viable design options for the capsule/cryostat. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Lorenzini, E. C.; Shapiro, I. I.; Cheimets, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Glashow, S.] Boston Univ, Dept Phys, Boston, MA 02215 USA. [Lorenzini, E. C.; Bombardelli, C.] Univ Padua, Dept Mech Engn, I-35100 Padua, Italy. [Iafolla, V.; Nozzoli, S.] Inst Space Phys, I-00133 Rome, Italy. RP Lorenzini, EC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM enrico.lorenzini@unipd.it OI Iafolla, Valerio Antonio/0000-0001-5297-1157 NR 6 TC 2 Z9 2 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2007 VL 39 IS 2 BP 249 EP 253 DI 10.1016/j.asr.2006.04.021 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 286BV UT WOS:000254821300007 ER PT J AU Bao, XM Zhang, HQ Lin, J Jiang, YC Li, LP AF Bao, Xingming Zhang, Hongqi Lin, Jun Jiang, Yunchun Li, Leping TI Evolution of coronal mass ejections in the early stage SO ADVANCES IN SPACE RESEARCH LA English DT Article DE coronal mass ejections; flare; filament eruption ID FILAMENT ERUPTIONS; FLARES; RECONNECTION AB This work reports the investigation of two coronal mass ejections (CME) observed in white light, H alpha, EUV and X-ray by various instruments both in space and on ground on February 18, 2003 and January 19, 2005, respectively. The white light coronal images show that the first CME began with the rarefaction of a region above the solar limb and was followed by the formation of its leading edge at the boundary of the rarefying region at altitude of 0.46 R-circle dot from the solar surface. The rarefaction coincided the slow rising phase of the filament eruption, and the CME leading edge was observed to form as the filament eruption started to accelerate apparently. In the early stage of the second CME, a bright loop was first observed above the solar limb with height of 0.37 R-circle dot in EUV images. We found that the more gradual CMEs initial process, the larger the timing difference between CMEs and their associated flares. The lower part of the filament brightened in H alpha images as the filament rose to a certain height. These brightenings imply that the filament may be heated by magnetic reconnection below the filament in the early stage of the eruption. We suggest that the possible mechanism which led to the formation of the CME leading edge and cavity is magnetic reconnection which occurred under the filament when it reached a certain height. (c) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bao, Xingming; Zhang, Hongqi] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Lin, Jun; Jiang, Yunchun; Li, Leping] Chinese Acad Sci, NAOC, Yunan Astron Observ, Kunming 650011, Yunnan, Peoples R China. [Lin, Jun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bao, XM (reprint author), Chinese Acad Sci, Natl Astron Observ China, A20 Datun Rd,Chaoyang Dist, Beijing 100012, Peoples R China. EM xbao@bao.ac.cn RI LIN, JUN/B-9890-2017 NR 13 TC 1 Z9 1 U1 1 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2007 VL 39 IS 12 BP 1847 EP 1852 DI 10.1016/j.asr.2007.02.055 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 268OK UT WOS:000253588900008 ER PT B AU Cioffi-Revilla, C Luke, S Parker, DC Rogers, JD Fitzhugh, WW Honeychurch, W Frohlich, B DePriest, P Amartuvshin, C AF Cioffi-Revilla, Claudio Luke, Sean Parker, Dawn C. Rogers, J. Daniel Fitzhugh, William W. Honeychurch, William Frohlich, Bruno DePriest, Paula Amartuvshin, Chunag BE Takahashi, S Scallach, D Rouchier, J TI Agent-based modeling simulation of social adaptation and long-term change in inner Asia SO ADVANCING SOCIAL SIMULATION: THE FIRST WORLD CONGRESS LA English DT Proceedings Paper CT 1st World Congress on Social Simulation CY AUG 21-25, 2006 CL Kyoto Univ, Kyoto, JAPAN SP Toyto Inst Technol HO Kyoto Univ DE computational social science; agent-based modeling; environmental adaptation; political development; social complexity; Inner Asia; MASON toolkit AB We present a new international project to develop temporally and spatially calibrated agent-based models of the rise and fall of polities in Inner Asia (Central Eurasia) in the past 5,000 years. Gaps in theory, data, and computational models for explaining long-term sociopolitical change-both growth and decay-motivate this project. We expect three contributions: (1) new theoretically-grounded simulation models validated and calibrated by the best available data; (2) a new long-term cross-cultural database with several data sets; and (3) new conceptual, theoretical, and methodological contributions for understanding social complexity and long-term change and adaptation in real and artificial societies. Our theoretical framework is based on explaining sociopolitical evolution by the process of "canonical variation". C1 [Cioffi-Revilla, Claudio; Luke, Sean; Parker, Dawn C.; Honeychurch, William] George Mason Univ, Krasnow Inst Adv Study, Ctr Social Complex, Fairfax, VA 22030 USA. [Luke, Sean] George Mason Univ, Volgenau Sch Informat Technol & Engn, Dept Comp Sci, Fairfax, VA 22030 USA. [Rogers, J. Daniel; Fitzhugh, William W.; Honeychurch, William; Frohlich, Bruno; DePriest, Paula] Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA. [Amartuvshin, Chunag] Mongolian Acad Sci, Mongolian Inst Archaeol, Ulanbataar, Mongol Peo Rep. RP Cioffi-Revilla, C (reprint author), George Mason Univ, Krasnow Inst Adv Study, Ctr Social Complex, Fairfax, VA 22030 USA. RI Parker, Dawn/H-3793-2015 FU US National Science Foundation [BCS-0527471] FX This project is funded by the US National Science Foundation grant BCS-0527471. More information is available at http://cs.gmu.edu/-eclab/prqjects/asia/. Thanks to Nigel Gilbert, Scott Moss, Akira Namatame, David Sallach, and two anonymous referees for comments. NR 43 TC 4 Z9 4 U1 0 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-4-431-73150-4 PY 2007 BP 189 EP + DI 10.1007/978-4-431-73167-2_18 PG 3 WC Anthropology; Computer Science, Interdisciplinary Applications; Linguistics; Mathematics, Applied; Social Sciences, Mathematical Methods; Sociology SC Anthropology; Computer Science; Linguistics; Mathematics; Mathematical Methods In Social Sciences; Sociology GA BGQ42 UT WOS:000249739800018 ER PT J AU Coolidgel, RH Hunt, DR AF Coolidgel, R. H. Hunt, D. R. TI Metric evaluation of changes in cadaver stature. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. Amer Museum Nat Hist, Smithsonian Inst, Dept Anthropol, New York, NY 10024 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 90 EP 90 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500134 ER PT J AU Garofalo, EM Zuckerman, MK Ortner, DJ AF Garofalo, E. M. Zuckerman, M. K. Ortner, D. J. TI The incomplete juvenile: cranial vault thickness as an aging technique for juvenile skeletal remains. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Johns Hopkins Univ, Sch Med, Biol Funct Anat & Evolut, Baltimore, MD USA. Emory Univ, Dept Anthropol, Atlanta, GA 30322 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Phys Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 112 EP 113 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500230 ER PT J AU Harris, TR Monfort, SL AF Harris, T. R. Monfort, S. L. TI Evaluating C peptide as a measure of net energy gain in Colobus guereza. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Max Planck Inst Evolutionary Anthropol, Dept Primatol, D-04103 Leipzig, Germany. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 126 EP 126 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500287 ER PT J AU London, MR Jones, EB AF London, Marilyn R. Jones, Erica B. TI A case of maxillo-mandibular and spheno-mandibular ankylosis from Alaska. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Maryland, Dept Anthropol, College Pk, MD 20742 USA. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 158 EP 159 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500428 ER PT J AU Ousley, SD Jantz, RL Freid, D AF Ousley, S. D. Jantz, R. L. Freid, D. TI Exploring Human Craniometric Variation: Statistical, Mensural, Biological, and Historical Considerations. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. NR 0 TC 0 Z9 0 U1 1 U2 5 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 182 EP 182 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500529 ER PT J AU Pearlstein, K Hunt, DR Mann, RW AF Pearlstein, K. Hunt, D. R. Mann, R. W. TI The expression of femoral trochanteric spicules with relation to age. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Div Phys Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 185 EP 185 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500544 ER PT J AU Pobiner, BL DeSilva, J Sanders, WJ Mitani, JC AF Pobiner, Briana L. DeSilva, Jeremy Sanders, William J. Mitani, John C. TI Taphonomy of primate skeletal remains from chimpanzee hunts at Ngogo, Kibale National Park, Uganda. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Michigan, Dept Anthropol, Ann Arbor, MI 48109 USA. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 190 EP 190 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500564 ER PT J AU Potts, R AF Potts, R. TI Environmental dynamics and the evolution of adaptability. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, NMNH, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 192 EP 192 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500572 ER PT J AU Teague, RL Potts, R AF Teague, R. L. Potts, R. TI Faunal and behavioral context of earliest pleistocene Homo in East Asia. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 George Washington Univ, Dept Anthropol, CASHP, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. Smithsonian Inst, Human Origins Program, NMNH, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 230 EP 230 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500736 ER PT J AU Tocheri, MW AF Tocheri, M. W. TI Derived wrist anatomy in the genus Homo as evidenced by 3D quantitative analyses: the implications for understanding the evolution of stone tool behaviors in hominins SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. NR 0 TC 0 Z9 0 U1 2 U2 4 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 232 EP 233 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500748 ER PT J AU Wescott, DJ Cunningham, DL Ubelaker, DH AF Wescott, D. J. Cunningham, D. L. Ubelaker, D. H. TI Growth and development of femur shape, size, and strength among three Native American groups. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Missouri, Dept Anthropol, Columbia, MO 65211 USA. Smithsonian Inst, Dept Anthropol, NMNH, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 247 EP 247 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500812 ER PT J AU Wilczak, CA Mulhern, DM AF Wilczak, C. A. Mulhern, D. M. TI Co-occurrence of DISH and HFI in the terry collection. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Maryland, Dept Anthropol, Coll Pk & Repatriat Osteol Lab, NMNH Smithsonian Inst, College Pk, MD 20742 USA. Ft Lewis Coll, Dept Anthropol, Colorado Springs, CO USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2007 SU 44 BP 249 EP 249 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 142NK UT WOS:000244656500819 ER EF