FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Laurin, M de Queiroz, K Cantino, P Cellinese, N Olmstead, R AF Laurin, M de Queiroz, K Cantino, P Cellinese, N Olmstead, R TI The PhyloCode, types, ranks and monophyly: a response to Pickett SO CLADISTICS LA English DT Article ID PHYLOGENETIC NOMENCLATURE; BIOLOGICAL NOMENCLATURE; TAXONOMY AB A report from the First International Phylogenetic Nomenclature Meeting recently published in Cladistics conveys several misconceptions about the PhyloCode and presents an erroneous interpretation of discussions that took place at that meeting. Contrary to Pickett's assertions, the PhyloCode is designed to name clades, not paraphyletic groups; the rejection of ranks has never been a fundamental principle of phylogenetic nomenclature; and specifiers under the PhyloCode differ in several ways from types under rank-based nomenclature. (C) The Willi Hennig Society 2005. C1 Univ Paris 07, CNRS, FRE 8570, Equipe Format Squelett, F-75005 Paris, France. Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. Yale Univ, Peabody Museum Nat Hist, Bot Div, New Haven, CT 06520 USA. Univ Washington, Dept Biol, Seattle, WA 98195 USA. RP Laurin, M (reprint author), Univ Paris 07, CNRS, FRE 8570, Equipe Format Squelett, Case 7077,2 Pl Jussieu, F-75005 Paris, France. EM laurin@ccr.jussieu.fr RI Laurin, Michel/B-7884-2008; OI Laurin, Michel/0000-0003-2974-9835; Cellinese, Nico/0000-0002-7157-9414 NR 22 TC 15 Z9 17 U1 0 U2 5 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0748-3007 J9 CLADISTICS JI Cladistics PD DEC PY 2005 VL 21 IS 6 BP 605 EP 607 DI 10.1111/j.1096-0031.2005.00090.x PG 3 WC Evolutionary Biology SC Evolutionary Biology GA 995FT UT WOS:000234086900004 ER PT J AU Urashima, T Nakamura, T Ikeda, A Asakuma, S Arai, I Saito, T Oftedal, OT AF Urashima, T Nakamura, T Ikeda, A Asakuma, S Arai, I Saito, T Oftedal, OT TI Characterization of oligosaccharides in milk of a mink, Mustela vison SO COMPARATIVE BIOCHEMISTRY AND PHYSIOLOGY A-MOLECULAR & INTEGRATIVE PHYSIOLOGY LA English DT Article DE mink; Mustela vison; Mustelidae; milk oligosaccharides; neutral oligosaccharides; sialyl oligosaccharides ID CHEMICAL-CHARACTERIZATION; URSUS-AMERICANUS; BLACK BEAR; POLAR BEAR; SAMPLE; GLYCOLIPIDS; CONSTRAINTS AB Carbohydrates were extracted from a sample of milk from a mink, Mustela vison (Family Mustelidae). Free neutral and acidic oligosaccharides were isolated from the carbohydrate fraction and their chemical structures were compared with those of white-nosed coati (Nasua narica, Procyonidae) and harbour seal (Phoca vitulina, Phocidae) that we had studied previously. The ratio of free lactose to milk oligosaccharides was similar to that in milk of the white-nosed coati; in both species, this ratio was much lower than that in the milk of most eutherians. The neutral oligosaccharides of mink milk had alpha(1-3)-linked Gal or alpha(1-2)-linked Fuc residues at their non-reducing ends, as in the neutral oligosaccharides of white-nosed coati milk. Some of the neutral and acidic oligosaccharides, determined here, had been found also in harbour seal milk, but the harbour seal oligosaccharides did not contain alpha(1-3)-linked Gal residues. (C) 2005 Elsevier Inc. All rights reserved. C1 Obihiro Univ Agr & Vet Med, Grad Sch Hood Hydiene, Obihiro, Hokkaido 0808555, Japan. Obihiro Univ Agr & Vet Med, Dept Bio Resource Sci, Obihiro, Hokkaido 0808555, Japan. Tohoku Univ, Dept Bio Prod, Grad Sch Agr, Sendai, Miyagi 9818555, Japan. Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Conservat & Res Ctr, Washington, DC 20008 USA. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Hood Hydiene, Inada Cho, Obihiro, Hokkaido 0808555, Japan. EM urashima@obihiro.ac.jp NR 38 TC 14 Z9 14 U1 0 U2 2 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1095-6433 J9 COMP BIOCHEM PHYS A JI Comp. Biochem. Physiol. A-Mol. Integr. Physiol. PD DEC PY 2005 VL 142 IS 4 BP 461 EP 471 DI 10.1016/j.cbpa.2005.09.015 PG 11 WC Biochemistry & Molecular Biology; Physiology; Zoology SC Biochemistry & Molecular Biology; Physiology; Zoology GA 004HV UT WOS:000234743500012 PM 16289988 ER PT J AU Littler, MM Littler, DS Brooks, BL AF Littler, MM Littler, DS Brooks, BL TI Extraordinary mound building Avrainvillea (Chlorophyta): the largest tropical marine plants SO CORAL REEFS LA English DT Editorial Material C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Littler, MM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, POB 37012 MRC 166, Washington, DC 20013 USA. EM littlerm@si.edu RI Brooks, Barrett/C-5306-2008 NR 3 TC 1 Z9 1 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2005 VL 24 IS 4 BP 555 EP 555 DI 10.1007/s00338-005-0019-z PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 990CK UT WOS:000233720600005 ER PT J AU Ritson-Williams, R Paul, VJ Bonito, V AF Ritson-Williams, R Paul, VJ Bonito, V TI Marine benthic cyanobacteria overgrow coral reef organisms SO CORAL REEFS LA English DT Editorial Material C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Ritson-Williams, R (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM williams@sms.si.edu NR 4 TC 8 Z9 10 U1 2 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2005 VL 24 IS 4 BP 629 EP 629 DI 10.1007/s00338-005-0059-4 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 990CK UT WOS:000233720600017 ER PT J AU Paul, VJ Thacker, RW Banks, K Golubic, S AF Paul, VJ Thacker, RW Banks, K Golubic, S TI Benthic cyanobacterial bloom impacts the reefs of South Florida (Broward County, USA) SO CORAL REEFS LA English DT Article DE cyanobacterial bloom; benthic cyanobacteria; Florida reef tract; Lyngbya ID TROPICAL MARINE CYANOBACTERIA; PHASE-SHIFTS; CORAL-REEF; COMMUNITIES; MACROALGAE; MANAGEMENT; NUTRIENTS; PATTERNS; ECOLOGY; LAGOON AB Benthic cyanobacteria of the genus Lyngbya can form prominent mats and blooms in tropical and subtropical coral reef and seagrass habitats worldwide. A Lyngbya bloom on the reef tract offshore of Broward County, Florida, was first noted in 2002, and although it is seasonally variable in its distribution and abundance, it has persisted and spread over the past 3 years. In this study, the most abundant species of Lyngbya found in the blooms have been identified and compared to other species of Lyngbya by morphological and molecular methods. The most common species of Lyngbya is consistent with the properties of Lyngbya confervoides C. Agardh. The 16S ribosomal DNA sequence shares 88-92% identity with other known Lyngbya sequences, suggesting that this bloom consists primarily of a new, previously unsequenced species of Lyngbya. The second most common Lyngbya in the bloom is consistent with Lyngbya polychroa. This persistent bloom is a concern because it smothers octocorals and other invertebrates and negatively impacts these southeastern Florida reefs. C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. Broward Cty Environm Protect Dept, Ft Lauderdale, FL 33301 USA. Boston Univ, Ctr Biol Sci, Boston, MA 02215 USA. Univ Alabama, Dept Biol, Birmingham, AL 35294 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM Paul@sms.si.edu NR 29 TC 65 Z9 71 U1 0 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2005 VL 24 IS 4 BP 693 EP 697 DI 10.1007/s00338-005-0061-x PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 990CK UT WOS:000233720600024 ER PT J AU Latychev, K Mitrovica, JX Tamisiea, ME Tromp, J Christara, CC Moucha, R AF Latychev, K Mitrovica, JX Tamisiea, ME Tromp, J Christara, CC Moucha, R TI GIA-induced secular variations in the Earth's long wavelength gravity field: Influence of 3-D viscosity variations SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE geopotential harmonics; glacial isostatic adjustment; 3D structure ID GLACIAL ISOSTATIC-ADJUSTMENT; SEA-LEVEL CHANGE; LOWER MANTLE; PLEISTOCENE DEGLACIATION; LITHOSPHERIC THICKNESS; TEMPORAL VARIATIONS; ZONAL HARMONICS; LAGEOS; RHEOLOGY; ACCELERATION AB Predictions of present day secular variations in the Earth's long wavelength geopotential driven by glacial isostatic adjustment (GIA) have previously been analyzed to Infer the radial profile of mantle viscosity and to constrain ongoing cryospheric mass balance. These predictions have been based on spherically symmetric Earth models, We explore the impact of lateral variations in mantle viscosity using a new finite-volume formulation for computing the response of 3-D Maxwell viscoelastic Earth models. The geometry of the viscosity field is constrained from seismic-to-mographic images of mantle structure, while the amplitude of the lateral viscosity variations is tuned by a free parameter in the modeling. We focus IS on the zonal J, harmonics for degrees l =2.,..,8 and demonstrate that large-scale lateral viscosity variations of two to three orders Of magnitude have a modest. 5 10%. impact on predictions Of J(2), In contrast, predictions of higher degree harmonics show a much greater sensitivity to lateral variation in viscosity structure. We conclude that future analyses of secular trends (for degree l 2) estimated front ongoing (GRACE, CHAMP) satellite missions must incorporate GIA predictions based on 3-D viscoelastic Earth models. (C) 2005 Elsevier B.V. All rights reserved. C1 Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Seismol Lab, Pasadena, CA 91125 USA. Univ Toronto, Dept Comp Sci, Toronto, ON M5S 3G4, Canada. RP Latychev, K (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM latychev@physics.utoronto.ca RI Tromp, Jeroen/B-6185-2015 OI Tromp, Jeroen/0000-0002-2742-8299 NR 34 TC 3 Z9 3 U1 2 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC 1 PY 2005 VL 240 IS 2 BP 322 EP 327 DI 10.1016/j.epsl.2005.10.001 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 000NX UT WOS:000234470100011 ER PT J AU Neubauer, SC Givler, K Valentine, SK Megonigal, JP AF Neubauer, SC Givler, K Valentine, SK Megonigal, JP TI Seasonal patterns and plant-mediated controls of subsurface wetland biogeochemistry SO ECOLOGY LA English DT Article DE anaerobic metabolism; iron reduction; methanogenesis; Patuxent River; Maryland; sulfate reduction; tidal brackish marsh; tidal freshwater marsh ID SALT-MARSH SEDIMENTS; ORGANIC-CARBON OXIDATION; FRESH-WATER ECOSYSTEMS; SULFATE REDUCTION; METHANE PRODUCTION; PADDY SOIL; ROOT-ZONE; IRON; MANGANESE; RATES AB In tidal marshes, spatial and temporal variability in the importance of microbial metabolic pathways influences ecosystem-level processes such as soil carbon storage, the regeneration of inorganic nutrients, and the production of atmospherically important trace gases. We measured seasonal changes in rates of microbial Fe(III) reduction, sulfate reduction, and methanogenesis in tidal freshwater and brackish marshes on the Patuxent River, Maryland, USA, and assessed the ability of plant roots to influence these processes by regenerating electron acceptors and supplying electron donors. In both marshes, the importance of microbial Fe(III) reduction was greatest early in the summer and decreased through the study period. Coincident with the seasonal decline in Fe(III) reduction, methanogenesis (freshwater marsh) or sulfate reduction (brackish site) increased in importance. At the brackish marsh, the partitioning of anaerobic carbon metabolism between Fe(III) reduction and sulfate reduction was similar within and below the root zone, suggesting that rhizosphere processes did not control anaerobic metabolism at this site. Instead, seasonal biogeochemical patterns at the brackish marsh were affected by factors such as water table depth and iron-sulfur interactions. At the tidal freshwater site, our results suggest that changes in rates of Fe(III) reduction and methanogenesis were directly affected by plantmediated processes. In midsummer, Fe(III) reduction accounted for a greater fraction of total anaerobic metabolism in rhizosphere-influenced surface soils than in soils below the root zone. High rates of Fe(III) reduction occurred at the expense of methanogenesis. This study documented strong temporal variations in the outcome of microbial competition for electron donors that ultimately affected the balance between Fe(III) reduction and methanogenesis within tidal freshwater marsh soils. Our data suggested that variations in microbial metabolic pathways were regulated by physiochemical factors at the brackish site and plant activity at the freshwater site. Plant regulation of Fe(III) reduction is a largely unstudied mechanism by which plants influence wetland carbon cycling and greenhouse gas production. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Villanova Univ, Dept Biol, Villanova, PA 19085 USA. Warren Wilson Coll, Asheville, NC 28815 USA. RP Neubauer, SC (reprint author), Baruch Marine Field Lab, POB 1630, Georgetown, SC 29442 USA. EM scott@belle.baruch.sc.edu RI Neubauer, Scott/A-3443-2011 OI Neubauer, Scott/0000-0001-8948-2832 NR 47 TC 85 Z9 88 U1 9 U2 67 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 DEC PY 2005 VL 86 IS 12 BP 3334 EP 3344 DI 10.1890/04-1951 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 994YI UT WOS:000234066700025 ER PT J AU deRivera, CE Ruiz, GM Hines, AH Jivoff, P AF deRivera, CE Ruiz, GM Hines, AH Jivoff, P TI Biotic resistance to invasion: Native predator limits abundance and distribution of an introduced crab SO ECOLOGY LA English DT Article DE biological invasion; biotic resistance; blue crab; Callinectes sapidus; Carcinus maenas; European green crab; geographic range; nonindigenous species; predation ID JUVENILE BLUE CRABS; CHESAPEAKE-BAY; CALLINECTES-SAPIDUS; CARCINUS-MAENAS; SHALLOW-WATER; PREY INTERACTIONS; RANGE LIMITS; SHORE CRAB; MARINE; REFUGE AB Introduced species frequently escape the natural enemies (predators, competitors, and parasites) that limit their distribution and abundance in the native range. This reduction in native predators, competitors, and parasites may result in ecological release in the introduced range. However, biological interactions also can limit the establishment and spread of normative populations. The extent to which such biotic resistance occurs is poorly resolved., especially for marine ecosystems. Here we test whether a native predator, the blue crab Callinectes sapidus, affects the abundance and geographic range of the introduced European green crab Carcinus maenas in eastern North America. Both crab species occur in shallow, soft-sediment habitats of bays and estuaries, and their ranges overlap in eastern North America. First, we tested for a negative relationship in the abundances of the two species from trap samples across a 640-km (5.78 degrees latitude) coastal transect. Second, we estimated variation in predation pressure on tethered Carcinus maenas across latitude and as a function of Callinectes sapidus abundance. Third, we measured predation rates on Carcinus maenas by Callinectes sapidus in field and laboratory experiments. Our results support the hypothesis that the native predator Callinectes sapidus provides biotic resistance to invasion and prevents the southward spread and establishment of Carcinus maenas. Within and across bays, Carcinus maenas were significantly less abundant at sites and depths with Callinectes sapidus compared with areas lacking Callinectes sapidus. Moreover, no Carcinus maenas were found in Chesapeake Bay, where Callinectes sapidus were most abundant. Predation of tethered Carcinus maenas increased with Callinectes sapidus abundance. In laboratory and field experiments, Callinectes sapidus preyed readily on Carcinus maenas. Thus, we conclude the predation by Callinectes sapidus, alone or in combination with other factors, limits the abundance and geographic range of an invasive marine species. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Rider Univ, Dept Biol, Lawrenceville, NJ 08648 USA. RP deRivera, CE (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM deriverac@si.edu OI Ruiz, Gregory/0000-0003-2499-441X NR 65 TC 138 Z9 144 U1 9 U2 93 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 DEC PY 2005 VL 86 IS 12 BP 3364 EP 3376 DI 10.1890/05-0479 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 994YI UT WOS:000234066700028 ER PT J AU Carney, KM Matson, PA AF Carney, KM Matson, PA TI Plant communities, soil microorganisms, and soil carbon cycling: Does altering the world belowground matter to ecosystem functioning? SO ECOSYSTEMS LA English DT Article DE biodiversity; microbial community; carbon cycling; decomposition; enzyme activity; PLFA; catabolic potential; tropics; La Selva Biological Station ID PHOSPHOLIPID FATTY-ACID; SUBSTRATE UTILIZATION PATTERNS; MICROBIAL COMMUNITIES; BACTERIAL COMMUNITIES; CATABOLIC DIVERSITY; TROPICAL SOIL; BIODIVERSITY; DECOMPOSITION; BIOMASS; LITTER AB Soil microorganisms mediate many critical ecosystem processes. Little is known, however, about the factors that determine soil microbial community composition, and whether microbial community composition influences process rates. Here, we investigated whether aboveground plant diversity affects soil microbial community composition, and whether differences in microbial communities in turn affect ecosystem process rates. Using an experimental system at La Selva Biological Station, Costa Rica, we found that plant diversity (plots contained 1, 3, 5, or > 25 plant species) had a significant effect on microbial community composition (as determined by phospholipid fatty acid analysis). The different microbial communities had significantly different respiration responses to 24 labile carbon compounds. We then tested whether these differences in microbial composition and catabolic capabilities were indicative of the ability of distinct microbial communities to decompose different types of litter in a fully factorial laboratory litter transplant experiment. Both microbial biomass and microbial community composition appeared to play a role in litter decomposition rates. Our work suggests, however, that the more important mechanism through which changes in plant diversity affect soil microbial communities and their carbon cycling activities may be through alterations in their abundance rather than their community composition. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Stanford Univ, Dept Geog & Environm Sci, Stanford, CA 94305 USA. RP Carney, KM (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM karen.carney@gmail.com NR 66 TC 83 Z9 93 U1 4 U2 58 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 J9 ECOSYSTEMS JI Ecosystems PD DEC PY 2005 VL 8 IS 8 BP 928 EP 940 DI 10.1007/s10021-005-0047-0 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 992HC UT WOS:000233874000005 ER PT J AU Leimgruber, P Kelly, DS Steininger, MK Brunner, J Muller, T Songer, M AF Leimgruber, P Kelly, DS Steininger, MK Brunner, J Muller, T Songer, M TI Forest cover change patterns in Myanmar (Burma) 1990-2000 SO ENVIRONMENTAL CONSERVATION LA English DT Article DE biodiversity; change detection; deforestation rates; forest; forest dynamics; Landsat ID DEER CERVUS-ELDI; TROPICAL DEFORESTATION; CONSERVATION; HABITAT; AMAZON; AREA AB Myanmar is one of the most forested countries in mainland South-cast Asia. These forests support a large number of important species and endemics and have great value for global efforts in biodiversity conservation. Landsat satellite imagery from the 1990s and 2000s was used to develop a countrywide forest map and estimate deforestation. The country has retained much of its forest cover, but forests have declined by 0.3% annually. Deforestation varied considerably among administrative units, with central and more populated states and divisions showing the highest losses. Ten deforestation hotspots had annual deforestation rates well above the countrywide average. Major reasons for forest losses in these hotspots stemmed from increased agricultural conversion, fuelwood consumption, charcoal production, commercial logging and plantation development. While Myanmar continues to be a stronghold for closed canopy forests, several areas have been experiencing serious deforestation. Most notable are the mangrove forests in the Ayeyarwady delta region and the remaining dry forests at the northern edge of the central dry zone. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Conservat Int, Washington, DC 20036 USA. RP Leimgruber, P (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. EM leimgruberp@crc.si.edu RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 NR 33 TC 44 Z9 46 U1 5 U2 34 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0376-8929 J9 ENVIRON CONSERV JI Environ. Conserv. PD DEC PY 2005 VL 32 IS 4 BP 356 EP 364 DI 10.1017/S0376892905002493 PG 9 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 053NJ UT WOS:000238311500010 ER PT J AU Rearick, MS Gilmour, CC Heyes, A Mason, RP AF Rearick, MS Gilmour, CC Heyes, A Mason, RP TI Measuring sulfide accumulation in diffusive gradients in thin films by means of purge and trap followed by ion-selective electrode SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Article DE sulfide; ill situ; diffusive gradients; thin films; ion-selective electrode ID ACID-VOLATILE SULFIDE; DISSOLVED SULFIDE; NATURAL-WATERS; IN-SITU; HYDROGEN-SULFIDE; SIMULTANEOUS RELEASE; GAS-CHROMATOGRAPHY; SULFUR SPECIATION; METHYLENE-BLUE; PORE WATERS AB A procedure for measuring ill Situ Sulfide Concentrations by Coupling diffusive gradients in thin films (DGT) to solid-state ion-selective electrodes (ISE) is described and evaluated. Laboratory tests were performed to evaluate the coupling of these techniques, and these results were compared to the previously used methods of computer imaging densitometry (CID)and methylene blue. An average elution efficiency, of 89%, as detected by ISE, was determined for a series of solutions containing amounts of Sulfide ranging from 0.009 to 2.50 mu mol. The validity of the standard mass-transfer equation for sulfide accumulation by DGT probes and subsequent detection by ISE was tested by measuring the mass of sulfide collected over time and with respect to varying diffusive gel thicknesses. Regressions of the sulfide mass accumulation versus the independent variables of time and inverse diffusive thickness proved to be linear. The use of DGT coupled to ISE provides it preconcentration method for sulfide that improves the detection limit (DL) over other techniques. This alternative method provides quantitative measurements of DGT-captured Sulfide from solutions with a detection limit of at least 0.1 mu mol/L for a 24-h deployment. The DGT technique also provides potential advantages ill understanding sulfide speciation over existing methods. C1 Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Mason, RP (reprint author), Univ Connecticut, Dept Marine Sci, 1080 Shennecossett Rd, Groton, CT 06340 USA. EM robert.mason@uconn.edu RI Heyes, Andrew/E-5269-2012; Mason, Robert/A-6829-2011; Gilmour, Cynthia/G-1784-2010 OI Gilmour, Cynthia/0000-0002-1720-9498 NR 30 TC 5 Z9 5 U1 0 U2 9 PU SETAC PI PENSACOLA PA 1010 NORTH 12TH AVE, PENSACOLA, FL 32501-3367 USA SN 0730-7268 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD DEC PY 2005 VL 24 IS 12 BP 3043 EP 3047 DI 10.1897/05-061R.1 PG 5 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA 989ZU UT WOS:000233713700006 PM 16445083 ER PT J AU Freyberg, MJ Brauninger, H Burkert, W Hartner, GD Citterio, O Mazzoleni, F Pareschi, G Spiga, D Romaine, S Gorenstein, P Ramsey, BD AF Freyberg, M. J. Braeuninger, H. Burkert, W. Hartner, G. D. Citterio, O. Mazzoleni, F. Pareschi, G. Spiga, D. Romaine, S. Gorenstein, P. Ramsey, B. D. TI The MPE X-ray test facility PANTER: Calibration of hard X-ray (15-50 kev) optics SO EXPERIMENTAL ASTRONOMY LA English DT Article; Proceedings Paper CT Workshop on Focusing Telescopes in Nuclear Astrophysics CY SEP 12-15, 2005 CL Bonifacio, FRANCE DE X-ray astronomy; X-ray telescopes; X-ray optics; X-ray detectors; multilayers; calibration ID XMM-NEWTON; PERFORMANCE; ASTRONOMY; DESIGN; TELESCOPES; ROSAT AB The Max-Planck-Institut fur extraterrestrische Physik (MPE) in Garching, Get-many, uses its large X-ray beam line facility PANTER for testing X-ray astronomical instrumentation. A number of telescopes, gratings, filters, and detectors, e.g. for astronomical satellite missions like Exosat, ROSAT, Chandra (LETG), BeppoSAX, SOHO (CDS), XMM-Newton, ABRIXAS, Swift (XRT), have been successfully calibrated in the soft X-ray energy range (< 15keV). Moreover, measurements with mirror test samples for new missions like ROSITA and XEUS have been carried out at PANTER. Here we report on an extension of the energy range, enabling calibrations of hard X-ray optics over the energy range 15-50 keV. Several future X-ray astronomy missions (e.g., Simbol-X, Constellation-X, XEUS) have been proposed, which make use of hard X-ray optics based on multilayer coatings. Such optics are currently being developed by the Osservatorio Astronomico di Brera (OAB), Milano. Italy, and the Harvard-Smithsonian Center for Astrophysics (CIA), Cambridge, MA, USA. These optics have been tested at the PANTER facility with a broad energy band beam (up to 50 keV) using the XMM-Newton EPIC-pn flight spare CCD camera with its good intrinsic energy resolution, and also with monochromatic X-rays between C-K (0.277 keV) and Cu-K alpha (8.04 keV). C1 Max Planck Inst Extraterr Phys, PANTER Xray Test Facil, D-82061 Neuried, Germany. INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, MSFC, Dept Space Sci, Huntsville, AL 35812 USA. RP Freyberg, MJ (reprint author), Max Planck Inst Extraterr Phys, PANTER Xray Test Facil, Gautinger Str 45, D-82061 Neuried, Germany. EM mjf@mpe.mpg.de OI Spiga, Daniele/0000-0003-1163-7843; Pareschi, Giovanni/0000-0003-3967-403X NR 16 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2005 VL 20 IS 1-3 BP 407 EP 414 DI 10.1007/s10686-006-9068-8 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 126RD UT WOS:000243531600041 ER PT J AU Alto, BW Yanoviak, SP Lounibos, LP Drake, BG AF Alto, BW Yanoviak, SP Lounibos, LP Drake, BG TI Effects of elevated atmospheric CO2 on water chemistry and mosquito (Diptera : Culicidae) growth under competitive conditions in container habitats SO FLORIDA ENTOMOLOGIST LA English DT Article DE global change; freshwater; Aedes albopictus; larval competition; population growth parameters ID AEDES-ALBOPICTUS DIPTERA; LEAF-LITTER; LARVAL COMPETITION; TRISERIATUS DIPTERA; TREEHOLE MOSQUITO; CARBON-DIOXIDE; QUALITY; DECOMPOSITION; DETRITUS; ECOSYSTEM AB We investigated the direct and indirect effects of elevated atmospheric CO2 on freshwater container habitats and their larval mosquito occupants. We predicted that a-doubling of atmospheric CO2 would (1) alter the chemical properties of water in this system, (2) slow degradation of leaf litter, and (3) decrease larval growth of Aedes albopictus (Skuse) mosquitoes raised on that litter under competitive conditions. Effects of elevated CO2 on water quality parameters were not detected, but the presence of leaf litter significantly reduced pH and dissolved oxygen relative to water-filled containers without litter. Degradation rates of oak leaf litter from plants grown under elevated CO2 atmospheres did not differ from breakdown rates of litter from ambient CO2 conditions. Litter from plants grown in an elevated CO2 atmospheres did not influence mosquito population growth, but mosquito production decreased significantly with increasing larval density. Differences among mosquito density treatments influenced survivorship most strongly among male Ae. albopictus and time to emergence most strongly among females, suggesting fundamental sex-determined differences in response to competition. Results of this and other studies indicate that direct and indirect effects of doubled atmospheric CO2 are minimal in artificial containers with freshwater. C1 Univ Florida, Florida Med Entomol Lab, Vero Beach, FL 32962 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Alto, BW (reprint author), Univ Florida, Florida Med Entomol Lab, 200 9th St SE, Vero Beach, FL 32962 USA. FU NIAID NIH HHS [R01 AI044793-04, R01 AI044793, R01 AI044793-03, R01 AI044793-01, R01 AI044793-02] NR 64 TC 4 Z9 4 U1 0 U2 5 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 DEC PY 2005 VL 88 IS 4 BP 372 EP 382 DI 10.1653/0015-4040(2005)88[372:EOEACO]2.0.CO;2 PG 11 WC Entomology SC Entomology GA 006WP UT WOS:000234928700004 PM 22661767 ER PT J AU Sephton, MA Looy, CV Brinkhuis, H Wignall, PB de Leeuw, JW Visscher, H AF Sephton, MA Looy, CV Brinkhuis, H Wignall, PB de Leeuw, JW Visscher, H TI Catastrophic soil erosion during the end-Permian biotic crisis SO GEOLOGY LA English DT Article DE Permian-Triassic boundary; ecological crisis; mass extinction; carbon isotope; polysaccharide; soil erosion ID PEAT-FORMING PLANTS; CARBON-ISOTOPE; TRIASSIC BOUNDARY; MASS EXTINCTIONS; SOUTH-AFRICA; DEAD ZONE; BASIN; SULFUR; AUSTRALIA; EVENT AB Organic geochemical analyses of sedimentary organic matter from a marine Permian-Triassic transition sequence in northeastern Italy reveal a significant influx of land-derived diagenetic products of polysaccharides. This unique event reflects massive soil erosion resulting from destruction of land vegetation due to volcanogenic disturbance of atmospheric chemistry. The excessive supply of soil materials to the oceans provides a direct link between terrestrial and marine ecological crises, suggesting that ecosystem collapse on land could have contributed to the end-Permian marine extinctions. C1 Univ London Imperial Coll Sci Technol & Med, Impacts & Astromat Res Ctr, Dept Earth Sci & Engn, London SW7 2AZ, England. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Utrecht, Dept Palaeoecol, Palaeobot & Palynol Lab, NL-3584 CD Utrecht, Netherlands. Univ Leeds, Sch Earth Sci, Leeds LS2 9JT, W Yorkshire, England. Royal Netherlands Inst Sea Res, Dept Marine Biogeochem & Toxicol, NL-1790 AB Den Burg, Netherlands. RP Sephton, MA (reprint author), Univ London Imperial Coll Sci Technol & Med, Impacts & Astromat Res Ctr, Dept Earth Sci & Engn, S Kensington Campus, London SW7 2AZ, England. EM m.a.sephton@imperial.ac.uk; looy.cindy@nmnh.si.edu; h.brinkhuis@bio.uu.nl; p.wignall@earth.leeds.ac.uk; deleeuw@nioz.nl; h.visscher@bio.uu.nl RI Brinkhuis, Henk/B-4223-2009; de Leeuw, Jan/F-6471-2011; OI Sephton, Mark/0000-0002-2190-5402 NR 43 TC 130 Z9 137 U1 3 U2 31 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD DEC PY 2005 VL 33 IS 12 BP 941 EP 944 DI 10.1130/G2178.1 PG 4 WC Geology SC Geology GA 991XV UT WOS:000233849100006 ER PT J AU Erwin, DH AF Erwin, DH TI Out of the past and into the future SO GEOTIMES LA English DT News Item C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Santa Fe Inst, Santa Fe, NM 87501 USA. RP Erwin, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM erwind@si.edu RI Erwin, Douglas/A-9668-2009 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 USA SN 0016-8556 J9 GEOTIMES JI Geotimes PD DEC PY 2005 VL 50 IS 12 BP 32 EP 34 PG 3 WC Geosciences, Multidisciplinary SC Geology GA 990TO UT WOS:000233766300034 ER PT J AU Erickson, D AF Erickson, D TI Quantitative trait loci - Mapping the future of QTL's SO HEREDITY LA English DT Editorial Material ID GENETIC ARCHITECTURE; EPISTASIS C1 Smithsonian Inst, Labs Analyt Biol, Washington, DC 20560 USA. RP Erickson, D (reprint author), Smithsonian Inst, Labs Analyt Biol, Washington, DC 20560 USA. EM de51@umail.umd.edu NR 9 TC 8 Z9 10 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0018-067X J9 HEREDITY JI Heredity PD DEC PY 2005 VL 95 IS 6 BP 417 EP 418 DI 10.1038/sj.hdy.6800699 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 986QD UT WOS:000233463900001 PM 16222331 ER PT J AU Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Demleitner, M Henneken, E Murray, SS AF Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Demleitner, M Henneken, E Murray, SS TI The effect of use and access on citations SO INFORMATION PROCESSING & MANAGEMENT LA English DT Article DE open access; document use; citation analysis ID ASTROPHYSICS DATA SYSTEM; IMPACT AB It has been shown (Lawrence, S. (2001). Online or invisible? Nature, 411, 52 1) that journal articles which have been posted without charge on the internet are more heavily cited than those which have not been. Using data from the NASA Astrophysics Data System (ads.harvard.edu) and from the ArXiv e-print archive at Cornell University (arXiv.org) we examine the causes of this effect. (c) 2005 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden ST, Cambridge, MA 01238 USA. EM kurtz@cfa.harvard.edu RI Eichhorn, Guenther/C-9480-2009; Henneken, Edwin/F-9475-2010; KURTZ, Michael /B-3890-2009; OI Eichhorn, Guenther/0000-0002-3032-1978; Henneken, Edwin/0000-0003-4264-2450; Kurtz, Michael/0000-0002-6949-0090; Accomazzi, Alberto/0000-0002-4110-3511; Grant, Carolyn/0000-0003-4424-7366 NR 22 TC 76 Z9 76 U1 1 U2 19 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0306-4573 EI 1873-5371 J9 INFORM PROCESS MANAG JI Inf. Process. Manage. PD DEC PY 2005 VL 41 IS 6 BP 1395 EP 1402 DI 10.1016/j.ipm.2005.03.010 PG 8 WC Computer Science, Information Systems; Information Science & Library Science SC Computer Science; Information Science & Library Science GA 956XE UT WOS:000231332600007 ER PT J AU Christy, JH Rissanen Jr Backwell, PRY AF Christy, JH Rissanen, JR Backwell, PRY TI A one-day pause in the biweekly courtship cycle of atropical fiddler crab allows females to avoid releasing larvae during twilight SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2006 CL Orlando, FL C1 Australian Natl Univ, Canberra, ACT, Australia. Smithsonian Trop Res Inst, Balboa, Panama. EM christyj@si.edu NR 0 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2005 VL 45 IS 6 BP 977 EP 977 PG 1 WC Zoology SC Zoology GA 012KH UT WOS:000235337600091 ER PT J AU Koepfli, KP Gompper, ME Eizirik, E Ho, CC Linden, L Maldonado, JE Wayne, RK AF Koepfli, KP Gompper, ME Eizirik, E Ho, CC Linden, L Maldonado, JE Wayne, RK TI Molecular phylogeny reveals extensive morphological parallelism in the Procyonidae (mamimalia : carnivora) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2006 CL Orlando, FL C1 Univ Calif Los Angeles, Los Angeles, CA USA. Univ Missouri, Columbia, MO USA. Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. EM klausk@lifesci.ucla.edu RI Eizirik, Eduardo/K-8034-2012 OI Eizirik, Eduardo/0000-0002-9658-0999 NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2005 VL 45 IS 6 BP 1028 EP 1028 PG 1 WC Zoology SC Zoology GA 012KH UT WOS:000235337600294 ER PT J AU Schulze, A Cutler, EB Giribet, G AF Schulze, A Cutler, EB Giribet, G TI Molecular and morphological evolution in sipunculan worms SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2006 CL Orlando, FL C1 Harvard Univ, Smithsonian Marine Stn, Cambridge, MA 02138 USA. EM schulze@sms.si.edu NR 0 TC 1 Z9 1 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2005 VL 45 IS 6 BP 1070 EP 1070 PG 1 WC Zoology SC Zoology GA 012KH UT WOS:000235337600462 ER PT J AU Diaz, MC Thacker, RW Collin, R AF Diaz, MC Thacker, RW Collin, R TI Taxonomy and ecology of Caribbean sponges: Effective training for new investigators SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2006 CL Orlando, FL C1 Museum Natl Hist Nat, Washington, DC USA. Univ Alabama, Birmingham, AL USA. Smithsonian Trop Res Inst, Balboa, Panama. EM thacker@uab.edu RI Collin, Rachel/G-2001-2010 NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2005 VL 45 IS 6 BP 1124 EP 1124 PG 1 WC Zoology SC Zoology GA 012KH UT WOS:000235337601156 ER PT J AU Mah, CL AF Mah, CL TI A new species of Xyloplax (Echinodermata; Asteroidea; Concentricycloidea) from the Northeast Pacific: Comparative morphology and a reassessment of Concentricycloid phylogeny SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2006 CL Orlando, FL C1 Smithsonian Inst, Washington, DC 20560 USA. EM brisinga@gmail.com RI Mah, Christopher/B-5771-2008 NR 0 TC 0 Z9 0 U1 1 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2005 VL 45 IS 6 BP 1162 EP 1162 PG 1 WC Zoology SC Zoology GA 012KH UT WOS:000235337601306 ER PT J AU Santagata, S AF Santagata, S TI The significance of neuromuscular anatomy and metamorphosis in the larval and juvenile body plans of phoronids and brachiopods SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2006 CL Orlando, FL C1 Smithsonian Marine Stn, Ft Pierce, FL USA. Univ Washington, Friday Harbor Labs, Seattle, WA 98195 USA. EM scott_santagata@hotmail.com NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2005 VL 45 IS 6 BP 1188 EP 1188 PG 1 WC Zoology SC Zoology GA 012KH UT WOS:000235337601413 ER PT J AU Crouch, TD AF Crouch, Tom D. TI Sky as frontier: Adventure, aviation, and empire. 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 DEC PY 2005 VL 92 IS 3 BP 1030 EP 1031 PG 2 WC History SC History GA 082JI UT WOS:000240382300104 ER PT J AU Hooper, E Legendre, P Condit, R AF Hooper, E Legendre, P Condit, R TI Barriers to forest regeneration of deforested and abandoned land in Panama SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE abandoned agriculture; natural regeneration; old-field succession; Saccharum spontaneum; secondary succession; seed dispersal; tropical forest ID EARLY PLANT SUCCESSION; MONTANE RAIN-FOREST; SEED RAIN; EASTERN AMAZONIA; TREE ESTABLISHMENT; TROPICAL PASTURE; PUERTO-RICO; COSTA-RICA; SOIL; VEGETATION AB 1. In Panama, abandoned agricultural lands that supported tropical rain forest are invaded by the exotic invasive grass Saccharum spontaneum, which precludes native forest regeneration. This study aimed to evaluate the importance of several barriers to forest regeneration and highlight mitigation opportunities. 2. We examined four barriers to natural regeneration: Saccharum competition, seed dispersal limitation, fire and soil nutrient deficiency. Tree and shrub regeneration was measured in a factorial experiment combining Saccharum cutting treatments, distances from adjacent forest and a prescribed burn to assess the first three barriers, respectively. We compared soil nutrients in Saccharum plots with those from adjacent forest. Additionally, we determined the importance of distance to remnant vegetation (large-leaved monocots, shrubs and isolated trees) on forest regeneration. 3. Fire significantly decreased plant species richness of forest regeneration. Fire inhibited the germination of most species; the effect was exacerbated by cutting the Saccharum. 4. Grass competition significantly decreased seedling growth, while soil nutrient deficiency did not affect forest regeneration. 5. Seed dispersal limitation affected density and species richness. Significantly more species (3x) regenerated at 10 m compared with 35 m from the forest. Mean seedling densities were, respectively, four, three and two times higher under large-leaved monocots, isolated trees and shrubs than in open Saccharum. When seed input was experimentally equalized, large-seeded species had the highest establishment rate, suggesting that if their propagules were dispersed to the site they would regenerate in high proportions. However, under natural conditions they regenerated poorly and represented the most dispersal-limited species group. 6. Synthesis and applications. Our results suggest that facilitation of natural regeneration may be a feasible, low-cost management option for restoring native forest cover to large areas. Firebreaks must be established to promote biodiversity of forest regeneration. We do not recommend Saccharum cutting or fertilization as site treatments. Shading effectively eliminates Saccharum. Planting a variety of tree species in clumps throughout the Saccharum may overcome dispersal limitations and catalyse natural regeneration. Trees that attract different frugivores are recommended, especially large-seeded forest species. C1 Univ Montreal, Dept Sci Biol, Lab Pierre Legendre, Montreal, PQ H3C 3J7, Canada. McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. RP Hooper, E (reprint author), Univ Montreal, Dept Sci Biol, Lab Pierre Legendre, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM ehoope1@uic.edu NR 53 TC 88 Z9 100 U1 8 U2 55 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD DEC PY 2005 VL 42 IS 6 BP 1165 EP 1174 DI 10.1111/j.1365-2664.2005.01106.x PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 987JW UT WOS:000233515200017 ER PT J AU Santra, R Kirby, K AF Santra, R Kirby, K TI Ab initio configuration-interaction investigation of optical transitions in K+He and K+H-2 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MOLECULAR-ORBITAL METHODS; TRANSMISSION SPECTRA; LINE-PROFILES; T-DWARFS; ATOMS; SPECTROSCOPY; ATMOSPHERES; WAVELENGTHS; LIFETIME; SYSTEMS AB The potassium resonance line (4s -> 4p) centered around 770 nm is a major contributor to the optical extinction in the atmospheres of certain classes of brown dwarfs and extrasolar giant planets. The resonance line is significantly broadened by collisions with He and H-2, and an accurate calculation of the line profile is needed for astrophysical models of these objects. As a first step, we report an accurate ab initio study of the K+He and K+H-2 potential-energy curves correlating to the K 4s and 4p atomic energy levels, together with the dipole moments governing the transitions between these potential-energy curves. The molecular calculations have been carried out using a multireference configuration-interaction method, with the molecular orbitals expanded in a large Gaussian basis set. The transition dipole moments show significant variation with the molecular geometry. Calculations for the K+H-2 system have been carried out for a range of H-2 orientations and internuclear separations, so that the effect of H-2 rotation and vibration may be explicitly included in future calculations of the pressure-broadened line profiles. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Santra, R (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA. RI Santra, Robin/E-8332-2014 OI Santra, Robin/0000-0002-1442-9815 NR 26 TC 19 Z9 19 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 1 PY 2005 VL 123 IS 21 AR 214309 DI 10.1063/1.2107648 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 991PB UT WOS:000233824800023 PM 16356050 ER PT J AU Stark, G Huber, KP Yoshino, K Smith, PL Ito, K AF Stark, G Huber, KP Yoshino, K Smith, PL Ito, K TI Oscillator strength and linewidth measurements of dipole-allowed transitions in N-14(2) between 93.5 and 99.5 nm SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID HIGH-RESOLUTION ABSORPTION; VUV SPECTROSCOPIC FACILITY; TITANS UPPER-ATMOSPHERE; MOLECULAR NITROGEN; CROSS-SECTIONS; LIFETIME MEASUREMENTS; ULTRAVIOLET EMISSION; C'(4) (1)SIGMA(U)(+); LASER SPECTROSCOPY; ELECTRON-IMPACT AB Line oscillator strengths in 16 electric dipole-allowed bands of N-14(2) in the 93.5-99.5 nm (106 950-100 500 cm(-1)) region have been measured at an instrumental resolution of 6.5x10(-4) nm (0.7 cm(-1)). The transitions terminate on vibrational levels of the 3p sigma (1)Sigma(u)(+), 3p pi (1)Pi(u), and 3s sigma (1)Pi(u) Rydberg states and of the b(') (1)Sigma(u)(+) and b (1)Pi(u) valence states. The J dependences of band f values derived from the experimental line f values are reported as polynomials in J(')(J(')+1) and are extrapolated to J(')=0 in order to facilitate comparisons with results of coupled-Schrodinger-equation calculations that do not take into account rotational interactions. Most bands in this study reveal a marked J dependence of the f values and/or display anomalous P-, Q- and R-branch intensity patterns. These patterns should help inform future spectroscopic models that incorporate rotational effects, and these are critical for the construction of realistic atmospheric radiative transfer models. Linewidth measurements are reported for four bands. Information provided by the J dependences of the experimental linewidths should be of use in the development of a more complete understanding of the predissociation mechanisms in N-2. C1 Wellesley Coll, Dept Phys, Wellesley, MA 02481 USA. Natl Res Council Canada, Steacie Inst Mol Sci, Ottawa, ON K1A 0R6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. High Energy Accelerator Res Org, Photon Factory, Inst Mat Struct Sci, Tsukuba, Ibaraki 305080, Japan. RP Stark, G (reprint author), Wellesley Coll, Dept Phys, Wellesley, MA 02481 USA. EM gstark@wellesley.edu NR 62 TC 45 Z9 45 U1 1 U2 9 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 1 PY 2005 VL 123 IS 21 AR 214303 DI 10.1063/1.2134703 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 991PB UT WOS:000233824800017 PM 16356044 ER PT J AU Farris, HE Rand, AS Ryan, MJ AF Farris, HE Rand, AS Ryan, MJ TI The effects of time, space and spectrum on auditory grouping in tungara frogs SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE cocktail party effect; auditory stream; auditory scene analysis; complex call; mate choice; chorus; phonotaxis; amphibian; frog; tungara; Physalaemus pustulosus ID PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; SENSORY EXPLOITATION; STREAM SEGREGATION; 2-TONE SUPPRESSION; NEOTROPICAL FROG; CALL COMPONENTS; TONE SEQUENCES; COMPLEX CALLS; FREQUENCY AB Male tungara frogs (Physalaemus pustulosits) produce complex calls consisting of two components, a similar to 350 ms FM sweep called the "whine" followed by up to seven 40 ms harmonic bursts called "chucks". In order to choose and locate a calling male, females attending to choruses must group call components into auditory streams to correctly assign calls to their sources. Previously we showed that spatial cues play a limited role in grouping: calls with normal spectra and temporal structure are grouped over wide angular separations ( <= 135 degrees). In this study we again use phonotaxis to first test whether an alternative cue, the sequence of call components, plays a role in auditory grouping and second, whether grouping is mediated by peripheral or central mechanisms. We found that while grouping is not limited to the natural call sequence, it does vary with the relative onset times of the two calls. To test whether overlapping stimulation in the periphery is required for grouping, the whine and chuck were filtered to restrict their spectra to the sensitivity ranges of the amphibian and basilar papillae, respectively. For these dichotic-like stimuli, grouping still occurred (albeit only to 45 degrees separation), suggesting that stream formation is mediated by central mechanisms. C1 Univ Texas, Sect Integrat Biol C0930, Austin, TX 78712 USA. Louisiana State Univ, Hlth Sci Ctr, Ctr Neurosci, New Orleans, LA 70112 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Farris, HE (reprint author), Univ Texas, Sect Integrat Biol C0930, 1 Univ Stn, Austin, TX 78712 USA. EM Hfarri@lsuhsc.edu NR 41 TC 24 Z9 24 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0340-7594 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD DEC PY 2005 VL 191 IS 12 BP 1173 EP 1183 DI 10.1007/s00359-005-0041-1 PG 11 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA 996YE UT WOS:000234211400011 PM 16088388 ER PT J AU Rothman, LS Jacquemart, D Barbe, A Benner, DC Birk, M Brown, LR Carleer, MR Chackerian, C Chance, K Coudert, LH Dana, V Devi, VM Flaud, JM Gamache, RR Goldman, A Hartmann, JM Jucks, KW Maki, AG Mandin, JY Massie, ST Orphal, J Perrin, A Rinsland, CP Smith, MAH Tennyson, J Tolchenov, RN Toth, RA Vander Auwera, J Varanasi, P Wagner, G AF Rothman, LS Jacquemart, D Barbe, A Benner, DC Birk, M Brown, LR Carleer, MR Chackerian, C Chance, K Coudert, LH Dana, V Devi, VM Flaud, JM Gamache, RR Goldman, A Hartmann, JM Jucks, KW Maki, AG Mandin, JY Massie, ST Orphal, J Perrin, A Rinsland, CP Smith, MAH Tennyson, J Tolchenov, RN Toth, RA Vander Auwera, J Varanasi, P Wagner, G TI The HITRAN 2004 molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT 8th Biennial HITRAN Database Conference CY JUN 16-18, 2004 CL Harvard Smithsonian Ctr Astrophys, Cambridge, MA HO Harvard Smithsonian Ctr Astrophys DE HITRAN; spectroscopic database; molecular spectroscopy; molecular absorption; line parameters; absorption cross-sections; aerosols ID SELF-BROADENING COEFFICIENTS; ABSOLUTE LINE-INTENSITIES; FOURIER-TRANSFORM SPECTROSCOPY; ABSORPTION CROSS-SECTIONS; DIODE-LASER SPECTROSCOPY; FAR-INFRARED SPECTRUM; MULTISPECTRUM FITTING PROCEDURE; PRESSURE-SHIFT COEFFICIENTS; EFFECTIVE DIPOLE-MOMENT; MU-M REGION AB This paper describes the status of the 2004 edition of the HITRAN molecular spectroscopic database. The HITRAN compilation consists of several components that serve as input for radiative transfer calculation codes: individual line parameters for the microwave through visible spectra of molecules in the gas phase; absorption cross-sections for molecules having dense spectral features, i.e., spectra in which the individual lines are unresolvable; individual line parameters and absorption cross-sections for bands in the ultra-violet; refractive indices of aerosols; tables and files of general properties associated with the database; and database management software. The line-by-line portion of the database contains spectroscopic parameters for 39 molecules including many of their isotopologues. The format of the section of the database on individual line parameters of HITRAN has undergone the most extensive enhancement in almost two decades. It now lists the Einstein A-coefficients, statistical weights of the upper and lower levels of the transitions, a better system for the representation of quantum identifications, and enhanced referencing and uncertainty codes. In addition, there is a provision for making corrections to the broadening of line transitions due to line mixing. (C) 2005 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. DLR, Remote Sensing Technol Inst, Wessling, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Free Univ Brussels, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Paris 11, Photophys Mol Lab, F-91405 Orsay, France. Univ Paris 06, Lab Phys Mol & Applicat, F-75252 Paris, France. Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. Harvard Smithsonian Ctr Astrophys, Opt & Infrared Astron Div, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. UCL, Dept Phys & Astron, London WC1E 6BT, England. SUNY Stony Brook, Stony Brook, NY 11794 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu RI Tennyson, Jonathan/I-2222-2012; Orphal, Johannes/A-8667-2012; OI Tennyson, Jonathan/0000-0002-4994-5238; Orphal, Johannes/0000-0002-1943-4496; Rothman, Laurence/0000-0002-3837-4847; Chance, Kelly/0000-0002-7339-7577 NR 210 TC 2058 Z9 2154 U1 16 U2 155 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC 1 PY 2005 VL 96 IS 2 BP 139 EP 204 DI 10.1016/j.jqsrt.2004.10.008 PG 66 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 956MG UT WOS:000231303400002 ER PT J AU Jacquemart, D Gamache, R Rothman, LS AF Jacquemart, D Gamache, R Rothman, LS TI Semi-empirical calculation of air-broadened half-widths and air pressure-induced frequency shifts of water-vapor absorption lines SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT 8th Biennial HITRAN Database Conference CY JUN 16-18, 2004 CL Harvard Smithsonian Ctr Astrophys, Cambridge, MA HO Harvard Smithsonian Ctr Astrophys DE water-vapor absorption; air-broadened half-width; air pressure-induced line shift; line shape ID ROBERT-BONAMY FORMALISM; MU-M; PARAMETERS; REGION; H2O; CM(-1); (H2O)-O-16; NITROGEN AB This paper describes a semi-empirical calculation of the air-broadened half-widths and the air pressure induced frequency shifts for the (H2O)-O-16 isotopologue. This semi-empirical calculation is based on fits of several recent high-quality measurements and theoretical calculations to the first-order terms in the expansion of the complex Robert-Bonamy (CRB) equations, which yields a second- and first-order polynomial function of the differences in the upper- and lower-state vibrational quantum numbers for the half-width and line shift, respectively. The aim of this work was to obtain a complete set of air-broadened half-widths and air pressure-induced frequency shifts for transitions of (H2O)-O-16 present in the HITRAN database from microwave to the visible in order to supplement the observed and calculated values. For around 700 sets of rotational quantum numbers (J'K'K-c' <- J '' K-a'' K-c''), semi-empirical coefficients describing the vibrational dependence of the air-broadened half-widths and the air pressure-induced frequency shifts have been obtained directly from the fit of experimental and/or theoretical data. The accuracy of the parameters deduced from this calculation is estimated to be between 5% and 10% for the air-broadened half-widths and between 0.001 and 0.01 cm(-') aim(-') for the air pressure-induced frequency shifts. For sets of rotational quantum numbers for which either none or insufficient experimental/theoretical data were available to deduce a vibrational dependence, further approximations have been used to obtain a complete set of semi-empirical coefficients. (C) 2005 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 28 TC 26 Z9 27 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC 1 PY 2005 VL 96 IS 2 BP 205 EP 239 DI 10.1016/j.jqsrt.2004.11.018 PG 35 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 956MG UT WOS:000231303400003 ER PT J AU Ubelaker, DH AF Ubelaker, DH TI A companion to the anthropology of American Indians. SO JOURNAL OF THE ROYAL ANTHROPOLOGICAL INSTITUTE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROYAL ANTHROPOLOGICAL INST PI LONDON PA 50 FITZROY STREET, LONDON W1P 5HS, ENGLAND SN 1359-0987 J9 J ROY ANTHROPOL INST JI J. R. Anthropol. Inst. PD DEC PY 2005 VL 11 IS 4 BP 871 EP 871 PG 1 WC Anthropology SC Anthropology GA 987TU UT WOS:000233541000043 ER PT J AU Nascimento, HEM Laurance, WF Condit, R Laurance, SG D'Angelo, S Andrade, AC AF Nascimento, HEM Laurance, WF Condit, R Laurance, SG D'Angelo, S Andrade, AC TI Demographic and life-history correlates for Amazonian trees SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Amazon; growth; mortality; rain forest; recruitment; tree guild; tree life history; wood density ID TROPICAL RAIN-FOREST; NEOTROPICAL FOREST; BRAZILIAN AMAZON; LANDSCAPE-SCALE; WOOD DENSITY; DIVERSITY; GROWTH; MORTALITY; DYNAMICS; BIOMASS AB Questions: Which demographic and life-history differences are found among 95 sympatric tree species? Are there correlations among demographic parameters within this assemblage? Location: Central Amazonian rain forest. Methods: Using long-term data from 24 1-ha permanent plots, eight characteristics were estimated for each species: wood density, annual mortality rate, annual recruitment rate, mean stem diameter, maximum stem diameter, mean stem-growth rate, maximum stem-growth rate, population density. Results: An ordination analysis revealed that tree characteristics varied along two major axes of variation, the major gradient expressing light requirements and successional status, and the second gradient related to tree size. Along these gradients, four relatively discrete tree guilds could be distinguished: fast-growing pioneer species, shade-tolerant subcanopy species, canopy trees, and emergent species. Pioneers were uncommon and most trees were canopy or emergent species, which frequently had low mortality and recruitment. Wood density was negatively associated with tree mortality, recruitment, and growth rates when all species were considered. Growth rates varied markedly among and within species, with pioneers exhibiting far faster and less variable growth rates than did the other species. Slow growth in subcanopy species relative to canopy and emergent trees was not a simple consequence of mean tree size, but apparently resulted from physiological constraints imposed by low-light and other conditions in the forest understorey. Conclusions: Trees of Amazonian rain forests could be classified with some success into four relatively distinctive guilds. However, several demographic and life-history traits, such as those that distinguish early and late successional species, probably vary along a continuum, rather than being naturally grouped into relatively discrete categories. C1 Smithsonian Trop Res Inst, Balboa, Panama. Natl Inst Amazonian Res, BDFFP, BR-69011970 Manaus, Amazonas, Brazil. RP Nascimento, HEM (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM henrique@inpa.gov.br; laurancew@si.edu; condit@ctfs.si.edu; laurances@si.edu; sammya@inpa.gov.br; titina@inpa.gov.br RI Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012; Laurance, Susan/G-6021-2011 OI Laurance, Susan/0000-0002-2831-2933 NR 51 TC 39 Z9 40 U1 0 U2 14 PU OPULUS PRESS UPPSALA AB PI GRANGARDE PA GAMLA VAGEN 40, S-770 13 GRANGARDE, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD DEC PY 2005 VL 16 IS 6 BP 625 EP 634 DI 10.1111/j.1654-1103.2005.tb02405.x PG 10 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 000IK UT WOS:000234454500003 ER PT J AU Deem, SL Noss, AJ Cuellar, RL Karesh, WB AF Deem, SL Noss, AJ Cuellar, RL Karesh, WB TI Health evaluation of free-ranging and captive blue-fronted Amazon parrots (Amazona aestiva) in the Gran Chaco, Bolivia SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Amazona aestiva; Bolivia; hematology; plasma chemistry; psittacine; serology ID HEMATOZOA; PERU AB Bolivia has a total of 47 species of Psittacidae, seven of which have been identified in our study site, the semiarid Gran Chaco of the Isoso. One species, the blue-fronted parrot (Amazona aestiva), is frequently captured by local Isoseno Guaranf Indians for exploitation on the national and international market. These birds are often temporarily housed in small villages under unhygienic conditions with poultry and other domestic species. On occasion, these parrots escape back to the wild. Additionally, many of these birds are kept as pets or are used to lure wild par-rots within slingshot range for subsequent capture. In this study, we evaluated the health status, including the level of exposure to selected infectious agents, in the wild-caught captive birds and free-ranging birds. Physical examinations were performed, and blood was collected, from 54 live birds (20 captive and 34 free-ranging). Feces were collected from 15 birds (seven captive and eight free-ranging). Necropsies were also performed on four recently dead wildcaught birds. On serologic testing, no birds were found to have antibodies to avian influenza virus, Chlamydophila psittaci, infectious bronchitis virus, infectious bursal disease virus, infectious laryngotracheitis virus, Marek's disease virus, paramyxovirus-1, paramyxovirus-2, paramyxovirus-3, polyomavirus, eastern equine encephalitis virus, western equine encephalitis virus, or Venezuelan equine encephalitis virus. Positive antibody titers were found for psittacine herpesvirus (8/44, 18.2%), Aspergillus spp. (3/51, 5.9%), and Salmonella pullorum (33/49, 67.3%). All three of the birds that tested antibody positive for Aspergillus spp. were captive, whereas six of the eight and 15 of the 33 birds that tested positive for psittacine herpesvirus and S. pullorum, respectively, were wild. C1 Wildlife Conservat Soc, Field Vet Program, Bronx, NY 10460 USA. WCS Bolivia, Santa Cruz, Bolivia. RP Deem, SL (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. NR 18 TC 23 Z9 25 U1 5 U2 18 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 2005 VL 36 IS 4 BP 598 EP 605 DI 10.1638/04094.1 PG 8 WC Veterinary Sciences SC Veterinary Sciences GA 029VV UT WOS:000236593400004 PM 17312715 ER PT J AU Napier, JE Murray, S Garner, MM Viner, T Murphy, H AF Napier, JE Murray, S Garner, MM Viner, T Murphy, H TI Uterine leiomyomas in three captive eastern bongo (Tragelaphus eurycerus isaaci) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Eastern bongo; Tragelaphus eurycerus isaaci; leiomyoma; neoplasia; cervix; uterus AB Uterine leiomyomas occurred in three eastern bongo (Tragelaphus eurycerus isaaci) 10. 15, and 16 yr of age at three separate zoological institutions. Two animals were nulliparous, and one had given birth to 14 calves over its lifetime. Two of the leiomyomas originated in the cervix. The third originated in the uterine wall and incorporated the body of the uterus and both uterine horns. The tumors in the two animals that had never calved were large and nonresectable. They were associated with gastrointestinal clinical signs including diarrhea, anorexia, and the inability to defecate. The tumor in the animal that had calved was an incidental finding at necropsy. Uterine leiomyomas have not been previously documented in the literature on eastern bongo. C1 Smithsonian Natl Zoo Pk, Washington, DC 20008 USA. NW ZooPath, Monroe, WA 98272 USA. Zoo New England, Boston, MA 02121 USA. RP Napier, JE (reprint author), Potawatomi Zoo, 500 S Greenlawn Ave, South Bend, IN 46615 USA. NR 9 TC 1 Z9 1 U1 0 U2 3 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 2005 VL 36 IS 4 BP 709 EP 711 DI 10.1638/04114.1 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA 029VV UT WOS:000236593400021 PM 17312732 ER PT J AU Bronson, E Deem, SL Sanchez, C Murray, S AF Bronson, E Deem, SL Sanchez, C Murray, S TI Placental retention in a golden lion tamarin (Leontopithecus rosalia) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE golden lion tamarin; Leontopithecus rosalia; placental retention AB A 4-yr-old female golden lion tamarin (Leontopithecus rosalia) had placental retention after delivery of a stillborn fetus. Conservative therapy with oxytocin and dinoprost tromethamine did not result ill placental expulsion and ovariohysterectomy was performed. Placental retention is a rare condition in humans and has not been well documented in non-human primates. C1 Smithsonian Natl Zool Pk, Washington, DC 20008 USA. RP Bronson, E (reprint author), Smithsonian Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 9 TC 4 Z9 4 U1 0 U2 2 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 2005 VL 36 IS 4 BP 716 EP 718 DI 10.1638/04096.1 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA 029VV UT WOS:000236593400023 PM 17312734 ER PT J AU Perry, L AF Perry, L TI Reassessing the traditional interpretation of "Manioc" artifacts in the Orinoco Valley of Venezuela SO LATIN AMERICAN ANTIQUITY LA English DT Article ID STONE TOOL FUNCTION; STARCH GRAINS; REMAINS; PERU; CULTIVATION; REVEAL; PLANT; CLUES AB There exists general consensus in the archaeological literature that bitter maniac was a staple crop in precontact agricultural systems in the lowlands of South America. This view is based upon the indirect evidence derived from archaeological ceramic and lithic assemblages rather than archaeobotanical evidence, the preserved remains of bitter maniac itself. Studies of microlithic "manioc " grater flakes from Pozo Azul Norte-1, a site located in the middle Orinoco valley of Venezuela, reveal a much more complex function of these artifacts involving the processing of several starchy roots including arrow root, guapo, yam, and ginger; as well as seeds including maize and possibly palm. The starch and use-wear data collected in these investigations indicate that archaeobotanical data are a more reliable means of assessing the function of these tools than are ethnographic analogues. C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Lab, Dept Anthropol, Washington, DC 20013 USA. RP Perry, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Lab, Dept Anthropol, MRC 112,POB 37012, Washington, DC 20013 USA. EM perryli@si.edu NR 67 TC 23 Z9 23 U1 0 U2 7 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 DEC PY 2005 VL 16 IS 4 BP 409 EP 426 PG 18 WC Archaeology SC Archaeology GA 001QJ UT WOS:000234551100003 ER PT J AU Schroll, S AF Schroll, S TI Anselm Kiefer: Heaven and earth. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Schroll, S (reprint author), Smithsonian Inst Libs, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD DEC PY 2005 VL 130 IS 20 BP 124 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 992ZX UT WOS:000233923600163 ER PT J AU Fiertz, C Cooper, SK Flanders, J Johnson, J LaPointe, T Oremland, M AF Fiertz, C Cooper, SK Flanders, J Johnson, J LaPointe, T Oremland, M TI Smithsonian's Ocean Science Initiative: a partnership between the National Museum of Natural History (NMNH) and the National Oceanic and Atmospheric Administration (NOAA) SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article AB The Smithsonian's National Museum of Natural History is launching an Ocean Science Initiative (OSI), which includes an Ocean Web Portal, a Center for Ocean Science, and its centerpiece-the nation's largest permanent Ocean Hall exhibit to open in the fall of 2008. NMNH is the most visited natural history museum in the world. Its dynamic team of research and exhibit staff, and unparalleled collections, in combination with NOAA!s knowledge and expertise in ocean science, provides the opportunity to develop a truly unique exhibit, Web portal and other supporting educational programs. This paper focuses on the partnership, the Hall, its development process, and evolving education and Web portal plans. C1 Natl Museum Nat Hist, Smithsonian, Washington, DC 20560 USA. NOAA, Washington, DC USA. RP Fiertz, C (reprint author), Natl Museum Nat Hist, Smithsonian, Washington, DC 20560 USA. EM fiertzc@si.edu NR 3 TC 0 Z9 0 U1 0 U2 2 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD WIN PY 2005 VL 39 IS 4 BP 105 EP 110 PG 6 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 027ZA UT WOS:000236453700018 ER PT J AU Ortega, J Young, S Simons, LH Maldonado, JE AF Ortega, J Young, S Simons, LH Maldonado, JE TI Characterization of six microsatellite DNA loci for Sorex arizonae SO MOLECULAR ECOLOGY NOTES LA English DT Article DE heterozygosity; microsatellites; polymorphic loci; rare species; Sorex arizonae ID SHREW AB Sorex arizonae is a rare species that occupies a narrow range of habitat types in several mountain ranges of New Mexico, Arizona and Northern Mexico. Here we identify and characterize six microsatellite loci for this species. We screened 63 individuals from four different localities from New Mexico and Arizona to analyse genetic variability. Alleles ranged from three to 16. Heterozygosity ranged from 40% to 78%. Most polymorphic loci were in Hardy-Weinberg equilibrium with the exception of one locus. Primers appear to have reasonable cross-species applicability as five loci amplified in another shrew species (Sorex monticolus). C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Lab, Washington, DC 20008 USA. USDA, Forest Serv, Shasta Trinity Nat Recreat Area, Reddingf, CA 96003 USA. RP Ortega, J (reprint author), Univ Nacl Autonoma Mexico, Lab Macroecol, Dept Ecol Biodivers, Inst Ecol, Circuito Exterior Junto Jardin Bot,Ciudad Univ,Ap, Mexico City 04510, DF, Mexico. EM artibeus2@aol.com RI Young, Sarah/E-2883-2014 OI Young, Sarah/0000-0002-8301-5106 NR 7 TC 1 Z9 2 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD DEC PY 2005 VL 5 IS 4 BP 851 EP 853 DI 10.1111/j.1471-8286.2005.01086.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 994SJ UT WOS:000234051200043 ER PT J AU Volkov, I Banavar, JR He, FL Hubbell, SP Maritan, A AF Volkov, I Banavar, JR He, FL Hubbell, SP Maritan, A TI Density dependence explains tree species abundance and diversity in tropical forests SO NATURE LA English DT Article ID NEUTRAL BIODIVERSITY; COEXISTENCE; COMMUNITIES; DISTANCE; ECOLOGY; NUMBER AB The recurrent patterns in the commonness and rarity of species in ecological communities - the relative species abundance - have puzzled ecologists for more than half a century(1,2). Here we show that the framework of the current neutral theory in ecology(3 - 10) can easily be generalized to incorporate symmetric density dependence(11 - 14). We can calculate precisely the strength of the rare- species advantage that is needed to explain a given RSA distribution. Previously, we demonstrated that a mechanism of dispersal limitation also fits RSA data well(3,4). Here we compare fits of the dispersal and density- dependence mechanisms for empirical RSA data on tree species in six New and Old World tropical forests and show that both mechanisms offer sufficient and independent explanations. We suggest that RSA data cannot by themselves be used to discriminate among these explanations of RSA patterns(15) - empirical studies will be required to determine whether RSA patterns are due to one or the other mechanism, or to some combination of both. C1 Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. RP Banavar, JR (reprint author), Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. EM banavar@psu.edu; maritan@pd.infn.it NR 24 TC 158 Z9 180 U1 12 U2 93 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 1 PY 2005 VL 438 IS 7068 BP 658 EP 661 DI 10.1038/nature04030 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 988JY UT WOS:000233593100048 PM 16319890 ER PT J AU Akkurt, H Groves, JL Trombka, J Starr, R Evans, L Floyd, S Hoover, R Lim, L McClanahan, T James, R McCoy, T Schweitzer, J AF Akkurt, H Groves, JL Trombka, J Starr, R Evans, L Floyd, S Hoover, R Lim, L McClanahan, T James, R McCoy, T Schweitzer, J TI Pulsed neutron generator system for astrobiological and geochemical exploration of planetary bodies SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 18th International Conference on Application of Accelerators in Research and Industry (CAARI) CY OCT 10-15, 2004 CL Ft Worth, TX SP US DOE, Natl Sci Fdn, Int Atom Energy Agcy, Natl Canc Inst, Sadia Natl Lab, Oak Ridge Natl Lab, Oak Ridge Associated Univ, Los Alamos Natl Lab, Synergy Vaccum, Ft Worth Convent & Vistors Bureau, Elsevier B V, Univ N Texas DE neutron generator; subsurface elemental composition; planetary surveys AB A pulsed neutron/gamma-ray detection system for use on rovers to survey the elemental concentrations of Martian and Lunar surface and subsurface materials is evaluated. A robotic survey system combining a pulsed neutron generator (PNG) and detectors (gamma ray and neutron) can measure the major constituents to a depth of about 30 cm. Scanning mode measurements can give the major elemental concentrations while the rover is moving; analyzing mode measurements can give a detailed elemental analysis of the adjacent material when the rover is stationary. A detailed map of the subsurface elemental concentrations will provide invaluable information relevant to some of the most fundamental astrobiological questions including the presence of water, biogenic activity, life habitability and deposition processes. (c) 2005 Elsevier B.V. All rights reserved. C1 Schlumberger Princeton Technol Ctr, Princeton Jct, NJ 07605 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. Comp Sci Corp, Lanham, MD 20706 USA. Brookhaven Natl Lab, Upton, NY 11973 USA. Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. Univ Connecticut, Storrs, CT 06269 USA. RP Groves, JL (reprint author), Schlumberger Princeton Technol Ctr, 20 Wallace Rd, Princeton Jct, NJ 07605 USA. EM groves@princeton.oilfield.slb.com RI McClanahan, Timothy/C-8164-2012; Lim, Lucy/C-9557-2012 OI Lim, Lucy/0000-0002-9696-9654 NR 7 TC 6 Z9 6 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD DEC PY 2005 VL 241 IS 1-4 BP 232 EP 237 DI 10.1016/j.nimb.2005.07.029 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 997PX UT WOS:000234260000052 ER PT J AU Gahn, FJ Baumiller, TK AF Gahn, FJ Baumiller, TK TI Arm regeneration in Mississippian crinoids: evidence of intense predation pressure in the Paleozoic? SO PALEOBIOLOGY LA English DT Article ID GREAT-BARRIER-REEF; MESOZOIC MARINE REVOLUTION; COMATULID CRINOIDS; ECHINODERMATA; ORDOVICIAN; AUSTRALIA; SURVIVAL; FOSSIL; ISLAND; FAUNA AB Although direct predator-prey interactions are unobservable in the fossil record, predation has been used to explain many evolutionary trends. Evidence of predation supporting such hypotheses is often presented as isolated instances of preserved sublethal damage, and less commonly, as the frequency of such injuries. For instance, numerous morphological and ecological trends and innovations observed in Phanerozoic crinoids have been causally, linked to predation, and whereas the high frequency of arm regeneration in living crinoids is generally assumed to represent intense predation, attempts to assess regeneration frequency and patterns in paleontological samples are few. Can the frequency of fossil injuries be assessed to test hypothesized predation-driven trends, or are such data unavailable? To address this question, we analyzed regeneration in crinoids from the lower Mississippian (Kinderhookian) Maynes Creek Formation near Le Grand, Iowa, a locality renowned for the preservation of thousands of crinoids in tangled masses of crowns, stalks, and holdfasts. Nine percent of the specimens that we examined contained at least one regenerating arm; however, whereas Some species lacked evidence of regeneration, others preserved up to 27% arm regeneration. Furthermore, we observed specimens with all arms regenerating, multiple adjacent arms regenerating from the same place along the arm, and a specimen with a damaged and regenerated primaxil and anal sac. The highest regeneration frequency was observed in the most abundant species, Rhodocrinites : kirbyi, a significantly higher value than expected under a model of no taxonomic selectivity (binomial: p < 0.05). Furthermore, bootstrapped simulations of the probable number of regenerated individuals suggest that the number of regenerated arms observed in our sample is two to three times less than what existed in the living population. Rhodocrinites kirbyi constituted over 40% of the individuals in the Le Grand crinoid fauna and had the longest stalk of the studied Species. In addition, regeneration in R. kirbyi is size related, with individuals above median dorsal cup height (7 mm) displaying nearly 50% regeneration, and smaller individuals only 2% (a statistically significant difference; chi(2) test: p < 0.001). The regeneration patterns in R. kirbyi are consistent with predatory attacks that target the most apparent prey. Moreover, this study suggests that predation is the most likely explanation for the regeneration patterns observed in Le Grand crinoids, and that the fossil record potentially provides a valuable, yet overlooked, data source for testing hypotheses pertinent to the role of predation in the evolution of Phanerozoic marine life. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. RP Gahn, FJ (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. EM gahn.forest@nmnh.si.edu; tomaszb@umich.edu RI Baumiller, Tomasz/C-3596-2012 NR 71 TC 19 Z9 20 U1 0 U2 4 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD WIN PY 2005 VL 31 IS 1 BP 151 EP 164 DI 10.1666/0094-8373(2005)031<0151:ARIMCE>2.0.CO;2 PG 14 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 887NT UT WOS:000226313500010 ER PT J AU Gingerich, O AF Gingerich, O TI Researching The 'Book Nobody Read': The 'De revolutionibus' of Nicolaus Copernicus SO PAPERS OF THE BIBLIOGRAPHICAL SOCIETY OF AMERICA LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ginger@cfa.harvard.edu NR 29 TC 4 Z9 4 U1 1 U2 2 PU BIBLIOGRAPHICAL SOC AMER PI NEW YORK PA PO BOX 1537 LENOX HILL STATION, NEW YORK, NY 10021 USA SN 0006-128X J9 PAP BIBLIOGR SOC AM JI Pap. Bibliogra. Soc. Am. PD DEC PY 2005 VL 99 IS 4 BP 484 EP 504 PG 21 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 997UM UT WOS:000234274300001 PM 19637422 ER PT J AU Gutierrez, M Capson, TL Guzman, HM Gonzalez, J Ortega-Barria, E Quinoa, E Riguera, R AF Gutierrez, M Capson, TL Guzman, HM Gonzalez, J Ortega-Barria, E Quinoa, E Riguera, R TI Antiprotozoal activity against Plasmodium falciparum and Trypanosoma cruzi of aeroplysinin-1 isolated from the new sponge Aplysina chiriquensis SO PHARMACEUTICAL BIOLOGY LA English DT Article DE aeroplysinin-1; antimalarial; antitrypanosomal; Aplysina chiriquensis; Aplysina gerardogreeni; dibromotyrosines; Plasmodium falciparum; Trypanosoma cruzi ID MARINE NATURAL-PRODUCTS; PARASITES; MALARIA; DRUGS AB Crude methanol extracts from the recently discovered sponge, Aplysina chiriquensis and Aplysina gerardogreeni, collected at the southwest Pacific Coast of Panama, showed moderate antiplasmodial activity. Fractionation of the crude extracts from A. chiriquensis led to the isolation of the known dibromotyrosine derivatives 1-5. Compound 3, aeroplysinin-1, displayed antiprotozoal activity against chloroquine-resistant Plasmodium falciparum and Trypanosoma cruzi. Comparative analysis by HPLC of the five specimens collected showed the presence of the same metabolites but in different relative proportions. Compounds 1-5 are reported for the first time as constituents of A. chiriquensis and A. gerardogreeni. This is the first report of the antiprotozoal activity of aeroplysinin-1 (3). C1 Univ Santiago de Compostela, Fac Quim, Dept Quim Organ, Inst Acuicultura, Santiago De Compostela 15782, Spain. Univ Santiago de Compostela, CSIC, Unidad RMN Biomol Asociada, Santiago De Compostela, Spain. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Secretariat Sci & Technol, Inst Adv Sci Invest & High Technol Serv, Clayton, Panama. RP Capson, TL (reprint author), Univ Santiago de Compostela, Fac Quim, Dept Quim Organ, Inst Acuicultura, Santiago De Compostela 15782, Spain. EM capsont@si.edu; ricardo@usc.es RI Quinoa, Emilio/D-8920-2011; Riguera, Ricardo/I-6476-2015 OI Quinoa, Emilio/0000-0003-3019-3408; Riguera, Ricardo/0000-0001-5133-0454 NR 19 TC 11 Z9 12 U1 0 U2 3 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1388-0209 J9 PHARM BIOL JI Pharm. Biol. PD DEC PY 2005 VL 43 IS 9 BP 762 EP 765 DI 10.1080/13880200500406503 PG 4 WC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy SC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy GA 011YI UT WOS:000235305000006 ER PT J AU Gordon, A Santra, R Kartner, FX AF Gordon, A Santra, R Kartner, FX TI Role of the Coulomb singularity in high-order harmonic generation SO PHYSICAL REVIEW A LA English DT Article ID INTENSE LASER FIELDS; MULTIPHOTON IONIZATION; RARE-GASES; X-RAYS; ATOMS; PULSES; RADIATION; REGIME AB High-order harmonic generation (HHG) from a single hydrogen atom is studied analytically and numerically in the regime of small Keldysh parameter. The HHG spectra from different Coulomb-like model potentials, such as soft-core and/or one-dimensional (1D) potentials are compared to the three-dimensional (3D) Coulomb potential. It is shown, using analytic arguments, that the famous plateau in the HHG spectrum owes its existence to the Coulomb singularity, whereas soft-core potentials give spectra that fall off exponentially with increasing frequency. The idea is demonstrated numerically on a 3D soft-core potential that has the same long-range asymptotic behavior and ground-state energy as hydrogen. In addition, a number of widely used 1D Coulomb-like potentials are discussed. It is shown that in order that a 1D potential be a reasonable substitute for the 3D Coulomb potential, it must have a cusp singularity. A specific potential satisfying this criterion is proposed. C1 MIT, Dept Elect Engn & Comp Sci, Cambridge, MA 02139 USA. MIT, Elect Res Lab, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP MIT, Dept Elect Engn & Comp Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Santra, Robin/E-8332-2014 OI Santra, Robin/0000-0002-1442-9815 NR 37 TC 20 Z9 21 U1 0 U2 1 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 DEC PY 2005 VL 72 IS 6 AR 063411 DI 10.1103/PhysRevA.72.063411 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 998QU UT WOS:000234334900102 ER PT J AU Anderson, JD AF Anderson, JD TI Ludwig Prandtl's bounyary layer SO PHYSICS TODAY LA English DT Article C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. Univ Maryland, College Pk, MD 20742 USA. RP Anderson, JD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 12 TC 24 Z9 24 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD DEC PY 2005 VL 58 IS 12 BP 42 EP 48 DI 10.1063/1.2169443 PG 7 WC Physics, Multidisciplinary SC Physics GA 987UF UT WOS:000233542100025 ER PT J AU Langley, JA Johnson, NC Koch, GW AF Langley, JA Johnson, NC Koch, GW TI Mycorrhizal status influences the rate but not the temperature sensitivity of soil respiration SO PLANT AND SOIL LA English DT Article DE arbuscular mycorrhiza; autotrophic; heterotrophic; soil respiration; sunflower ID ROOT RESPIRATION; CARBON; FOREST; DECOMPOSITION; NITROGEN; Q(10); RHIZOSPHERE; VEGETATION; CLIMATE; FUNGI AB Mycorrhizal fungi, which can produce a large portion of total soil respiration, respond strongly to global changes such as elevated CO2, N-deposition, and land-use change. Predictions of future ecosystem C sequestration hinge on respiration budgets, but the mycorrhizal influence on total soil respiration remains unknown. In this study, sunflowers (Helianthus annuus) were subjected to various mycorrhizal treatments, and their root and soil systems were enclosed in chambers that continuously monitored belowground (root + mycorrhizal + heterotrophic) CO2 production during plant growth, death, and decomposition. Rhizocosms with high mycorrhizal colonization exhibited higher soil respiration rates as plants matured, an increase that was in proportion to the mycorrhizal stimulation of plant growth. Living mycorrhizal plants behaved like nonmycorrhizal ones in that total rhizocosm respiration had the same relationship to plant mass and the same temperature sensitivity as nonmycorrhizal plants. Upon removal of the shoots though, mycorrhizal plants exhibited the largest relative reduction in respiration resulting in a unique relationship of soil respiration with plant mass. The mycorrhizal influence on heterotrophic respiration merits as much attention from experimenters and modelers as the mycorrhizal contribution to autotrophic respiration. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. No Arizona Univ, Dept Sci Biol, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. RP Langley, JA (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM langleya@si.edu NR 35 TC 24 Z9 33 U1 2 U2 40 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X J9 PLANT SOIL JI Plant Soil PD DEC PY 2005 VL 277 IS 1-2 BP 335 EP 344 DI 10.1007/s11104-005-7932-3 PG 10 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 987OR UT WOS:000233527700029 ER PT J AU Fabricant, D Fata, R Roll, J Hertz, E Caldwell, N Gauron, T Geary, J McLeod, B Szentgyorgyi, A Zajac, J Kurtz, M Barberis, J Bergner, H Brown, W Conroy, M Eng, R Geller, M Goddard, R Honsa, M Mueller, M Mink, D Ordway, M Tokarz, S Woods, D Wyatt, W Epps, H Dell'Antonio, I AF Fabricant, D Fata, R Roll, J Hertz, E Caldwell, N Gauron, T Geary, J McLeod, B Szentgyorgyi, A Zajac, J Kurtz, M Barberis, J Bergner, H Brown, W Conroy, M Eng, R Geller, M Goddard, R Honsa, M Mueller, M Mink, D Ordway, M Tokarz, S Woods, D Wyatt, W Epps, H Dell'Antonio, I TI Hectospec, the MMT's 300 optical fiber-fed spectrograph SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MOUNTING LARGE LENSES; WIDE-FIELD CORRECTOR; CONVERTED MMT; SKY-SUBTRACTION; DESIGN; INSTRUMENTS; REDSHIFTS; SUPPORT; SYSTEM AB The Hectospec is a 300 optical fiber fed spectrograph commissioned at the MMT in the spring of 2004. In the configuration pioneered by the Autofib instrument at the Anglo-Australian Telescope, Hectospec's fiber probes are arranged in a radial "fisherman on the pond" geometry and held in position with small magnets. A pair of high-speed, six-axis robots move the 300 fiber buttons between observing configurations within similar to 300 s, and to an accuracy of similar to 25 mu m. The optical fibers run for 26 m between the MMT's focal surface and the bench spectrograph, operating at R similar to 1000-2000. Hectochelle, another high-dispersion bench spectrograph offering R similar to 35,000, is also available. The system throughput, including all losses in the telescope optics, fibers, and spectrograph, peaks at similar to 10% at the grating blaze in 1 '' FWHM seeing. Correcting for aperture losses at the 1.'' 5 diameter fiber entrance aperture, the system throughput peaks at similar to 17%, close to our prediction of 20%. Hectospec has proven to be a workhorse instrument at the MMT. Together, Hectospec and Hectochelle have been scheduled for 1/3 of the available nights since its commissioning. Hectospec has returned approximately 60,000 reduced spectra for 16 scientific programs during its first year of operation. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Brown Univ, Providence, RI 02912 USA. RP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM dfabricant@cfa.harvard.edu OI Mink, Jessica/0000-0003-3594-1823; Kurtz, Michael/0000-0002-6949-0090 NR 32 TC 203 Z9 204 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2005 VL 117 IS 838 BP 1411 EP 1434 DI 10.1086/497385 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993KE UT WOS:000233952200010 ER PT J AU Marsden, BG AF Marsden, BG TI Fred Lawrence Whipple (1906-2004) - Obituary SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Biographical-Item C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marsden, BG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bmarsden@cfa.harvard.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2005 VL 117 IS 838 BP 1452 EP 1458 DI 10.1086/497156 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993KE UT WOS:000233952200013 ER PT J AU Duran-Gonzalez, A Laguarda-Figueras, A Solis-Marin, FA Sanchez, BEB Ahearn, CG Torres-Vega, J AF Duran-Gonzalez, A Laguarda-Figueras, A Solis-Marin, FA Sanchez, BEB Ahearn, CG Torres-Vega, J TI Echinoderms (Echinodermata) from the Mexican waters of the Gulf of Mexico. SO REVISTA DE BIOLOGIA TROPICAL LA Spanish DT Article DE Echinodermata; Gulf of Mexico; Veracruz; Tabasco; Campeche; Yucatan ID ECHINOIDEA AB We present a systematic list of the echinoderms from Gulf of Mexico's Mexican waters based on specimens of the Coleccion Nacional de Equinodermos, Instituto de Ciencias del Mar y Limnologia, Universidad Nacional Autonoma de Mexico and the National Museum of Natural History, Smithsonian Institution, Washington, D.C. This list reveals an important echinoderm biodiversity present in the Gulf of Mexico, where five of the six echinoderm classes are represented. A total of 209 echinoderm species is recorded, distributed in 129 genera, 63 families and 25 orders. 31 new records for the Gulf of Mexico are presented: Asteroidea (16), Ophiuroidea (nine), Echinoidea (one) and Holothuroidea (five). C1 Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Sistemat & Ecol Equinodermos, Mexico City 04510, DF, Mexico. Univ Nacl Autonoma Mexico, Inst Geol, Dept Paleontol, Mexico City 04510, DF, Mexico. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Duran-Gonzalez, A (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Sistemat & Ecol Equinodermos, Apdo Post 70-305, Mexico City 04510, DF, Mexico. EM duran-gonzalez@mar.icmyl.unam.mx; laguarda@icmyl.unam.mx; fasolis@icmyl.unam.mx; blancab@servidor.unam.mx; AHEARN.CYNTHIA@NMNH.SI.EDU; torres@icmyl.unam.mx NR 56 TC 8 Z9 10 U1 1 U2 8 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD DEC PY 2005 VL 53 SU 3 BP 53 EP 68 PG 16 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 027EL UT WOS:000236396500005 PM 17469247 ER PT J AU Laguarda-Figueras, A Solis-Marin, FA Duran-Gonzalez, A Ahearn, CG Sanchez, BEB Torres-Vega, J AF Laguarda-Figueras, A Solis-Marin, FA Duran-Gonzalez, A Ahearn, CG Sanchez, BEB Torres-Vega, J TI Echinoderms (Echinodermata) of the Mexican Caribbean. SO REVISTA DE BIOLOGIA TROPICAL LA Spanish DT Article DE Echinodermata; Mexican Caribbean; quintana roo ID DIADEMA-ANTILLARUM; MASS MORTALITY; HOLOTHUROIDEA; ECHINOIDEA AB A systematic list of the echinoderms of the Mexican Caribbean based on museum specimens of the Coleccion Nacional de Equinodermos, Instituto de Ciencias del Mar y Limnologia, Universidad Nacional Autonoma de Mexico and the National Museum of Natural History, Smithsonian Institution, Washington, D.C. is presented. This list reveals an important echinoderm biodiversity in the Mexican Caribbean, where five of the six echinoderm classes are represented. A total of 178 echinoderm species is recorded, distributed in 113 genera, 51 families and 22 orders. 30 new records for the Mexican Caribbean are presents: Crinoidea (three), Asteroidea (two), Ophiuroidea (eleven), Echinoidea (one), Holothuroidea (thirteen). C1 Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Sistemat & Ecol Equinodermos, Mexico City 04510, DF, Mexico. Smithsonian Inst, Natl Museum Natl Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Univ Nacl Autonoma Mexico, Inst Geol, Dept Palaeontol, Mexico City 04510, DF, Mexico. RP Laguarda-Figueras, A (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Sistemat & Ecol Equinodermos, Apdo Post 70-305, Mexico City 04510, DF, Mexico. EM laguarda@icmyl.unam.mx; fasolis@icmyl.unam.mx; duran-gonzalez@mar.icmyl.unam.mx; ahearn.cynthia@nmnh.si.edu; blancab@servidor.unam.mx; torres@icmyl.unam.mx NR 61 TC 14 Z9 16 U1 1 U2 10 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD DEC PY 2005 VL 53 SU 3 BP 109 EP 122 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 027EL UT WOS:000236396500007 PM 17469249 ER PT J AU Solis-Marin, FA Laguarda-Figueras, A Duran-Gonzalez, A Ahearn, CG Vega, JT AF Solis-Marin, FA Laguarda-Figueras, A Duran-Gonzalez, A Ahearn, CG Vega, JT TI Echinoderms (Echinodermata) from the Gulf of California, Mexico. SO REVISTA DE BIOLOGIA TROPICAL LA Spanish DT Article DE Echinodermata; Mexico; Gulf of California; Baja California; Baja California Sur; Sonora; Sinaloa ID HOLOTHUROIDEA AB A systematic list of the echinoderms of the Gulf of California, based on museum specimens of the Coleccion Nacional de Equinodermos, Instituto de Ciencias del Mar y Limnologia, Universidad Nacional Autonoma de Mexico and the National Museum of Natural History, Smithsonian Institution, Washington, D.C. is presented. A total of 193 echinoderm species is recorded, distributed in 108 genera, 51 families and 19 orders. 12 new records for the Gulf of California are presented: Asteroidea (four), Ophiuroidea (three) and Holothuroidea (five). C1 Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Sisemat & Ecol Equinodermos, Mexico City 04510, DF, Mexico. Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Solis-Marin, FA (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Sisemat & Ecol Equinodermos, Apdo Post 70-305, Mexico City 04510, DF, Mexico. EM fasolis@icmyl.unam.mx; laguarda@icmyl.unam.mx; duran-gonzalez@mar.icmyl.unam.mx; AHEARN.CYNTHIA@NMNH.SI.EDU; torres@icmyl.unam.mx NR 62 TC 24 Z9 26 U1 0 U2 9 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD DEC PY 2005 VL 53 SU 3 BP 123 EP 137 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 027EL UT WOS:000236396500008 PM 17469250 ER PT J AU Lessios, HA AF Lessios, HA TI Echinoids of the Pacific Waters of Panama: Status of knowledge and new records SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE Eastern Pacific; sea urchins; Bay of Panama; Gulf of Chiriqui; systematics ID NEOTROPICAL SEA-URCHINS; GAMETIC INCOMPATIBILITY; POPULATION-STRUCTURE; DIADEMA-ANTILLARUM; GENUS ECHINOMETRA; MITOCHONDRIAL-DNA; EASTERN PACIFIC; MASS MORTALITY; EGG SIZE; 2 SIDES AB This paper is primarily intended as a guide to researchers who wish to know what echinoid species are available in the Bay of Panama and in the Gulf of Chiriqui, how to recognize them, and what has been published about them up to 2004. Fifty seven species of echinoids have been reported in the literature as occurring in the Pacific waters of Panama, of which I have collected and examined 3 1, including two species, Caenopedina diomediae and Meoma frangibilis, that have hitherto only been mentioned in the literature from single type specimens. For the 31 species I was able to examine, I list the localities in which they were found, my impression as to their relative abundance, the characters that distinguish them, and what is known about their biology and evolution. Not surprisingly, most available information concerns abundant shallow water species, while little is known about deep water, rare, or infaunal species. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Lessios, HA (reprint author), Smithsonian Trop Res Inst, Apdo 0843-03092, Balboa, Panama. EM Lessiosh@stri.org NR 69 TC 12 Z9 16 U1 0 U2 0 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD DEC PY 2005 VL 53 SU 3 BP 147 EP 170 PG 24 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 027EL UT WOS:000236396500010 PM 17469251 ER PT J AU Cedeno, I de Obaldia, R Sanjur, O Bayard, V Ortega-Barria, E Escobar, C AF Cedeno, I de Obaldia, R Sanjur, O Bayard, V Ortega-Barria, E Escobar, C TI Use of the polymerase chain reaction for diagnosing bovine tuberculosis in Panama SO REVUE SCIENTIFIQUE ET TECHNIQUE-OFFICE INTERNATIONAL DES EPIZOOTIES LA English DT Article DE bovine tuberculosis; bovines; Central America; diagnosis; Mycobacterium bovis; Panama; polymerase chain reaction; purified protein derivative; Republic of Panama; tuberculosis ID LENGTH-POLYMORPHISM ANALYSIS; MYCOBACTERIUM-BOVIS; IDENTIFICATION; CATTLE; PCR; EPIDEMIOLOGY; ANIMALS; STRAINS AB In addition to causing large losses to the cattle industry, Mycobacterium bovis, the causative agent for bovine tuberculosis, is a serious public health issue because it can potentially infect humans. Diagnosis based on isolation and identification of the bacillus is tedious and may take weeks. The diagnosis of M. bovis by polymerase chain reaction (PCR), using species-specific primers, is fast, highly sensitive and of great value in epidemiological studies. In this study, deoxyribonucleic acid (DNA) was extracted from 60 nasal mucus samples collected from three different farms, all located in an area where M. bovis is endemic. Two farms tested negative for an antibody response to the M. tuberculosis purified protein derivative (PPD) antigen, whereas the other farm gave a positive result. The amplified fragment of DNA was 460 base pairs with a sequence similar to that previously reported. Only 5% of the samples from the third farm tested positive for the presence of antibodies against PPD, whereas 65% of samples (from all three farms) gave a positive result when PCR was used. Thus, the authors suggest the use of the PCR species-specific primers test to support the programme against bovine tuberculosis in Panama. C1 Minist Desarrollo Agropecuario Salud Anim, Lab Diagnost & Invest Vet Dr Gerardino Medina, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. Minist Salud, Inst Conmemorat Gorgas Estudios Salud, Panama City, Panama. RP Cedeno, I (reprint author), Minist Desarrollo Agropecuario Salud Anim, Lab Diagnost & Invest Vet Dr Gerardino Medina, Panama City, Panama. NR 21 TC 5 Z9 5 U1 0 U2 2 PU OFFICE INT EPIZOOTIES PI PARIS PA 12 RUE DE PRONY, 75017 PARIS, FRANCE SN 0253-1933 J9 REV SCI TECH OIE JI Rev. Sci. Tech. Off. Int. Epizoot. PD DEC PY 2005 VL 24 IS 3 BP 1067 EP 1075 PG 9 WC Veterinary Sciences SC Veterinary Sciences GA 028WQ UT WOS:000236519900024 PM 16642775 ER PT J AU Lopez, OR Kursar, TA Cochard, H Tyree, MT AF Lopez, OR Kursar, TA Cochard, H Tyree, MT TI Interspecific variation in xylem vulnerability to cavitation among tropical tree and shrub species SO TREE PHYSIOLOGY LA English DT Article DE drought tolerance; hydraulic conductivity; tropical rainforest; water potential; water stress; xylem cavitation ID DRY FOREST TREES; HYDRAULIC ARCHITECTURE; WATER RELATIONS; WOODY-PLANTS; NEOTROPICAL FOREST; SEVERE DROUGHT; CANOPY TREES; EMBOLISM; PANAMA; LEAF AB In tropical moist forests, seasonal drought limits plant survival, productivity and diversity. Drought-tolerance mechanisms of tropical species should reflect the maximum seasonal water deficits experienced in a particular habitat. We investigated stem xylem vulnerability to cavitation in nine tropical species with different life histories and habitat associations. Stem xylem vulnerability was scored as the xylem water potential causing 50 and 75% loss of hydraulic conductivity (P50 and P75, respectively). Four shade-tolerant shrubs ranged from moderately resistant (P50 = -1.9 MPa for Ouratea lucens Kunth. Engl.) to highly resistant to cavitation (P50 = -4.1 MPa for Psychotria horizontalis Sw.), with shallow-rooted species being the most resistant. Among the tree species, those characteristic of waterlogged soils, Carapa guianensis Aubl., Prioria copaifera Griseb. and Ficus citrifolia Mill., were the most vulnerable to cavitation (P50 = -0.8 to -1.6 MPa). The wet-season, deciduous tree, Cordia alliodora (Ruiz & Pav.) Oken., had resistant xylem (P50 = -3.2 MPa), whereas the dry-season, deciduous tree, Bursera simaruba (L.) Sarg. was among the most vulnerable to cavitation (P50 = -0.8 MPa) of the species studied. For eight out of the nine study species, previously reported minimum seasonal leaf water potentials measured in the field during periods of drought correlated with our P50 and P75 values. Rooting depth, deciduousness, soil type and growth habit might also contribute to desiccation tolerance. Our results support the functional dependence of drought tolerance on xylem resistance to cavitation. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Clermont Ferrand, INRA, UMR PIAF, F-63039 Clermont Ferrand, France. US Forest Serv, USDA, Aiken Forestry Sci Lab, Burlington, VT 05402 USA. RP Lopez, OR (reprint author), Univ Utah, Dept Biol, 257 S & 1400 E, Salt Lake City, UT 84112 USA. EM prioria@yahoo.com RI Cochard, Herve/P-7406-2015 OI Cochard, Herve/0000-0002-2727-7072 NR 52 TC 35 Z9 36 U1 3 U2 29 PU HERON PUBLISHING PI VICTORIA PA 202, 3994 SHELBOURNE ST, VICTORIA, BC V8N 3E2, CANADA SN 0829-318X J9 TREE PHYSIOL JI Tree Physiol. PD DEC PY 2005 VL 25 IS 12 BP 1553 EP 1562 PG 10 WC Forestry SC Forestry GA 994GT UT WOS:000234019900009 PM 16137941 ER PT J AU Laurance, WF AF Laurance, WF TI When bigger is better: the need for Amazonian mega-reserves SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID BRAZILIAN AMAZON; FOREST; DEFORESTATION; CONSERVATION; ENVIRONMENT; AREA AB The rate of forest destruction has accelerated sharply in Brazilian Amazonia, but there are also vital conservation opportunities with the ongoing designation of important new protected areas. In a timely paper, Carlos Peres argues that an extensive network of mega-reserves, operationally defined as those exceeding 1 million ha in area, is needed to ensure the long-term persistence of Amazonian species and ecological processes. Although such protected areas might seem excessively large to some, disparate lines of evidence suggest that mega-reserves are vital for the future of Amazonian biodiversity. 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 25 TC 31 Z9 31 U1 2 U2 25 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 DEC PY 2005 VL 20 IS 12 BP 645 EP 648 DI 10.1016/j.tree.2005.10.009 PG 4 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 992IX UT WOS:000233878700002 PM 16701449 ER PT J AU Morton, ES AF Morton, ES TI Predation and variation in breeding habitat use in the Ovenbird, with special reference to breeding habitat selection in northwestern Pennsylvania SO WILSON BULLETIN LA English DT Article ID FOREST-DOMINATED LANDSCAPE; PAIRING SUCCESS; SEIURUS-AUROCAPILLUS; REPRODUCTIVE SUCCESS; EXTRAPAIR PATERNITY; HOODED WARBLERS; NEST-PREDATORS; BIRDS; EDGE; FRAGMENTATION AB From 1971 through 2003, Ovenbirds (Seiurus aurocapilla) at the Hemlock Hill Biological Research Area in northwestern Pennsylvania never bred in forest interior. Instead, they exhibited atypical habitat selection for breeding by occupying regenerating forest edges. Pairs in, 14 territories, the entire population, showed normal annual return rates and pairing rates compared with other studies. For this ground-foraging bird, other studies showed that deep soil litter is preferred-but at my study site, soil litter depth in Ovenbird-occupied areas was lower than that found in the unoccupied forest interior. During May, July, and August, songs played in forest interior to attract Ovenbirds to settle there were unsuccessful. I tested the hypothesis that eastern chipmunk (Tamias striatus) abundance influenced this atypical habitat selection. Chipmunks were nearly absent from Ovenbird territories, but were abundant in the forest interior. I discuss habitat selection in birds in relation to simple cues and relate this to variation in habitat selection and use found in Ovenbirds. C1 Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20008 USA. York Univ, Dept Biol, N York, ON M3J 1P3, Canada. RP Morton, ES (reprint author), Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20008 USA. EM mortone@si.edu NR 55 TC 22 Z9 23 U1 4 U2 28 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD DEC PY 2005 VL 117 IS 4 BP 327 EP 335 DI 10.1676/04-135.1 PG 9 WC Ornithology SC Zoology GA 995MI UT WOS:000234104000001 ER PT J AU Trapani, J Yamamoto, Y Stock, DW AF Trapani, J Yamamoto, Y Stock, DW TI Ontogenetic transition from unicuspid to multicuspid oral dentition in a teleost fish: Astyanax mexicanus, the Mexican tetra (Ostariophysi : Characidae) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE allometry; first-generation dentition; morphology; morphometrics; ontogeny; teeth; tooth development; tooth replacement ID TROUT SALMO-GAIRDNERI; TOOTH REPLACEMENT; PHARYNGEAL DENTITION; UPPER JAW; CICHLASOMA-MINCKLEYI; 1ST-GENERATION TEETH; EYE DEGENERATION; BLIND CAVEFISH; RIVER-BASIN; EVOLUTION AB Teleost fishes display a remarkable diversity of adult dentitions; this diversity is all the more remarkable in light of the uniformity of first-generation dentitions. Few studies have quantitatively documented the transition between generalized first-generation dentitions and specialized adult dentitions in teleosts. We investigated this transition in the Mexican tetra, Astyanax mexicanus (Characidae), by measuring aspects of the dentition in an ontogenetic series of individuals from embryos to 160 days old, in addition to adults of unknown age. The first-generation dentition and its immediate successors consist of small, unicuspid teeth that develop extraosseously. Multicuspid teeth first appear during the second tooth replacement event, and are derived from single tooth germs, rather than from the fusion of multiple conical tooth germs. We document that the transition from unicuspid to multicuspid teeth corresponds to a change in the location of developing tooth germs (from extraosseous to intraosseous) and in patterns of tooth replacement (from haphazard to simultaneous within a jaw quadrant). In addition, while the size of the largest teeth scales with positive allometry to fish size, the transition to multicuspid teeth is accompanied by an exceptionally large increase in tooth size. (c) 2005 The Linnean Society of London, Zoological Journal of the Linnean Society, 2005, 145, 523-538. C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, NHB, Washington, DC 20013 USA. Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. UCL, Evolutionary Anat Unit, Dept Anat & Dev Biol, London WC1E 6BT, England. RP Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, NHB, MRC121, Washington, DC 20013 USA. EM jtrapani@umich.edu NR 78 TC 24 Z9 24 U1 0 U2 6 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 DEC PY 2005 VL 145 IS 4 BP 523 EP 538 DI 10.1111/j.1096-3642.2005.00193.x PG 16 WC Zoology SC Zoology GA 987PW UT WOS:000233530800002 ER PT J AU Ghent, RR Phillips, RJ Hansen, VL Nunes, DC AF Ghent, RR Phillips, RJ Hansen, VL Nunes, DC TI Finite element modeling of short-wavelength folding on Venus: Implications for the plume hypothesis for crustal plateau formation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID UNEVENLY SPACED DATA; TIME-SERIES ANALYSIS; TESSERA TERRAIN; TECTONIC DEFORMATION; SPECTRAL-ANALYSIS; GLOBAL TECTONICS; FORTUNA-TESSERA; THERMAL STATE; EVOLUTION; LITHOSPHERE AB [1] The key geological observations and structural interpretations associated with the current plume hypothesis for Venusian crustal plateau formation are that ( 1) short-wavelength, spatially periodic tectonic structures originated as mechanical instabilities in a regionally extensive surface brittle layer whose basal boundary was thermally generated and controlled; ( 2) characteristic wavelengths of spatially periodic structures record the brittle layer thickness at the time of deformation; and ( 3) structural wavelengths increased with time, driven by brittle layer thickening in response to cooling. The plume hypothesis accommodates these constraints by proposing that crustal plateaus formed above mantle plumes impinging on thin lithosphere; it further suggests that surface temperatures temporarily elevated to similar to 1000 K may have been required to maintain a sufficiently thin brittle layer for formation of the shortest- wavelength structures. We report here on finite element simulations designed to test the feasibility of the proposed thermal conditions. Specifically, we model formation of short-wavelength folds thought to have initiated as contractional layer instabilities early in the plateau formation process. Under high surface temperatures, the finite element meshes develop semibrittle zones in which short-wavelength folds can form, but development of even modest structural relief requires unrealistically high total mesh shortening. Thus elevated surface temperatures inhibit development of short-wavelength folds because the models' effective integrated mechanical strength under such hot conditions is excessively low. Decreasing the surface temperature increases structural relief but produces tectonic wavelengths that are larger than those observed. We conclude that a model with solely thermal control of mechanical properties cannot explain the observed structures. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Univ Minnesota, Dept Geol Sci, Duluth, MN 55812 USA. Lunar & Planetary Inst, Houston, TX 77058 USA. RP Ghent, RR (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, POB 37012,NASM Room 3754, Washington, DC 20013 USA. EM ghentr@si.edu NR 59 TC 7 Z9 7 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV 26 PY 2005 VL 110 IS E11 AR E11006 DI 10.1029/2005JE002522 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 988WP UT WOS:000233632500001 ER PT J AU Allesina, S Bondavalli, C Scharler, UM AF Allesina, S Bondavalli, C Scharler, UM TI The consequences of the aggregation of detritus pools in ecological networks SO ECOLOGICAL MODELLING LA English DT Article DE ecological networks; aggregation; trophospecies; detritus; food web; ascendency ID FOOD-WEB STRUCTURE; TROPHIC STRUCTURE; ECOSYSTEM; LAGOON; MEXICO; ENERGY; FLOWS; BAY; BIOMASS; MODELS AB Ecological networks are quantitative, graph-based descriptions of ecosystems, consisting of compartments (trophospecies and nutrient pools) that exchange fluxes of nutrients or energy. Previous research pointed out how the model's design is a crucial task that can heavily influence analyses results, and how merging compartments for the purpose of comparing two or more different ecosystems can significantly alter the indices on which the comparison is based. All these works have been focused on the aggregation of trophospecies, whereas networks may comprise several nutrient compartments that may be lumped as well, either for lack of information or for comparison constraints. We show how the aggregation of these non-living compartments can have a greater influence on network analysis results than trophospecies clustering. This problem should on the one hand encourage modelers to make an effort to test the possible effects of aggregations, and on the other show how the role of non-living compartments could be very important in determining network dynamics. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Parma, Dept Environm Sci, I-43100 Parma, Italy. Michigan State Univ, Dept Wildlife & Fisheries, E Lansing, MI 48824 USA. Univ Maryland, Chesapeake Biol Lab, Ctr Environm Studies, Solomons, MD 20688 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Allesina, S (reprint author), Univ Parma, Dept Environm Sci, Via Sci 33-A, I-43100 Parma, Italy. EM allesina@msu.edu RI Allesina, Stefano/A-2255-2009; Scharler, Ursula/F-3598-2010 NR 53 TC 30 Z9 30 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 J9 ECOL MODEL JI Ecol. Model. PD NOV 25 PY 2005 VL 189 IS 1-2 BP 221 EP 232 DI 10.1016/j.ecolmodel.2005.04.002 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 985JT UT WOS:000233374300013 ER PT J AU Sajeev, Y Santra, R Pal, S AF Sajeev, Y Santra, R Pal, S TI Correlated complex independent particle potential for calculating electronic resonances SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID COUPLED-CLUSTER METHOD; ACCURATE ABINITIO TREATMENT; ABSORBING POTENTIALS; TEMPORARY ANIONS; SHAPE RESONANCE; FOCK SPACE; SCHWINGER MULTICHANNEL; MOLECULE SCATTERING; EXCITATION-ENERGIES; GENERAL FORMALISM AB We have formulated and applied an analytic continuation method for the recently formulated correlated independent particle potential [A. Beste and R. J. Bartlett J. Chem. Phys. 120, 8395 (2004)] derived from Fock space multireference coupled cluster theory. The technique developed is an advanced ab initio tool for calculating the properties of resonances in the low-energy electron-molecule collision problem. The proposed method quantitatively describes elastic electron-molecule scattering below the first electronically inelastic threshold. A complex absorbing potential is utilized to define the analytic continuation for the potential. A separate treatment of electron correlation and relaxation effects for the projectile-target system and the analytic continuation using the complex absorbing potential is possible, when an approximated form of the correlated complex independent particle potential is used. The method, which is referred to as complex absorbing potential-based correlated independent particle (CAP-CIP), is tested by application to the well-known (2)Pi(g) shape resonance of e-N-2 and the B-2(2g) shape resonance of e-C2H4 (ethylene) with highly satisfactory results. (c) 2005 American Institute of Physics. C1 Natl Chem Lab, Div Phys Chem, Theory Grp, Pune 411008, Maharashtra, India. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Natl Chem Lab, Div Phys Chem, Theory Grp, Pune 411008, Maharashtra, India. EM pal@ems.ncl.res.in RI Santra, Robin/E-8332-2014; OI Santra, Robin/0000-0002-1442-9815; yesodharan, sajeev/0000-0002-2250-5101 NR 66 TC 22 Z9 22 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 22 PY 2005 VL 123 IS 20 AR 204110 DI 10.1063/1.2130338 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 989GN UT WOS:000233661000012 PM 16351243 ER PT J AU Spurr, R Loyola, D Thomas, W Balzer, W Mikusch, E Aberle, B Slijkhuis, S Ruppert, T van Roozendael, M Lambert, JC Soebijanta, T AF Spurr, R Loyola, D Thomas, W Balzer, W Mikusch, E Aberle, B Slijkhuis, S Ruppert, T van Roozendael, M Lambert, JC Soebijanta, T TI GOME level 1-to-2 data processor version 3.0: a major upgrade of the GOME/ERS-2 total ozone retrieval algorithm SO APPLIED OPTICS LA English DT Article ID MONITORING EXPERIMENT GOME; ABSORPTION CROSS-SECTIONS; RADIATIVE-TRANSFER MODEL; SENSING REFERENCE DATA; 231-794 NM RANGE; AIR-MASS FACTORS; NO2; SATELLITES; PARAMETERS; TOMS AB The global ozone monitoring experiment (GOME) was launched in April 1995, and the GOME data processor (GDP) retrieval algorithm has processed operational total ozone amounts since July 1995. GDP level 1-to-2 is based on the two-step differential optical absorption spectroscopy (DOAS) approach, involving slant column fitting followed by air mass factor (AMF) conversions to vertical column amounts. We present a major upgrade of this algorithm to version 3.0. GDP 3.0 was implemented in July 2002, and the 9-year GOME data record from July 1995 to December 2004 has been processed using this algorithm. The key component in GDP 3.0 is an iterative approach to AMF calculation, in which AMFs and corresponding vertical column densities are adjusted to reflect the true ozone distribution as represented by the fitted DOAS effective slant column. A neural network ensemble is used to optimize the fast and accurate parametrization of AMFs. We describe results of a recent validation exercise for the operational version of the total ozone algorithm; in particular, seasonal and meridian errors are reduced by a factor of 2. On a global basis, GDP 3.0 ozone total column results lie between -2% and +4% of ground-based values for moderate solar zenith angles lower than 70 degrees. A larger variability of about +5% and -8% is observed for higher solar zenith angles up to 90 degrees. (c) 2005 Optical Society of America. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Deutsch Zentrum Luft & Raumfahrt, DLR, IMF, D-82234 Wessling, Germany. Deutsch Zentrum Luft & Raumfahrt, DLR, DFD, D-82234 Wessling, Germany. Inst Aeron Spatiale Belgique, BIRA, B-1180 Brussels, Belgium. RP Spurr, R (reprint author), RT Solut Inc, 9 Channing St, Cambridge, MA 02138 USA. OI Loyola R., Diego G./0000-0002-8547-9350 NR 39 TC 18 Z9 18 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 NOV 20 PY 2005 VL 44 IS 33 BP 7196 EP 7209 DI 10.1364/AO.44.007196 PG 14 WC Optics SC Optics GA 984ZD UT WOS:000233345000026 PM 16318193 ER PT J AU Furlanetto, SR Loeb, A AF Furlanetto, SR Loeb, A TI Is double reionization physically plausible? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : evolution; intergalactic medium ID DARK-MATTER HALOES; 1ST COSMOLOGICAL OBJECTS; 21 CENTIMETER TOMOGRAPHY; PROBE WMAP OBSERVATIONS; LOW-MASS GALAXIES; INTERGALACTIC MEDIUM; HIGH-REDSHIFT; STAR-FORMATION; RADIATIVE FEEDBACK; POPULATION-III AB Recent observations of z similar to 6 quasars and the cosmic microwave background imply a complex history of cosmic reionization. Such a history requires some form of feedback to extend reionization over a long time interval, but the nature of the feedback and how rapidly it operates remain highly uncertain. Here we focus on one aspect of this complexity: which physical processes can cause the global ionized fraction to evolve nonmonotonically with cosmic time? We consider a range of mechanisms and conclude that double reionization is much less likely than a long, but still monotonic, ionization history. We first examine how galactic winds affect the transition from metal-free to normal star formation. Because the transition is actually spatially inhomogeneous and temporally extended, this mechanism cannot be responsible for double reionization, given plausible parameters for the winds. We next consider photoheating, which causes the cosmological Jeans mass to increase in ionized regions and hence suppresses galaxy formation there. In this case, double reionization requires that small halos form stars efficiently, that the suppression from photoheating is strong relative to current expectations, and that ionizing photons are preferentially produced outside previously ionized regions. Finally, we consider H-2 photodissociation, in which the buildup of a soft ultraviolet background suppresses star formation in small halos. This can in principle cause the ionized fraction to temporarily decrease, but only during the earliest stages of reionization. Finally, we briefly consider the effects of some of these feedback mechanisms on the topology of reionization. C1 CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), CALTECH, Div Phys Math & Astron, Mail Code 130-33, Pasadena, CA 91125 USA. EM sfurlane@tapir.caltech.edu; aloeb@cfa.harvard.edu NR 86 TC 65 Z9 65 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 NOV 20 PY 2005 VL 634 IS 1 BP 1 EP 13 DI 10.1086/429080 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800001 ER PT J AU Huang, JS Rigopoulou, D Willner, SP Papovich, C Shu, C Ashby, MLN Barmby, P Bundy, K Conselice, C Egami, E Perez-Gonzalez, PG Rosenberg, JL Smith, HA Wilson, G Fazio, GG AF Huang, JS Rigopoulou, D Willner, SP Papovich, C Shu, C Ashby, MLN Barmby, P Bundy, K Conselice, C Egami, E Perez-Gonzalez, PG Rosenberg, JL Smith, HA Wilson, G Fazio, GG TI Infrared luminous Lyman break galaxies: A population that bridges LBGs and scuba galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : high-redshift; infrared : galaxies; surveys ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; ARRAY CAMERA IRAC; REDSHIFT SURVEY; LOCKMAN HOLE; MASSIVE GALAXIES; FIELD; IDENTIFICATIONS; SPECTROSCOPY; EVOLUTION AB A deep mid- and far-infrared survey in the extended Groth strip (EGS) area gives 3.6 to 8 mu m flux densities or upper limits for 253 Lyman break galaxies (LBGs). The LBGs are a diverse population but with properties correlated with luminosity. The LBGs show a factor of 30 range in indicated stellar mass and a factor of 10 range in apparent dust content relative to stellar mass. About 5% of LBGs are luminous at all wavelengths, with powerful emission at rest 6 mu m. In the rest 0.9 to 2 mu m spectral range these galaxies have stellar spectral slopes with no sign of an AGN power-law component, suggesting that their emission is mainly powered by intensive star formation. Galaxies in this luminous population share the infrared properties of cold Submillimeter Common-User Bolometric Array (SCUBA) sources: both are massive and dusty starburst galaxies at 2 < z < 3; their stellar mass is larger than 10(11) M-circle dot. We suggest that these galaxies are the progenitors of present-day giant elliptical galaxies, with a substantial fraction of their stars already formed at z approximate to 3. 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. Shanghai Normal Univ, Joint Ctr Astrophys, Shanghai 200234, Peoples R China. Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. 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; Perez-Gonzalez, Pablo/J-2871-2016; OI Barmby, Pauline/0000-0003-2767-0090; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Conselice, Christopher/0000-0003-1949-7638 NR 37 TC 38 Z9 38 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP 137 EP 141 DI 10.1086/491697 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800012 ER PT J AU Wilkes, BJ Pounds, KA Schmidt, GD Smith, PS Cutri, RM Ghosh, H Nelson, B Hines, DC AF Wilkes, BJ Pounds, KA Schmidt, GD Smith, PS Cutri, RM Ghosh, H Nelson, B Hines, DC TI XMM-Newton observations of red AGNs SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; X rays : galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; TYPE-2 SEYFERT-GALAXIES; QUASI-STELLAR OBJECTS; ALL-SKY SURVEY; CHANDRA MULTIWAVELENGTH PROJECT; AREA SURVEY HELLAS; ASCA OBSERVATIONS; LOCKMAN HOLE; SPECTRAL PROPERTIES AB XMM-Newton spectra of five red 2MASS active galactic nuclei (AGNs), selected from a sample observed by Chandra to be relatively X-ray bright and to cover a range of hardness ratios, confirm the presence of substantial absorbing material in three sources with optical classifications ranging from type 1 to type 2. A flat ( hard) power-law continuum is observed in the other two. The combination of X-ray absorption and broad optical emission lines suggests either a small (nuclear) absorber or a favored viewing angle so as to cover the X-ray source but not the broad emission-line region (BELR). A soft excess is detected in all three type 1 sources. We speculate that this may arise in an extended region of ionized gas, perhaps linked to the polarized (scattered) optical light present in these sources. The spectral complexity revealed by XMM-Newton emphasizes the limitations of the low-S/N Chandra data. The new results strengthen our earlier conclusions that the observed X-ray continua of red AGNs are unusually hard at energies greater than or similar to 2 keV. Their observed spectra are consistent with contributing significantly to the missing hard or absorbed population of the cosmic X-ray background (CXRB), although their intrinsic power-law slopes are typical of broad-line (type 1) AGNs (Gamma similar to 1.7-1.9). This suggests that the missing X-ray-absorbed CXRB population may include type 1 AGNs or QSOs in addition to the type 2 AGNs generally assumed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Ohio State Univ, Dept Astron, MacPherson Lab 4055, Columbus, OH 43210 USA. Space Sci Inst, Boulder, CO 80301 USA. RP Wilkes, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 52 TC 22 Z9 22 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 NOV 20 PY 2005 VL 634 IS 1 BP 183 EP 192 DI 10.1086/444555 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800018 ER PT J AU Scott, JE Kriss, GA Lee, JC Quijano, JK Brotherton, M Canizares, CR Green, RF Hutchings, J Kaiser, ME Marshall, H Oegerle, W Ogle, P Zheng, W AF Scott, JE Kriss, GA Lee, JC Quijano, JK Brotherton, M Canizares, CR Green, RF Hutchings, J Kaiser, ME Marshall, H Oegerle, W Ogle, P Zheng, W TI Intrinsic absorption in the spectrum of NGC 7469: Simultaneous Chandra, FUSE, and STIS observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual ( NGC 7469); galaxies : Seyfert; quasars : absorption lines; ultraviolet : galaxies; X rays : galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY SPECTROSCOPY; TELESCOPE IMAGING SPECTROGRAPH; HUBBLE-SPACE-TELESCOPE; BROAD-LINE REGION; SEYFERT-1 GALAXY NGC-7469; IONIZED-GAS; XMM-NEWTON; ECHELLE OBSERVATIONS; PHYSICAL CONDITIONS AB We present simultaneous X-ray, far-ultraviolet, and near-ultraviolet spectra of the Seyfert 1 galaxy NGC 7469 obtained with the Chandra X-Ray Observatory, the Far Ultraviolet Spectroscopic Explorer, and the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. Previous nonsimultaneous observations of this galaxy found two distinct UV absorption components, at -560 and -1900 km s(-1), with the former as the likely counterpart of the X-ray absorber. We confirm these two absorption components in our new UV observations, in which we detect prominent O VI, Ly alpha, N V, and C IV absorption. In our Chandra spectrum we detect O VIII emission, but no significant O VIII or O VII absorption. We also detect a prominent Fe K alpha emission line in the Chandra spectrum, as well as absorption due to hydrogen-like and helium-like neon, magnesium, and silicon at velocities consistent with the -560 km s(-1) UV absorber. The FUSE and STIS data reveal that the H I and C IV column densities in this UV- and X-ray-absorbing component have increased over time, as the UV continuum flux decreased. We use measured H I, N V, C IV, and O VI column densities to model the photoionization state of both absorbers self-consistently. We confirm the general physical picture of the outflow in which the low-velocity component is a highly ionized, high-density absorber with a total column density of 10(20) cm(-2), located near the broad emission-line region, although due to measurable columns of N V and C IV, we assign it a somewhat smaller ionization parameter than found previously, U similar to 1. The high-velocity UV component is of lower density, log N = 18.6, and likely resides farther from the central engine, as we find its ionization parameter to be U = 0.08. C1 NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Greenbelt, MD 20771 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. Jet Propuls Lab, Pasadena, CA 91109 USA. RP Scott, JE (reprint author), NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Code 661, Greenbelt, MD 20771 USA. EM jscott@stis.gsfc.nasa.gov; gak@stsci.edu; jclee@cfa.harvard.edu; jkim@stsci.edu; mborther@uwyo.edu; crc@space.mit.edu; rgreen@noao.edu; john.hutchings@hia.nrc.ca; kaiser@pha.jhu.edu; hermanm@space.mit.edu; oegerle@uvo.gsfc.nasa.gov; pmo@sgra.jpl.nasa.gov; zheng@pha.jhu.edu RI Oegerle, William/C-9070-2012; Lee, Julia/G-2381-2015 OI Lee, Julia/0000-0002-7336-3588 NR 71 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP 193 EP 209 DI 10.1086/496911 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800019 ER PT J AU Gallagher, JS Garnavich, PM Berlind, P Challis, P Jha, S Kirshner, RP AF Gallagher, JS Garnavich, PM Berlind, P Challis, P Jha, S Kirshner, RP TI Chemistry and star formation in the host galaxies of Type Ia supernovae SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; supernovae : general ID TELESCOPE KEY PROJECT; HUBBLE CONSTANT; STELLAR POPULATION; FORMATION HISTORY; FIELD GALAXIES; LIGHT CURVES; MASS STARS; SN 1999BY; LUMINOSITY; UNIVERSE AB We study the effect of environment on the properties of Type Ia supernovae by analyzing the integrated spectra of 57 local Type Ia supernova host galaxies. We deduce from the spectra the metallicity, current star formation rate, and star formation history of the host and compare these to the supernova decline rates. Additionally, we compare the host properties to the difference between the derived supernova distance and the distance determined from the best-fit Hubble law. From this we investigate possible uncorrected systematic effects inherent in the calibration of Type Ia supernova luminosities using light-curve fitting techniques. Our results indicate a statistically insignificant correlation in the direction of higher metallicity spiral galaxies hosting fainter Type Ia supernovae. However, we present qualitative evidence suggesting that progenitor age is more likely to be the source of variability in supernova peak luminosities than is metallicity. We do not find a correlation between the supernova decline rate and host galaxy absolute B magnitude, nor do we find evidence of a significant relationship between decline rate and current host galaxy star formation rate. A tenuous correlation is observed between the supernova Hubble residuals and host galaxy metallicities. Further host galaxy observations will be needed to refine the significance of this result. Finally, we characterize the environmental property distributions for Type Ia supernova host galaxies through a comparison with two larger, more general galaxy distributions using Kolmogorov-Smirnov tests. The results show the host galaxy metallicity distribution to be similar to the metallicity distributions of the galaxies of the NFGS and SDSS. Significant differences are observed between the SN Ia distributions of absolute B magnitude and star formation histories and the corresponding distributions of galaxies in the NFGS and SDSS. Among these is an abrupt upper limit observed in the distribution of star formation histories of the host galaxy sample, suggesting a Type Ia supernovae characteristic delay time lower limit of approximately 2.0 Gyr. Other distribution discrepancies are investigated and the effects on the supernova properties are discussed. C1 Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. FL Whipple Observ, Amado, AZ 85645 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Gallagher, JS (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. NR 55 TC 108 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 NOV 20 PY 2005 VL 634 IS 1 BP 210 EP 226 DI 10.1086/491664 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800020 ER PT J AU Trudolyubov, S Kotov, O Priedhorsky, W Cordova, F Mason, K AF Trudolyubov, S Kotov, O Priedhorsky, W Cordova, F Mason, K TI XMM-Newton observations of the M31 northern disk: Properties of selected X-ray sources and unresolved emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual ( M31); X-rays : galaxies; X-rays : stars ID SUPERNOVA REMNANT CANDIDATES; ROSAT PSPC SURVEY; GLOBULAR-CLUSTERS; CENTRAL REGION; EXTERNAL GALAXIES; NOVA REMNANTS; SKY SURVEY; HOT GAS; CHANDRA; M-31 AB We present the results of an XMM-Newton survey of the northern part of M31 disk. The X-ray properties of the 37 brightest sources are studied in detail. Combining the results of X-ray analysis with available data at other wavelengths, we were able to identify 19 out of 37 sources. Two sources in our sample were previously unknown: the hard X-ray source XMMU J004415.8+413057 and a transient supersoft source XMMU J004414.1+412206. We report on the discovery of X-ray pulsations from the source XMMU J004415.8+413057 with a period of 197s. Three X-ray sources were identified with optical and radio SNR candidates. Five bright X-ray sources coincide with Galactic foreground stars. The properties of the remaining 18 bright X-ray sources detected in the survey are consistent with an AGN in the background of M31 and X-ray binaries belonging to M31. We report on the first unambiguous detection of the soft unresolved X-ray emission from the disk of M31. It follows the pattern of the spiral arms and can be traced up to the distance of similar to 10 kpc from the center of the galaxy. The spectrum of the unresolved emission shows dominant soft thermal component, which can be fit with a similar to 0.37 keV optically thin thermal plasma emission model or a combination of two thermal plasma models with temperatures of similar to 0.1 and similar to 0.7 keV. We suggest that significant part of the unresolved X-ray emission may represent hot diffuse gas and late-type stars in the disk of M31. C1 Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92507 USA. Russian Acad Sci, Space Res Inst, Moscow 117810, Russia. Los Almos Natl Lab, Los Alamos, NM 87545 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Trudolyubov, S (reprint author), Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92507 USA. OI Priedhorsky, William/0000-0003-0295-9138 NR 73 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP 314 EP 331 DI 10.1086/496940 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800027 ER PT J AU Williams, BF Barnard, R Garcia, MR Kolb, U Osborne, JP Kong, AKH AF Williams, BF Barnard, R Garcia, MR Kolb, U Osborne, JP Kong, AKH TI A potential supernova remnant-X-ray binary association in M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual ( M31); supernova remnants; X-rays : binaries ID NEUTRON-STAR BINARIES; PULSAR WIND NEBULA; NOVA REMNANTS; XMM-NEWTON; CHANDRA; KICKS; TRANSIENT; SYSTEMS; CAMERA; M-31 AB The well-studied X-ray/optical/radio supernova remnant (SNR) DDB 1-15 (CXOM31 J004327.8+411829; r3-63) in M31 has been investigated with archival XMM-Newton and Chandra observations. The timing data from XMM-Newton reveal a power density spectrum (PDS) characteristic of accreting compact objects in X-ray binaries (XRBs). The PDS shows features typical of Roche lobe overflow accretion, hinting that the XRB is low mass. The Chandra observations resolve the SNR into a shell and show a variable count rate at the 94% confidence level in the northwest quadrant. Together, these XMM-Newton and Chandra data suggest that there is an XRB in the SNR r3-63 and that the XRB is located in the northwestern portion of the SNR. The currently available X-ray and optical data show no evidence that the XRB is high mass. If the XRB is lowmass, r3-63 would be the first SNR found to contain a lowmass X-ray binary. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Open Univ, Dept Phys & Astron, Milton Keynes MK7 6BT, Bucks, England. Univ Leicester, Leicester LE1 7RH, Leics, England. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head.cfa.harvard.edu; r.barnard@open.ac.uk; garcia@head.cfa.harvard.edu; u.c.kolb@open.ac.uk; julo@star.le.ac.uk; akong@space.mit.edu NR 33 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP 365 EP 375 DI 10.1086/496944 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800031 ER PT J AU Warren, JS Hughes, JP Badenes, C Ghavamian, P McKee, CF Moffett, D Plucinsky, PP Rakowski, C Reynoso, E Slane, P AF Warren, JS Hughes, JP Badenes, C Ghavamian, P McKee, CF Moffett, D Plucinsky, PP Rakowski, C Reynoso, E Slane, P TI Cosmic-ray acceleration at the forward shock in Tycho's supernova remnant: Evidence from Chandra X-ray observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual ( Tycho); supernovae : general; supernova remnants; X-rays : ISM ID PARTICLE-ACCELERATION; IA SUPERNOVAE; EMISSION; MODELS; INSTABILITIES; EXPANSION; SPECTRUM; EJECTA; RADIO; SIMULATIONS AB We present evidence for cosmic-ray acceleration at the forward shock in Tycho's supernova remnant (SNR) from three X-ray observables: ( 1) the proximity of the contact discontinuity to the forward shock, or blast wave, ( 2) the morphology of the emission from the rim of Tycho, and (3) the spectral nature of the rim emission. We determine the locations of the blast wave (BW), contact discontinuity (CD), and reverse shock (RS) around the rim of Tycho's supernova remnant using a principal component analysis and other methods applied to new Chandra data. The azimuthal-angle-averaged radius of the BW is 251". For the CD and RS we find average radii of 241" and 183", respectively. Taking account of projection effects, we find ratios of 1:0.93:0.70 (BW: CD: RS). We show these values to be inconsistent with adiabatic hydrodynamic models of SNR evolution. The CD: BW ratio can be explained if cosmic-ray acceleration of ions is occurring at the forward shock. The RS : BW ratio, as well as the strong Fe K alpha emission from the Tycho ejecta, imply that the RS is not accelerating cosmic rays. We also extract radial profiles from similar to 34% of the rim of Tycho and compare them to models of surface brightness profiles behind the BW for a purely thermal plasma with an adiabatic shock. The observed morphology of the rim is much more strongly peaked than predicted by the model, indicating that such thermal emission is implausible here. Spectral analysis also implies that the rim emission is nonthermal in nature, lending further support to the idea that Tycho's forward shock is accelerating cosmic rays. C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Furman Univ, Dept Phys, Greenville, SC 29613 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. RP Warren, JS (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. EM jesawyer@physics.rutgers.edu; jph@physics.rutgers.edu OI Badenes, Carles/0000-0003-3494-343X NR 56 TC 184 Z9 185 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 NOV 20 PY 2005 VL 634 IS 1 BP 376 EP 389 DI 10.1086/496941 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800032 ER PT J AU Schnee, SL Ridge, NA Goodman, AA Li, JG AF Schnee, SL Ridge, NA Goodman, AA Li, JG TI A complete look at the use of IRAS emission maps to estimate extinction and dust temperature SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust; extinction; ISM : clouds; surveys ID INTERSTELLAR DUST; INFRARED-EMISSION; MOLECULAR CLOUDS; COLD DUST; MODELS; GAS AB We have created new dust temperature and column density maps of Perseus, Ophiuchus, and Serpens using 60 and 100 mu m data from the Improved Reprocessing of the IRAS Survey ( IRIS) recalibration of Infrared Astronomical Satellite ( IRAS) data. We describe an optimized method for finding the dust temperature, emissivity spectral index, and optical depth using optical and near-infrared extinction maps. The creation of these temperature and extinction maps ( covering tens of square degrees of molecular clouds) is one of the first results from the ongoing Coordinated Molecular Probe Line Extinction Thermal Emission ( COMPLETE) Survey of Star-Forming Regions. However, while the extinctions derived from the IRIS emission maps are globally accurate, we warn that far-infrared emission is not a good proxy for extinction on the scale of 1 pixel (similar to 5'). In addition to describing the global dust properties of these clouds, we have found two particularly interesting features in the column density and temperature maps. In the Ophiuchus dark cloud complex, the new dust temperature map shows a little-known warm ( 25 K) dust ring with a 2 pc diameter. This shell is approximately centered on the B star rho Ophiuchus, 1 degrees north of the well-studied rho Oph star-forming cluster. In Perseus, the column density map shows a 10 pc diameter ring, a feature not apparent in the filamentary chain of clouds seen in molecular gas. These rings are further discussed in detail in our companion papers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schnee, SL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 26 TC 36 Z9 36 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 NOV 20 PY 2005 VL 634 IS 1 BP 442 EP 450 DI 10.1086/491729 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800038 ER PT J AU Uscanga, L Canto, J Curiel, S Anglada, G Torrelles, JM Patel, NA Gomez, JF Raga, AC AF Uscanga, L Canto, J Curiel, S Anglada, G Torrelles, JM Patel, NA Gomez, JF Raga, AC TI A 1 AU expanding water maser circular ring in the W75N(B)-VLA 2 shell SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual ( W75N); ISM : jets and outflows; masers; stars : formation ID STAR-FORMING REGIONS; H-II REGIONS; YOUNG STELLAR OBJECTS; H2O MASERS; BIPOLAR OUTFLOW; OH-EMISSION; W75N; PROTOSTARS; MOTION; W49N AB We have identified and modeled a remarkable water maser "microstructure'' of similar or equal to 1.1 mas size within the expanding shell of similar or equal to 0."16 size associated with the young stellar object W75 N(B)-VLA2. The water maser spots of this microstructure present a spatial distribution and line-of-sight velocity components that fit extremely well a circular ring of similar or equal to 1 AU radius expanding at similar or equal to 2.5 km s(-1). In particular, we have studied the spatio-kinematics and intensity distribution of the maser emission of an expanding ring observed at arbitrary angles. We construct position-velocity diagrams for the maser spots, calculating the maximum intensity as a function of the impact parameter and then comparing the results with the observations. This is the first time that such well-ordered spatio-kinematical behavior of the water masers is observed and modeled at the very small scale of similar or equal to 1 AU. The VLA2 maser shell is probably produced by an energetic stellar wind that compresses the ambient medium and drives a shock into it. Water maser emission is excited in flattened structures behind the shocks. We speculate that either these kinds of spatio-kinematical microstructures are produced by fluid instabilities within the shocked material or they correspond to nearly round cloudlets (turbulent eddies?) in the ambient medium that were flattened by the expanding shock. C1 Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. CSIC, Inst Ciencias Espac, E-08034 Barcelona, Spain. CSIC, Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. Royal Observ, United Kingdom Astron Technol Ctr, Edinburgh, Midlothian, Scotland. INTA, Lab Astrofis Espac & Fis Fundamental, E-28080 Madrid, Spain. Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. RP Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. EM lucero@astroscu.unam.mx; scuriel@astroscu.unam.mx; torrelles@ieec.fcr.es; npatel@iaa.es; jfg@iaaa.es; raga@nuclecu.unam.mx RI Uscanga, Lucero/C-5850-2014; Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 37 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP 468 EP 475 DI 10.1086/491783 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800041 ER PT J AU Williams, JP Andrews, SM Wilner, DJ AF Williams, JP Andrews, SM Wilner, DJ TI The masses of the Orion proplyds from submillimeter dust emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : individual (Orion nebula, Trapezium cluster); stars : formation ID CIRCUMSTELLAR DISKS; OB ASSOCIATIONS; GRAIN-GROWTH; NEBULA; OBJECTS; RESOLUTION; PHOTOEVAPORATION; TRAPEZIUM; OUTFLOWS; CLUSTER AB We have imaged the 880 mu m continuum emission from the "proplyds'' in the center of the Trapezium cluster in Orion using the Submillimeter Array with a beam size of 1.(")5 FWHM and an rms of 2.7 mJy. Five sources are detected with fluxes in the range 18-38 mJy, which includes dust emission from four proplyds and ionized gas from theta 1 Ori G. The total masses of the detected proplyds derived from their dust emission range from 1.3 x 10(-2) to 2.4 x 10(-2) M-circle dot, assuming a dust temperature of 20 K and mass opacity of 0.03 cm(2) g(-1). The 18 other proplyds within the field of view were not formally detected individually, but by combining the fluxes measured at their locations, an average flux of 1.1 mJy was determined for them on a statistical basis, corresponding to a mass of 8 x 10(-4) M-circle dot. The four detected proplyds have sufficient disk mass bound to their central stars to form planetary systems on the scale of our solar system. C1 Inst Astron, Honolulu, HI 96822 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, JP (reprint author), Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jpw@ifa.hawaii.edu; andrews@ifa.hawaii.edu; dwilner@cfa.harvard.edu RI Williams, Jonathan/B-1643-2009; OI Williams, Jonathan/0000-0001-5058-695X NR 36 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 NOV 20 PY 2005 VL 634 IS 1 BP 495 EP 500 DI 10.1086/444493 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800043 ER PT J AU Wood, MA Robertson, JR Simpson, JC Kawaler, SD O'Brien, MS Nather, RE Winget, DE Montgomery, MH Metcalfe, TS Jiang, XJ Leibowitz, EM Ibbetson, P O'Donoghue, D Zola, S Krzesinski, J Pajdosz, G Vauclair, G Dolez, N Chevreton, M Sullivan, DJ Kanaan, A Nitta, A AF Wood, MA Robertson, JR Simpson, JC Kawaler, SD O'Brien, MS Nather, RE Winget, DE Montgomery, MH Metcalfe, TS Jiang, XJ Leibowitz, EM Ibbetson, P O'Donoghue, D Zola, S Krzesinski, J Pajdosz, G Vauclair, G Dolez, N Chevreton, M Sullivan, DJ Kanaan, A Nitta, A TI DQ Herculis in profile: Whole Earth Telescope observations and smoothed particle hydrodynamics simulations of an edge-on cataclysmic variable system SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; hydrodynamics; novae, cataclysmic variables; stars : individual (DQ Her) ID ACCRETION DISKS; PERIOD CHANGES; CLOSE BINARIES; STARS; OSCILLATIONS; SUPERHUMPS; PULSATIONS; PHOTOMETRY; SPECTRUM; CYCLES AB The old nova DQ Herculis was the Whole Earth Telescope Northern Hemisphere target for the 1997 July campaign and was observed on four nights with the SARA 0.9 m telescope during 2003 June. We present updated ephemerides for the eclipse and 71 s timings. The Fourier transform displays power at the presumed white dwarf spin period of 71.0655 s, but no significant power at either 142 or 35.5 s. The mean pulsed light curve is obtained by folding on the orbital period modulus the mean ephemeris of the 71 s period, and from this we calculate an O - C phase diagram and amplitude versus orbital phase diagrams. In addition to the phase variations during eclipse ingress and egress, the WET data reveal significant phase variations outside of eclipse. These must result from the self-eclipse of a non-axisymmetric disk. We simulated the disk in DQ Her using smoothed particle hydrodynamics. We improve our effective spatial signal-to-noise ratio by combining 250 snapshots of the N = 20; 000 phase space solution over time to obtain a 5 million particle ensemble disk. From the surface shape of the ensemble disk, the radius and vertical height above the midplane of the rim of the reprocessing region can be derived as a function of azimuthal angle. From this profile we can calculate the O - C phase and amplitude diagrams as a function of inclination angle. The calculated O - C diagrams are a remarkably good match to the observed phase and amplitude variations of the 71 s signal. The best match is for inclination angle 89.degrees 7. C1 Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. Florida Inst Technol, SARA Observ, Melbourne, FL 32901 USA. Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. NASA, Range Syst Design & Dev Branch, Kennedy Space Ctr, FL 32899 USA. Iowa State Univ, Dept Phys, Ames, IA 50011 USA. Yale Univ, Dept Astron, New Haven, CT 06511 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Cambridge, Astron Inst, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chinese Acad Sci, Natl Astron Observ, Beijing Astron Observ, Beijing 100012, Peoples R China. Tel Aviv Univ, Dept Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. S African Astron Observ, ZA-7935 Cape Town, South Africa. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. Pedagog Univ, Mt Suhora Observ, PL-30024 Krakow, Poland. Univ Toulouse 3, Observ Midi Pyrenees, CNRS UMRS 5572, F-31400 Toulouse, France. DAEC, Observ Paris, F-92195 Meudon, France. Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. Apache Point Observ, Sunspot, NM 88349 USA. RP Wood, MA (reprint author), Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. EM wood@astro.fit.edu RI Metcalfe, Travis/A-9388-2008; OI Metcalfe, Travis/0000-0003-4034-0416; Kawaler, Steven/0000-0002-6536-6367 NR 57 TC 12 Z9 12 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP 570 EP 584 DI 10.1086/496957 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800050 ER PT J AU Cranmer, SR AF Cranmer, SR TI A statistical study of threshold rotation rates for the formation of disks around Be stars SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; stars : atmospheres; stars : early-type; stars : emission-line, Be; stars : fundamental parameters; stars : rotation ID DETACHED BINARY-SYSTEMS; MASS-LOSS RATES; B-TYPE STARS; DIFFERENTIAL ROTATION; STELLAR ROTATION; CIRCUMSTELLAR ENVELOPES; MERIDIONAL CIRCULATION; PHYSICAL-PROPERTIES; CONTINUUM EMISSION; MODEL ATMOSPHERES AB This paper presents a detailed statistical determination of the equatorial rotation rates of classical Be stars. The rapid rotation of Be stars is likely to be linked to the ejection of gas that forms dense circumstellar disks. The physical origins of these disks are not understood, although it is generally believed that the ability to spin up matter into a Keplerian disk depends on how close the stellar rotation speed is to the critical speed at which the centrifugal force cancels gravity. There has been recent disagreement between the traditional idea that Be stars rotate between 50% and 80% of their critical speeds and new ideas (inspired by the tendency for gravity darkening to mask rapid rotation at the equator) that their rotation may be very nearly critical. This paper utilizes Monte Carlo forward modeling to simulate distributions of the projected rotation speed (v sin i), taking into account gravity darkening, limb darkening, and observational uncertainties. A chi(2) minimization procedure was used to find the distribution parameters that best reproduce observed v sin i distributions from R. Yudin's database. Early-type (O7e-B2e) Be stars were found to exhibit a roughly uniform spread of intrinsic rotation speed that extends from 40%-60% up to 100% of critical. Late-type (B3e-A0e) Be stars exhibit progressively narrower ranges of rotation speed as the effective temperature decreases; the lower limit rises to reach critical rotation for the coolest Be stars. The derived lower limits on equatorial rotation speed represent conservative threshold rotation rates for the onset of the Be phenomenon. The significantly subcritical speeds found for early-type Be stars represent strong constraints on physical models of angular momentum deposition in Be star disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu NR 114 TC 70 Z9 70 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 NOV 20 PY 2005 VL 634 IS 1 BP 585 EP 601 DI 10.1086/491696 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800051 ER PT J AU Wargelin, BJ Beiersdorfer, P Neill, PA Olson, RE Scofield, JH AF Wargelin, BJ Beiersdorfer, P Neill, PA Olson, RE Scofield, JH TI Charge-exchange spectra of hydrogenic and He-like iron SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; X-rays : diffuse background; X-rays : general ID X-RAY-EMISSION; BEAM ION-TRAP; GALACTIC RIDGE; ELECTRON-CAPTURE; CHANDRA OBSERVATIONS; ENERGY-LEVELS; HELIUM-LIKE; COLLISIONS; ORIGIN; COMETS AB We present H-like Fe XXVI and He-like Fe XXV charge-exchange spectra resulting from collisions of highly charged iron with N-2 gas at an energy of similar to 10 eV amu(-1) in an electron beam ion trap. Although individual high-n emission lines are not resolved in our measurements, we observe that the most likely level for Fe+25 -> Fe+24 electron capture is n(max) similar to 9, in line with expectations, while the most likely value for Fe+26 -> Fe+25 charge exchange is significantly higher. In the Fe XXV spectrum, the K alpha emission feature dominates, whether produced via charge exchange or collisional excitation. The K alpha centroid is lower in energy for the former case than for the latter (6666 vs. 6685 eV, respectively), as expected because of the strong enhancement of emission from the forbidden and intercombination lines, relative to the resonance line, in charge-exchange spectra. In contrast, the Fe XXVI high-n Lyman lines have a summed intensity greater than that of Ly alpha and are substantially stronger than predicted from theoretical calculations of charge exchange with atomic H. We conclude that the angular momentum distribution resulting from electron capture using a multielectron target gas is significantly different from that obtained with H, resulting in the observed high-n enhancement. A discussion is presented of the relevance of our results to studies of diffuse Fe emission in the Galactic center and Galactic ridge, particularly with Astro-E2/Suzaku. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Dept Phys, Livermore, CA 94550 USA. Univ Nevada, Dept Phys, Reno, NV 89557 USA. Univ Missouri, Dept Phys, Rolla, MO 65401 USA. RP Wargelin, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM bwargelin@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 NR 43 TC 30 Z9 30 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP 687 EP 697 DI 10.1086/496874 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AF UT WOS:000233347800059 ER PT J AU An, T Goss, WM Zhao, JH Hong, XY Roy, S Rao, AP Shen, ZQ AF An, T Goss, WM Zhao, JH Hong, XY Roy, S Rao, AP Shen, ZQ TI Simultaneous multiwavelength observations of sagittarius A SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy : center; radio continuum : galaxies ID SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; SUBMILLIMETER ARRAY; 1 MILLIMETER; MILKY-WAY; ASTERISK; RADIO; SPECTRUM; VARIABILITY; CENTIMETER AB We observed Sgr A* using the Very Large Array (VLA) and the Giant Metrewave Radio Telescope (GMRT) at multiple centimeter and millimeter wavelengths on 2003 June 17. The measured flux densities of Sgr A*, together with those obtained from the Submillimeter Array (SMA) and the Keck II 10 m telescope on the same date, are used to construct a simultaneous spectrum of Sgr A* from 90 cm to 3.8 mu m. The simultaneous spectrum shows a spectral break at about 3.6 cm, a possible signature of synchrotron self-absorption of the strong radio outburst that occurred near epoch 2003 July 17. At 90 cm, the flux density of Sgr A* is 0.22 +/- 0.06 Jy, suggesting a sharp decrease in flux density at wavelengths longer than 47 cm. The spectrum at long cm wavelengths appears to be consistent with free-free absorption by a screen of ionized gas with a cutoff similar to 100 cm. This cutoff wavelength appears to be three times longer than that of similar to 30 cm suggested by Davies, Walsh, & Booth based on observations in 1974 and 1975. Our analysis suggests that the flux densities of Sgr A* at wavelengths longer than 30 cm could be attenuated and modulated by stellar winds from massive stars close to Sgr A*. C1 Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ctr Radio Astrophys, TIFR, Pune 411007, Maharashtra, India. RP An, T (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. EM antao@shao.ac.cn NR 26 TC 28 Z9 28 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP L49 EP L52 DI 10.1086/498687 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100013 ER PT J AU Chatterjee, S Goss, WM Brisken, WF AF Chatterjee, S Goss, WM Brisken, WF TI Radio emission from the double-pulsar system J0737-3039 revisited SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (J0737-3039A, J0737-3039B); stars : neutron ID GREEN-BANK-TELESCOPE; XMM-NEWTON; MODULATION; ECLIPSE AB The double pulsar J0737 - 3039 is the only known system in which the relativistic wind emitted by a radio pulsar demonstrably interacts with the magnetosphere of another one. We report radio interferometric observations of the J0737 - 3039 system with the VLA at three wavelengths, with each observation spanning a full binary orbit. We detect J0737 - 3039 at 1.6 and 4.8 GHz, derive a spectral index of -, and place an upper 2.3 +/- 0.2 limit on its flux density at 8.4 GHz. Orbital modulation is detected in the 1.6 GHz data, with a significance of similar to 2 sigma. Both orbital phase-resolved and phase-averaged measurements at 1.6 GHz are consistent with the entire flux density arising from the pulsed emission of the two pulsars. Contrary to prior results, we find no evidence for unpulsed emission, and limit it to less than 0.5 mJy ( 5 sigma). C1 Natl Radio Astron Observ, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Chatterjee, S (reprint author), Natl Radio Astron Observ, 60 Garden St, Cambridge, MA 02138 USA. EM schatterjee@cfa.harvard.edu; mgoss@aoc.nrao.edu; wbrisken@aoc.nrao.edu NR 14 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP L101 EP L104 DI 10.1086/498822 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100026 ER PT J AU Gelfand, JD Lyubarsky, YE Eichler, D Gaensler, BM Taylor, GB Granot, J Newton-McGee, KJ Ramirez-Ruiz, E Kouveliotou, C Wijers, RAMJ AF Gelfand, JD Lyubarsky, YE Eichler, D Gaensler, BM Taylor, GB Granot, J Newton-McGee, KJ Ramirez-Ruiz, E Kouveliotou, C Wijers, RAMJ TI A rebrightening of the radio nebula associated with the 2004 December 27 giant flare from SGR 1806-20 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (SGR 1806-20); neutrinos; radio continuum : stars; shock waves; stars : magnetic fields; stars : neutron ID X-RAY PULSAR; MAGNETAR SGR-1806-20; RADIATIVE MECHANISM; ACCELERATION; CONSTRAINTS; REPEATERS; EMISSION; DISTANCE; SHOCK AB The 2004 December 27 giant gamma-ray flare detected from the magnetar SGR 1806 - 20 created an expanding radio nebula that we have monitored with the Australia Telescope Compact Array and the Very Large Array. These data indicate that there was an increase in the observed flux similar to 25 days after the initial flare that lasted for similar to 8 days, which we believe is the result of ambient material swept up and shocked by this radio nebula. For a distance to SGR 1806 - 20 of 15 kpc, using the properties of this rebrightening, we infer that the initial blast wave was dominated by baryonic material of mass M greater than or similar to 10(24.5) g. For an initial expansion velocity v similar to 0.7c derived in an accompanying paper), we infer that this material had an initial kinetic energy E greater than or similar to 10(44.5) ergs. If this material originated from the magnetar itself, it may have emitted a burst of ultra - high-energy (E greater than or similar to 1 TeV) neutrinos far brighter than that expected from other astrophysical sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Inst Adv Study, Princeton, NJ 08540 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Gelfand, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; LYUBARSKY, YURY/F-2362-2012; Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Gaensler, Bryan/0000-0002-3382-9558 NR 23 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 NOV 20 PY 2005 VL 634 IS 1 BP L89 EP L92 DI 10.1086/498643 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100023 ER PT J AU Laycock, S Grindlay, J van den Berg, M Zhao, P Hong, J Koenig, X Schlegel, EM Persson, SE AF Laycock, S Grindlay, J van den Berg, M Zhao, P Hong, J Koenig, X Schlegel, EM Persson, SE TI Constraining the nature of the galactic center X-ray source population SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; X-rays : binaries ID TRANSIENT; BINARIES; STARS AB We searched for infrared counterparts to the cluster of X-ray point sources discovered by Chandra in the Galactic center region (GCR). While the sources could be white dwarfs, neutron stars, or black holes accreting from stellar companions, their X-ray properties are consistent with magnetic cataclysmic variables (CVs), or high-mass X-ray binaries (HMXBs) at low accretion rates. A direct way to decide between these possibilities, and hence between alternative formation scenarios, is to measure or constrain the luminosity distribution of the companions. Using infrared (J, H, K, Br gamma) imaging, we searched for counterparts corresponding to typical HMXB secondaries: spectral type B0 V with K < 15 at the GCR. We found no significant excess of bright stars in Chandra error circles, indicating that HMXBs are not the dominant X-ray source population and that they account for fewer than 10% of the hardest X-ray sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. RP Laycock, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Koenig, Xavier/0000-0002-9478-4170 NR 16 TC 32 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP L53 EP L56 DI 10.1086/498821 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100014 ER PT J AU Lefevre, L Marchenko, SV Moffat, AFJ Chene, AN Smith, SR St-Louis, N Matthews, JM Kuschnig, R Guenther, DB Poteet, CA Rucinski, SM Sasselov, D Walker, GAH Weiss, WW AF Lefevre, L Marchenko, SV Moffat, AFJ Chene, AN Smith, SR St-Louis, N Matthews, JM Kuschnig, R Guenther, DB Poteet, CA Rucinski, SM Sasselov, D Walker, GAH Weiss, WW TI Oscillations in the massive Wolf-Rayet star WR 123 with the MOST satellite SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (HD 177230=WR 123); stars : oscillations; stars : Wolf-Rayet ID TIME-SERIES ANALYSIS; ENIGMATIC WN8 STARS; FUNDAMENTAL PARAMETERS; WIND INHOMOGENEITIES; PHOTOMETRY; VARIABILITY; SPECTRUM AB We present the results of intensive visual-broadband photometric monitoring of the highly variable WN8 Wolf-Rayet star WR 123, obtained by the MOST ( Microvariability and Oscillations of STars) satellite. This first Canadian astronomical space telescope observed WR 123 for 38 days nonstop during 2004 June and July. Fourier analysis shows that no periodic signal is stable for more than several days in the low-frequency domain ( f < 1 day(-1)), where most of the stochastic power is contained. Also, no significant variability is seen in the high-frequency domain ( 10 day(-1) < f < 1400 day(-1)) down to the level of 0.2 mmag, an order of magnitude lower than theoretical predictions for strange-mode pulsations. On the other hand, there seems to be a relatively stable 9.8 hr periodic signal present throughout the whole run. This period is probably too short to represent the axial rotation of the star, unless it is related to multiple substructures equidistantly spread along the stellar equator. It is also too short to be orbital in nature; it is more likely to be related to pulsational instablilities ( although with a much longer period than expected), thus finally revealing a possible fundamental driver behind the highly variable wind of this object, and others of similar type. C1 Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Observ Strasbourg, F-67000 Strasbourg, France. Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Lefevre, L (reprint author), Univ Montreal, Dept Phys, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM lefevre@astro.umontreal.ca NR 26 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP L109 EP L112 DI 10.1086/498393 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100028 ER PT J AU Megeath, ST Hartmann, L Luhman, KL Fazio, GG AF Megeath, ST Hartmann, L Luhman, KL Fazio, GG TI Spitzer/IRAC photometry of the eta Chameleontis association SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; planetary systems : protoplanetary disks; stars : pre-main-sequence ID TW-HYDRAE ASSOCIATION; YOUNG OPEN CLUSTER; ARRAY CAMERA IRAC; CHAMAELEONTIS CLUSTER; CIRCUMSTELLAR DISKS; TAURI STARS; CENSUS; SPECTROSCOPY; ACCRETION; EVOLUTION AB We present IRAC 3.6, 4.5, 5.8, and 8 mm photometry for the 17 A-, K-, and M-type members of the h Chameleontis association. These data show infrared excesses toward six of the 15 K and M stars, indicating the presence of circumstellar disks around 40% of the stars with masses of 0.1 - 1 M-circle dot. The two A stars show no infrared excesses. The excess emission around one of the stars is comparable to the median excess for classical T Tauri stars in the Taurus association; the remaining five show comparatively weak excess emission. Taking into account published Ha spectroscopy that shows that five of the six stars are accreting, we argue that the disks with weak mid-infrared excesses are disks in which the inner disks have been largely depleted of small grains by grain growth or, in one case, the small grains have settled to the midplane. This suggests that h Cha has a much higher fraction of disks caught in the act of transitioning into optically thin disks than that measured in younger clusters and associations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Penn State Univ, Dept Phys & Astron, University Pk, PA 16802 USA. RP Megeath, ST (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tmegeath@cfa.harvard.edu NR 31 TC 51 Z9 51 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP L113 EP L116 DI 10.1086/498503 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100029 ER PT J AU Sridharan, TK Beuther, H Saito, M Wyrowski, F Schilke, P AF Sridharan, TK Beuther, H Saito, M Wyrowski, F Schilke, P TI High-mass starless cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared : ISM; ISM : clouds; ISM : molecules; ISM : structure; stars : formation ID ULTRACOMPACT HII-REGIONS; PROTOSTELLAR CANDIDATES; CIRCUMSTELLAR ENVIRONMENTS; MOLECULAR CLOUD; DUST CONTINUUM; EMISSION; MILLIMETER; AMMONIA; SAMPLE; EXTINCTION AB We report the identification of a sample of potential high-mass starless cores (HMSCs). The cores were discovered by comparing images of fields containing candidate high-mass protostellar objects (HMPOs) at 1.2 mm and mid-infrared (MIR; 8.3 mu m) wavelengths. While the HMPOs are detected at both wavelengths, several cores emitting at 1.2 mm in the same fields show absorption or no emission at the MIR wavelength. We argue that the absorption is caused by cold dust. The estimated masses of a few times 10(2) - 10(3) M-circle dot and the lack of IR emission suggest that they may be massive cold cores in a prestellar phase, which could form massive stars. Ammonia observations indicate smaller velocity dispersions and lower rotation temperatures compared with HMPOs and ultracompact H II regions, suggesting a quiescent prestellar stage. We propose that these newly discovered cores are good candidates for the HMSC stage in high-mass star formation. This sample of cores will allow us to study the high-mass star and cluster formation processes at the earliest evolutionary stages. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ Japan, Tokyo 1818588, Japan. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Sridharan, TK (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM tksridha@cfa.harvard.edu; beuther@mpia-hd.mpg.de; Masao.Saito@nao.ac.jp; wyrowski@mpifr-bonn.mpg.de; schilke@mpifr-bonn.mpg.de NR 28 TC 78 Z9 78 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 NOV 20 PY 2005 VL 634 IS 1 BP L57 EP L60 DI 10.1086/498644 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100015 ER PT J AU Taylor, GB Gelfand, JD Gaensler, BM Granot, J Kouveliotou, C Fender, RP Ramirez-Ruiz, E Eichler, D Lyubarsky, YE Garrett, M Wijers, RAMJ AF Taylor, GB Gelfand, JD Gaensler, BM Granot, J Kouveliotou, C Fender, RP Ramirez-Ruiz, E Eichler, D Lyubarsky, YE Garrett, M Wijers, RAMJ TI The growth, polarization, and motion of the radio afterglow from the giant flare from SGR 1806-20 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (SGR 1806-20); radio continuum : general; stars : flare; stars : neutron; stars : winds, outflows ID MAGNETAR SGR-1806-20; DISTANCE; NEBULA AB The extraordinary giant flare ( GF) of 2004 December 27 from the soft gamma repeater SGR 1806 - 20 was followed by a bright radio afterglow. We present an analysis of VLA observations of this radio afterglow from SGR 1806 - 20, consisting of previously reported 8.5 GHz data covering days 7 - 20 after the GF, plus new observations at 8.5 and 22 GHz from day 24 to 81. We detect motion in the flux centroid of the afterglow, at an average velocity of ( 0.26 +/- 0.03) c ( assuming a distance of 15 kpc) at a position angle of - 45 degrees. This motion, in combination with the growth and polarization measurements, suggests an asymmetric outflow, mainly from one side of the magnetar. We find a deceleration in the expansion, from similar to 9 to < 5 mas day(-1). The time of deceleration is roughly coincident with the rebrightening in the radio light curve, as expected to result when the ejecta from the GF sweeps up enough of the external medium and transitions from a coasting phase to the Sedov-Taylor regime. The radio afterglow is elongated and maintains a 2 : 1 axis ratio with an average position angle of - 40 degrees ( north through east), oriented perpendicular to the average intrinsic linear polarization angle. C1 Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Inst Adv Study, Princeton, NJ 08540 USA. Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. VLBI Europe, Joint Inst, NL-7990 AA Dwingeloo, Netherlands. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Taylor, GB (reprint author), Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. RI Gaensler, Bryan/F-8655-2010; LYUBARSKY, YURY/F-2362-2012; Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Wijers, Ralph/0000-0002-3101-1808; Gaensler, Bryan/0000-0002-3382-9558 NR 16 TC 24 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP L93 EP L96 DI 10.1086/491648 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100024 ER PT J AU Wagg, J Wilner, DJ Neri, R Downes, D Wiklind, T AF Wagg, J Wilner, DJ Neri, R Downes, D Wiklind, T TI HCN J=5-4 emission in APM 08279+5255 At z=3.91 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : high-redshift; galaxies : ISM; quasars : emission lines; quasars : individual (APM 08279+5255) ID ABSORPTION-LINE QUASAR; DENSE MOLECULAR GAS; ULTRALUMINOUS GALAXIES; HIGH-REDSHIFT; STAR-FORMATION; APM-08279+5255; SPECTROSCOPY; CHEMISTRY; NGC-1068; CO AB We detect HCN J = 5-4 emission from the ultraluminous quasar APM 08279 + 5255 at z= 3.911 using the IRAM Plateau de Bure Interferometer. This object is strongly gravitationally lensed, yet still thought to be one of the most intrinsically luminous objects in the universe. The new data imply a line luminosity L'(HCN(J + 5-4)) = (4.0 +/- 0.5) x 10(10) K km s(-1) pc(2). The similar to 440 km s(-1) FWHM of the HCN J line matches that of the previously observed high-J CO lines in this object and suggests that the emission from both species emerges from the same region: a warm, dense circumnuclear disk. Simple radiative transfer models suggest an enhanced abundance of HCN relative to CO in the nuclear region of APM 08279 + 5255, perhaps due to increased ionization, or possibly the selective depletion of oxygen. The ratio of far-infrared luminosity to HCN luminosity is at the high end of the range found for nearby star-forming galaxies, but is comparable to that observed in the few high-redshift objects detected in the HCN J = 1-0 line. This is the first clear detection of high-J HCN emission redshifted into the 3 mm atmospheric window. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAOE, Puebla, Mexico. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. Space Telescope Sci Inst, ESA, Space Telescope Div, Baltimore, MD 21218 USA. RP Wagg, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jwagg@cfa.harvard.edu NR 31 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2005 VL 634 IS 1 BP L13 EP L16 DI 10.1086/498849 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985AI UT WOS:000233348100004 ER PT J AU Piperno, DR Sues, HD AF Piperno, DR Sues, HD TI Dinosaurs dined on grass SO SCIENCE LA English DT Editorial Material ID PHYTOLITH C1 Natl Museum Nat Hist, Washington, DC 20560 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Piperno, DR (reprint author), Natl Museum Nat Hist, Washington, DC 20560 USA. EM pipernod@si.edu NR 14 TC 29 Z9 37 U1 3 U2 20 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 18 PY 2005 VL 310 IS 5751 BP 1126 EP 1128 DI 10.1126/science.1121020 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 986GE UT WOS:000233437300028 PM 16293745 ER PT J AU Feuerbacher, S Santra, R AF Feuerbacher, S Santra, R TI Calculating molecular Rydberg states using the one-particle Green's function: Application to HCO and C(NH2)(3) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID COMPLEX ABSORBING POTENTIALS; ELECTRON-ION RECOMBINATION; FINITE FERMI SYSTEMS; DISSOCIATIVE RECOMBINATION; IONIZATION-POTENTIALS; PERTURBATION THEORY; PROPAGATOR THEORY; BASIS-SETS; ATOMS; SCATTERING AB A simple but accurate and computationally efficient method for routine ab initio calculations of molecular Rydberg states is described. The method, which can be applied to Rydberg states associated with a nondegenerate ion core, consists in the self-consistent solution of an effective one-electron problem. First, the restricted Hartree-Fock problem of the ion core is solved. The orbital energies and certain two-electron Coulomb matrix elements with respect to the molecular orbital basis are then used to construct an energy-dependent many-body correction to the Hartree-Fock mean field. This correction is derived from the Dyson equation satisfied by the one-particle Green's function. The method is applied to calculate Rydberg potential-energy curves of HCO. The presented data confirm and extend recent large-scale multireference configuration-interaction calculations and help develop a detailed theoretical description of the astrophysically important dissociative recombination of a low-energy electron with HCO+. As further illustration of the utility of the method, the first ab initio calculations of the excited states of an electron bound to the guanidinium cation [C(NH2)(3)](+) are reported. C1 Heidelberg Univ, Inst Chem Phys, D-69120 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Feuerbacher, S (reprint author), Heidelberg Univ, Inst Chem Phys, Neuenheimer Feld 229, D-69120 Heidelberg, Germany. RI Santra, Robin/E-8332-2014 OI Santra, Robin/0000-0002-1442-9815 NR 70 TC 3 Z9 3 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 15 PY 2005 VL 123 IS 19 AR 194310 DI 10.1063/1.2122687 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 985CH UT WOS:000233353200022 PM 16321091 ER PT J AU West-Eberhard, MJ AF West-Eberhard, MJ TI Phenotypic accommodation: Adaptive innovation due to developmental plasticity SO JOURNAL OF EXPERIMENTAL ZOOLOGY PART B-MOLECULAR AND DEVELOPMENTAL EVOLUTION LA English DT Article; Proceedings Paper CT Symposium on Morphological Innovation CY 2003 CL New Orleans, LA SP Soc Integrat & Comparat Biol ID UPRIGHT POSTURE; CICHLID FISHES; BIPEDAL GAIT; GOAT BORN; EVOLUTION; PISCES; DIET; CONSTRAINTS; MORPHOLOGY; BEHAVIOR AB Phenotypic accommodation is adaptive adjustment, without genetic change, of variable aspects of the phenotype following a novel input during development. Phenotypic accommodation can facilitate the evolution of novel morphology by alleviating the negative effects of change, and by giving a head start to adaptive evolution in a new direction. Whether induced by a mutation or a novel environmental factor, innovative morphological form comes from ancestral developmental responses, not from the novel inducing factor itself. Phenotypic accommodation is the result of adaptive developmental responses, so the novel morphologies that result are not "random" variants, but to some degree reflect past functionality. Phenotypic accommodation is the first step in a process of Darwinian adaptive evolution, or evolution by natural selection, where fitness differences among genetically variable developmental variants cause phenotype-frequency change due to gene-frequency change. C1 Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. RP West-Eberhard, MJ (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. EM mjwe@sent.com NR 52 TC 119 Z9 119 U1 3 U2 66 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1552-5007 J9 J EXP ZOOL PART B JI J. Exp. Zool. Part B PD NOV 15 PY 2005 VL 304B IS 6 BP 610 EP 618 DI 10.1002/jez.b.21071 PG 9 WC Evolutionary Biology; Developmental Biology; Zoology SC Evolutionary Biology; Developmental Biology; Zoology GA 990RJ UT WOS:000233760600012 PM 16161068 ER PT J AU Aiello, A AF Aiello, A TI Secret weapons: Defenses of insects, spiders, scorpions, and other many-legged creatures. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 1 U2 2 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 15 PY 2005 VL 130 IS 19 BP 92 EP 92 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 005ZL UT WOS:000234864800240 ER PT J AU Camargo, JMF Roubik, DW AF Camargo, JMF Roubik, DW TI Neotropical Meliponini: Paratrigonoides mayri, new genus and species from western Colombia (Hymenoptera, Apidae, Apinae) and phylogeny of related genera SO ZOOTAXA LA English DT Article DE stingless bees; new genus; taxonomy; Neotropics AB Paratrigonoides mayri gen. nov., sp. nov., from the Cauca Valley region of Antioquia, Colombia, is described. It resembles Paratrigona, especially species of the P. lineata group. The new genus is recognized by a combination of bidentate mandibles, the keirotrichiate area of tibia III not depressed on the posterior edge (plesiomorphies), yellow markings flanking the frontal median line and two spots below the lateral ocelli, supraclypeal area partly covering antennal sockets, and by the upper part of the preoccipital ridge lamellate and bordered by a row of robust hairs ( autapomorphies). The result of a cladistic analysis suggests Paratrigona + Aparatrigona form the sister-group of Paratrigonoides gen. nov. C1 Univ Sao Paulo, Fac Filosofia Ciencias & Letras Ribeirao Pret, BR-14040901 Ribeirao Preto, SP, Brazil. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Camargo, JMF (reprint author), Univ Sao Paulo, Fac Filosofia Ciencias & Letras Ribeirao Pret, Av Bandeirantes 3900, BR-14040901 Ribeirao Preto, SP, Brazil. EM jmfdcama@usp.br; roubikd@si.edu NR 16 TC 9 Z9 9 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 NOV 15 PY 2005 IS 1081 BP 33 EP 45 PG 13 WC Zoology SC Zoology GA 984EP UT WOS:000233285600002 ER PT J AU Wing, SL Harrington, GJ Smith, FA Bloch, JI Boyer, DM Freeman, KH AF Wing, SL Harrington, GJ Smith, FA Bloch, JI Boyer, DM Freeman, KH TI Transient floral change and rapid global warming at the Paleocene-Eocene boundary SO SCIENCE LA English DT Article ID CARBON-ISOTOPE EXCURSION; THERMAL MAXIMUM; BIGHORN BASIN; LATEST PALEOCENE; NORTH-AMERICA; OXYGEN-ISOTOPE; CLIMATE-CHANGE; FOSSIL LEAVES; TEMPERATURE; PLANT AB Rapid global warming of 5 degrees to 10 degrees C during the Paleocene-Eocene Thermal Maximum (PETM) coincided with major turnover in vertebrate faunas, but previous studies have found little floral change. Plant fossils discovered in Wyoming, United States, show that PETM floras were a mixture of native and migrant lineages and that plant range shifts were large and rapid (occurring within 10,000 years). Floral composition and leaf shape and size suggest that climate warmed by similar to 5 degrees C during the PETM and that precipitation was low early in the event and increased later. Floral response to warming and/or increased atmospheric CO2 during the PETM was comparable in rate and magnitude to that seen in postglaciat floras and to the predicted effects of anthropogenic carbon release and climate change on future vegetation. C1 Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Birmingham, Dept Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Florida Museum Nat Hist, Div Vertebrate Paleontol, Gainesville, FL 32611 USA. SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY 11794 USA. RP Wing, SL (reprint author), Smithsonian Museum Nat Hist, Dept Paleobiol, 10th St & Constitut Ave NW, Washington, DC 20560 USA. EM wings@si.edu RI McInerney, Francesca/B-7894-2009; Freeman, Katherine/H-5140-2011; OI McInerney, Francesca/0000-0002-2020-6650; Freeman, Katherine/0000-0002-3350-7671; Wing, Scott/0000-0002-2954-8905 NR 48 TC 257 Z9 270 U1 9 U2 98 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 NOV 11 PY 2005 VL 310 IS 5750 BP 993 EP 996 DI 10.1126/science.1116913 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 984YN UT WOS:000233343400036 PM 16284173 ER PT J AU Kotov, O Vikhlinin, A AF Kotov, O Vikhlinin, A TI XMM-Newton observations of evolution of cluster X-ray scaling relations at z=0.4-0.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; surveys; X-rays : galaxies ID M-T RELATION; GALAXY CLUSTERS; TEMPERATURE PROFILES; NEARBY CLUSTERS; DARK-MATTER; PROJECT; CHANDRA; SAMPLE; ASCA AB We present a spatially resolved analysis of the temperature and gas density profiles of galaxy clusters at z = 0.4-0.7 observed with XMM-Newton. These data are used to derive the total cluster mass within the radius r(500) without assuming isothermality and also to measure the average temperature and total X-ray luminosity, excluding the cooling cores. We derive the high-redshift M-T and L-T relations and compare them with the local measurements. The high-redshift L-T relation has low scatter and evolves as L proportional to (1 + z)(1.8+/-0.3) for a fixed T, in agreement with several previous Chandra and XMM-Newton studies (Vikhlinin et al., Lumb et al., and Maughan et al.). The observed evolution of the M-T relation follows M-500 proportional to E(z)(-alpha), where we measure alpha = 0.88 +/- 0.23. This is in agreement with predictions of the self-similar theory, alpha = 1. C1 Space Res Inst, Moscow, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kotov, O (reprint author), Space Res Inst, Moscow, Russia. NR 31 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2005 VL 633 IS 2 BP 781 EP 790 DI 10.1086/433170 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 983NK UT WOS:000233239000022 ER PT J AU Loeb, A Reid, MJ Brunthaler, A Falcke, H AF Loeb, A Reid, MJ Brunthaler, A Falcke, H TI Constraints on the proper motion of the Andromeda galaxy based on the survival of its satellite M33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; dark matter; galaxies : individual (M31, M33); galaxies : interactions; Local Group ID MILKY-WAY; NEARBY GALAXIES; DISK; HISTORY; MASS AB A major uncertainty in the dynamical history of the Local Group of galaxies originates from the unknown transverse speed of the Andromeda galaxy (M31) relative to the Milky Way. We show that the recent VLBA measurement of the proper motion of Andromeda's satellite, M33, severely constrains the possible values of M31' s proper motion. The condition that M33' s stellar disk has not been tidally disrupted by either M31 or the Milky Way over the past 10 billion years favors a proper motion amplitude of 100 +/- 20 km s(-1) for M31 with the quadrant of a negative velocity component along right ascension and a positive component along declination strongly ruled out. This inference can be tested by future astrometric measurements with SIM, Gaia, or the SKA. Our results imply that the dark halos of Andromeda and the Milky Way will pass through each other within the next 5 - 10 billion years. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands. Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Loeb, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 27 TC 43 Z9 44 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2005 VL 633 IS 2 BP 894 EP 898 DI 10.1086/491644 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 983NK UT WOS:000233239000030 ER PT J AU Koo, BC Lee, JJ Seward, FD Moon, DS AF Koo, BC Lee, JJ Seward, FD Moon, DS TI Chandra observations of the W51C supernova remnant SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (W51); supernova remnants; X-rays : ISM ID X-RAY SOURCE; MOLECULAR CLOUD; GALACTIC RIDGE; ROSAT OBSERVATIONS; NEBULA; G21.5-0.9; CTB-80; COMPLEX; ASCA; EMISSION AB We present the results of Chandra ACIS observations of the supernova remnant (SNR) W51C. The remnant is located in the cross section of the Sagittarius arm, and the Chandra images present a superb X-ray view of this complex region including the massive star-forming region W51B. The properties of thermal diffuse SNR emission are consistent with the results of previous studies except that an enhanced abundance of sulfur is required. It is found that the ASCA hard X-ray source CXO J192318.5+ 1403035, proposed to be a pulsar wind nebula, is composed of a relatively bright core surrounded by an extended (similar to 7.0 x 2.5 pc) diffuse envelope. The core contains a compact (< 0.1 pc) source at the center. The X-ray spectrum of CXO J192318.5+ 1403035 can be fitted by a power-law emission model with Gamma = 1.82(-0.29)(+0.28), and the implied X-ray (0.2 - 4.0 keV) luminosity is 5 x 10(33) ergs s(-1). The core contributes similar to 20% of the total luminosity. The core-envelope structure and its spectral properties support CXO J192318.5+ 140305 as a pulsar-wind nebula associated with the SNR W51C. There is also enhanced radio emission coincident with the source. It is conceivable that the central compact source might harbor a pulsar. However, the large extent and the hardening of X-rays at the extreme boundaries need to be explained. We have searched for the Br gamma line from the ionized gas associated with the source, but no emission was detected. C1 Seoul Natl Univ, SEES, Astron Program, Seoul 151742, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Koo, BC (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Kanagawa 2298510, Japan. EM koo@astrohi.snu.ac.kr; jjlee@astro.snu.ac.kr; fds@head.cfa.harvard.edu; moon@srl.caltech.edu NR 30 TC 20 Z9 20 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 NOV 10 PY 2005 VL 633 IS 2 BP 946 EP 952 DI 10.1086/491468 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 983NK UT WOS:000233239000036 ER PT J AU Hickox, RC Vrtilek, SD AF Hickox, RC Vrtilek, SD TI Pulse-phase spectroscopy of SMC X-1 with Chandra and XMM-Newton: Reprocessing by a precessing disk? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars : individual (SMC X-1); stars : neutron; X-rays : binaries ID X-RAY PULSARS; SOFT SPECTRAL COMPONENT; MAGNETIC NEUTRON STARS; 35 DAY EVOLUTION; LMC X-4; RESOLVED-SPECTROSCOPY; ROSAT OBSERVATIONS; GINGA OBSERVATIONS; ACCRETION DISCS; CENTAURUS X-3 AB We present pulse-phase X-ray spectroscopy of the high-mass X-ray pulsar SMC X-1 from five different epochs, using Chandra X-Ray Observatory ACIS-S and XMM-Newton EPIC pn data. The X-ray spectrum consistently shows two distinct components, a hard power law and a soft blackbody with kT(BB) similar to 0.18 keV. For all five epochs the hard component shows a simple double-peaked pulse shape and also a variation in the power-law slope, which becomes harder at maximum flux and softer at minimum flux. For the soft component, the pulse profile changes between epochs in both shape and phase relative to the power-law pulses. The soft component is likely produced by reprocessing of the hard X-ray pulsar beam by the inner accretion disk. We use a model of a twisted inner disk, illuminated by the rotating X-ray pulsar beam, to simulate pulsations in the soft component due to this reprocessing. We find that for some disk and beam geometries, precession of an illuminated accretion disk can roughly reproduce the observed long-term changes in the soft-pulse profiles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hickox, RC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 55 TC 9 Z9 9 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2005 VL 633 IS 2 BP 1064 EP 1075 DI 10.1086/491596 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 983NK UT WOS:000233239000047 ER PT J AU Bourke, TL Crapsi, A Myers, PC Evans, NJ Wilner, DJ Huard, TL Jorgensen, JK Young, CH AF Bourke, TL Crapsi, A Myers, PC Evans, NJ Wilner, DJ Huard, TL Jorgensen, JK Young, CH TI Discovery of a low-mass bipolar molecular outflow from L1014-IRS with the submillimeter array SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (L1014, L1014-IRS); ISM : jets and outflows; stars : formation; stars : low-mass, brown dwarfs; techniques : interferometric ID YOUNG STELLAR OBJECTS; DARK CLOUDS; PROTOSTAR; EVOLUTION; TAURUS; FLOWS; LINE AB Using the Submillimeter Array, we report the discovery of a compact low-mass bipolar molecular outflow from L1014-IRS and confirm its association with the L1014 dense core at 200 pc. Consequently, L1014-IRS is the lowest luminosity (L similar to 0.09 L-.), and perhaps the lowest mass, source known to be driving a bipolar molecular outflow, which is one of the smallest known in size (similar to 500 AU), mass (<10(-4) M-.), and energetics (e.g., with a M, force <10(-7) M-. km s(-1) yr(-1)). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Univ Texas, Austin, TX 78712 USA. Nicholls State Univ, Thibodaux, LA 70310 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tbourke@cfa.harvard.edu NR 17 TC 60 Z9 60 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 NOV 10 PY 2005 VL 633 IS 2 BP L129 EP L132 DI 10.1086/498449 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 983NL UT WOS:000233239200017 ER PT J AU Heitsch, F Burkert, A Hartmann, LW Slyz, AD Devriendt, JEG AF Heitsch, F Burkert, A Hartmann, LW Slyz, AD Devriendt, JEG TI Formation of structure in molecular clouds: A case study SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : kinematics and dynamics; methods : numerical; stars : formation; turbulence ID THERMALLY BISTABLE FLOW; STAR-FORMATION; INTERSTELLAR TURBULENCE; DYNAMICAL CONDENSATION; SUPERSONIC TURBULENCE; FRAGMENTATION; INSTABILITIES; COLLAPSE; TIME; HYDRODYNAMICS AB Molecular clouds (MCs) are highly structured and turbulent. Colliding gas streams of atomic hydrogen have been suggested as a possible source of MCs, imprinting the filamentary structure as a consequence of dynamical and thermal instabilities. We present a two-dimensional numerical analysis of MC formation via converging H I flows. Even with modest flow speeds and completely uniform inflows, nonlinear density perturbations arise as possible precursors of MCs. Thus, we suggest that MCs are inevitably formed with substantial structure, e. g., strong density and velocity fluctuations, which provide the initial conditions for subsequent gravitational collapse and star formation in a variety of Galactic and extragalactic environments. C1 Univ Observ Munich, D-81679 Munich, Germany. Univ Wisconsin, Madison, WI 53706 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ecole Normale Super Lyon, Ctr Rech Astron Lyon, F-69364 Lyon, France. Observ Lyon, Ctr Rech Astron Lyon, F-69561 St Genis Laval, France. RP Heitsch, F (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. NR 40 TC 104 Z9 104 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 NOV 10 PY 2005 VL 633 IS 2 BP L113 EP L116 DI 10.1086/498413 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 983NL UT WOS:000233239200013 ER PT J AU Tominaga, N Tanaka, M Nomoto, K Mazzali, PA Deng, J Maeda, K Umeda, H Modjaz, M Hicken, M Challis, P Kirshner, RP Wood-Vasey, WM Blake, CH Bloom, JS Skrutskie, MF Szentgyorgyi, A Falco, EE Inada, N Minezaki, T Yoshii, Y Kawabata, K Iye, M Anupama, GC Sahu, DK Prabhu, TP AF Tominaga, N Tanaka, M Nomoto, K Mazzali, PA Deng, J Maeda, K Umeda, H Modjaz, M Hicken, M Challis, P Kirshner, RP Wood-Vasey, WM Blake, CH Bloom, JS Skrutskie, MF Szentgyorgyi, A Falco, EE Inada, N Minezaki, T Yoshii, Y Kawabata, K Iye, M Anupama, GC Sahu, DK Prabhu, TP TI The unique type Ib supernova 2005bf: A WN star explosion model for peculiar light curves and spectra SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : Wolf-Rayet; supernovae : general; supernovae : individual (Cassiopeia A, SN 2005bf) ID SN 2002AP; HYPERNOVA; NUCLEOSYNTHESIS; EVOLUTION; ABUNDANCE; HYDROGEN; HELIUM; NICKEL AB Observations and modeling for the light curve (LC) and spectra of supernova (SN) 2005bf are reported. This SN showed unique features: the LC had two maxima, and declined rapidly after the second maximum, while the spectra showed strengthening He lines whose velocity increased with time. The double-peaked LC can be reproduced by a double-peaked Ni-56 distribution, with most Ni-56 at low velocity and a small amount at high velocity. The rapid postmaximum decline requires a large fraction of the gamma-rays to escape from the Ni-56-dominated region, possibly because of low-density "holes." The presence of Balmer lines in the spectrum suggests that the He layer of the progenitor was substantially intact. Increasing gamma-ray deposition in the He layer due to enhanced gamma-ray escape from the Ni-56-dominated region may explain both the delayed strengthening and the increasing velocity of the He lines. The SN has massive ejecta (similar to 6-7 M.), normal kinetic energy [similar to(1.0-1.5) x 10(51) ergs], a high peak bolometric luminosity (similar to 5 x 10(42) ergs s(-1)) for an epoch as late as similar to 40 days, and a large Ni-56 mass (similar to 0.32 M.). These properties and the presence of a small amount of H suggest that the progenitor was initially massive (M similar to 25-30 M.) and had lost most of its H envelope, and was possibly a WN star. The double-peaked Ni-56 distribution suggests that the explosion may have formed jets that did not reach the He layer. The properties of SN 2005bf resemble those of the explosion of Cassiopeia A. C1 Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. Max Planck Inst Astrophys, D-85748 Garching, Germany. Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34131 Trieste, Italy. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Univ Tokyo, Grad Sch Arts & Sci, Dept Earth Sci & Astron, Meguro Ku, Tokyo 1538902, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Tokyo, Sch Sci, Inst Astron, Tokyo 1810015, Japan. Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. Natl Astron Observ Japan, Opt & Infrared Astron Div, Tokyo 1818588, Japan. Indian Inst Astrophys, Bangalore 560034, Karnataka, India. RP Tominaga, N (reprint author), Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. EM tominaga@astron.s.u-tokyo.ac.jp RI Nomoto, Ken'ichi/A-4393-2011; OI Prabhu, Tushar/0000-0003-0797-5057 NR 36 TC 61 Z9 61 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 NOV 10 PY 2005 VL 633 IS 2 BP L97 EP L100 DI 10.1086/498570 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 983NL UT WOS:000233239200009 ER PT J AU Novikova, I Xiao, Y Phillips, DF Walsworth, RL AF Novikova, I Xiao, Y Phillips, DF Walsworth, RL TI EIT and diffusion of atomic coherence SO JOURNAL OF MODERN OPTICS LA English DT Article; Proceedings Paper CT 35th Winter Colloquium on the Physics of Quantum Electronics CY JAN 02-06, 2005 CL Snowbird, UT ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; BUFFER GAS; RELAXATION; LIGHT AB We study experimentally the effect of diffusion of Rb atoms on electromagnetically induced transparency (EIT) in a buffer gas vapour cell. In particular, we find that diffusion of atomic coherence in and out of the laser beam plays a crucial role in determining the EIT resonance lineshape and the stored light lifetime. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Novikova, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM i.novikova@osa.org RI Novikova, Irina/B-9041-2008 NR 23 TC 29 Z9 30 U1 0 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0950-0340 J9 J MOD OPTIC JI J. Mod. Opt. PD NOV 10 PY 2005 VL 52 IS 16 BP 2381 EP 2390 DI 10.1080/09500340500275637 PG 10 WC Optics SC Optics GA 982OD UT WOS:000233170600023 ER PT J AU Andre, SL Watters, TR Robinson, MS AF Andre, SL Watters, TR Robinson, MS TI The long wavelength topography of Beethoven and Tolstoj basins, Mercury SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MOON; TECTONICS; MISSION; GRAVITY; CRUSTAL AB Topography derived from Mariner 10 stereo images is used to characterize the interior structure of two mercurian basins, Beethoven and Tolstoj. Beethoven and Tolstoj basins are shallow ( similar to 2.5 km and similar to 2 km deep, respectively) and relatively flat-floored. Beethoven basin has an interior topographic rise near the northwest margin. The topography of Beethoven and Tolstoj basins is similar to that of lunar mare-filled basins. Well-developed basin-concentric wrinkle ridges and arcuate graben associated with lunar mascons are absent in both Beethoven and Tolstoj basins. The lack of mascon tectonic features suggests that either 1) the mercurian basins have a relatively thin veneer of fill material, 2) Mercury's elastic lithosphere was too strong for significant lithospheric flexure and subsidence to occur, or 3) the basin fill material has little or no density contrast with the surrounding crust and thus exerts little net load on the mercurian lithosphere. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Northwestern Univ, Ctr Planetary Sci, Evanston, IL 60208 USA. RP Andre, SL (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. EM andres@si.edu NR 27 TC 3 Z9 3 U1 1 U2 2 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 NOV 9 PY 2005 VL 32 IS 21 AR L21202 DI 10.1029/2005GL023627 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 985CP UT WOS:000233354000001 ER PT J AU Davis, CC Anderson, WR Wurdack, KJ AF Davis, CC Anderson, WR Wurdack, KJ TI Gene transfer from a parasitic flowering plant to a fern SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE biogeography; ferns; horizontal gene transfer; Ophioglossaceae; parasitic plants; phylogeography ID CLOSEST LIVING RELATIVES; BOTRYCHIUM-VIRGINIANUM; MITOCHONDRIAL GENES; HORIZONTAL TRANSFER; MAXIMUM-LIKELIHOOD; POPULATION-GROWTH; LAND PLANTS; OPHIOGLOSSACEAE; SPOROPHYTES; LIGHT AB The rattlesnake fern (Botrychium virginianum (L.) Sw.) is obligately mycotrophic and widely distributed across the northern hemisphere. Three mitochondrial gene regions place this species with other ferns in Ophioglossaceae, while two regions place it as a member of the largely parasitic angiosperm order Santalales (sandalwoods and mistletoes). These discordant phylogenetic placements suggest that part of the genome in B. virginianum was acquired by horizontal gene transfer (HGT), perhaps from root-parasitic Loranthaceae. These transgenes are restricted to B. virginianum and occur across the range of the species. Molecular and life-history traits indicate that the transfer preceded the global expansion of B. virginianum, and that the latter may have happened very rapidly. This is the first report of HGT from an angiosperm to a fern, through either direct parasitism or the mediation of interconnecting fungal symbionts. C1 Harvard Univ Hebaria, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. Univ Michigan Herbarium, Ann Arbor, MI 48108 USA. Smithsonian Inst, Dept Bot, Suitland, MD 20746 USA. Smithsonian Inst, Lab Anal Biol, Suitland, MD 20746 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 NR 48 TC 57 Z9 62 U1 1 U2 17 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. Lond. Ser. B-Biol. Sci. PD NOV 7 PY 2005 VL 272 IS 1578 BP 2237 EP 2242 DI 10.1098/rspb.2005.3226 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 976FV UT WOS:000232719200002 PM 16191635 ER PT J AU Castro, JM Manga, M Martin, MC AF Castro, JM Manga, M Martin, MC TI Vesiculation rates of obsidian domes inferred from H2O concentration profiles SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RHYOLITIC GLASSES; SILICIC VOLCANISM; LAVA DOMES; MAGMA; WATER; DIFFUSION; ASCENT; MELTS; MODEL AB Explosivity of rhyolite domes depends on bubble nucleation and growth. To understand these processes, we measure millimeter-scale variations in H2O by synchrotron Fourier transform infrared (FTIR) spectromicroscopy on interlayered obsidian- pumice samples. The H2O contents of all samples are above the 1-atm solubility value (similar to 0.10 wt.%) and decrease systematically towards vesicular zones, indicating that gas bubbles were growing and that degassing of melt to atmospheric pressure was incomplete. H2O profiles are compared with models for water diffusion in order to constrain the temporal scale of vesiculation. Diffusion timescales range from 0.4 to 15 days, and represent the time between bubble nucleation and quenching. We use these results to estimate the duration of volatile exsolution and evaluate the timing of the formation of explosion pits frequently found on the surfaces of obsidian domes, though never witnessed. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20012 USA. Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA. RP Castro, JM (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012, Washington, DC 20012 USA. EM castroj@si.edu RI Manga, Michael/D-3847-2013; OI Manga, Michael/0000-0003-3286-4682 NR 19 TC 24 Z9 24 U1 1 U2 11 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 NOV 5 PY 2005 VL 32 IS 21 AR L21307 DI 10.1029/2005GL024029 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 982LM UT WOS:000233159900005 ER PT J AU Howard, AD Moore, JM Irwin, RP AF Howard, AD Moore, JM Irwin, RP TI An intense terminal epoch of widespread fluvial activity on early Mars: 1. Valley network incision and associated deposits SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID DRAINAGE-BASIN EVOLUTION; MARGARITIFER SINUS; MARTIAN HIGHLANDS; NORTHERN PLAINS; CRATER LAKES; ORIGIN; REGION; WATER; PRECIPITATION; GROUNDWATER AB We present evidence that a final epoch of widespread fluvial erosion and deposition in the cratered highlands during the latest Noachian or early to mid-Hesperian was characterized by integration of flow within drainage networks as long as 4000 km and trunk valley incision of 50 to 350 m into earlier Noachian depositional basins. Locally deltaic sediments were deposited where incised valley systems debouched into basins. Large alluvial fans of sediment deposited from erosion of alcoves in steep crater walls probably formed contemporaneously. The depth of incision below Noachian surfaces correlates strongly with the gradient and the total valley length, suggesting consistent regional hydrology. Estimated discharges from channel dimensions indicate flow rates equivalent to mean annual floods in terrestrial drainage basins of equivalent size. Such high flow rates imply either runoff directly from precipitation or rapid melting of accumulated snow. Development of duricrusts on the Noachian landscape may have contributed to focusing of late-stage erosion within major trunk drainages. This late-stage epoch of intense fluvial activity appears to be fundamentally different than the fluvial environment prevailing during most of the Noachian Period, which was characterized by widespread fluvial erosion of highlands and crater rims, deeply infilling crater floors, and intercrater basins through ephemeral fluvial activity, and development of local rather than regionally integrated drainage networks. C1 Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Howard, AD (reprint author), Univ Virginia, Dept Environm Sci, POB 400123, Charlottesville, VA 22904 USA. EM ah6p@virginia.edu; jeff.moore@nasa.gov; irwinr@si.edu OI Howard, Alan/0000-0002-5423-1600 NR 77 TC 108 Z9 110 U1 2 U2 6 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 NOV 4 PY 2005 VL 110 IS E12 AR E12S14 DI 10.1029/2005JE002459 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 982MO UT WOS:000233162700002 ER PT J AU Shen, ZQ Lo, KY Liang, MC Ho, PTP Zhao, JH AF Shen, ZQ Lo, KY Liang, MC Ho, PTP Zhao, JH TI A size of similar to 1 AU for the radio source Sgr A* at the centre of the Milky Way SO NATURE LA English DT Article ID SUPERMASSIVE BLACK-HOLE; SAGITTARIUS-A; GALACTIC-CENTER; X-RAY; NUCLEI; MILLIMETER; SPECTRUM; MODELS AB Although it is widely accepted that most galaxies have supermassive black holes at their centres(1-3), concrete proof has proved elusive. Sagittarius A* (Sgr A*)(4), an extremely compact radio source at the centre of our Galaxy, is the best candidate for proof(5-7), because it is the closest. Previous very-long-baseline interferometry observations ( at 7 mm wavelength) reported that Sgr A* is similar to 2 astronomical units (AU) in size(8), but this is still larger than the 'shadow' ( a remarkably dim inner region encircled by a bright ring) that should arise from general relativistic effects near the event horizon of the black hole(9). Moreover, the measured size is wavelength dependent(10). Here we report a radio image of Sgr A* at a wavelength of 3.5 mm, demonstrating that its size is similar to 1 AU. When combined with the lower limit on its mass(11), the lower limit on the mass density is 6.5 x 10(21) M-. pc(-3) (where M-. is the solar mass), which provides strong evidence that Sgr A* is a supermassive black hole. The power-law relationship between wavelength and intrinsic size ( size proportional to wavelength(1.09)) explicitly rules out explanations other than those emission models with stratified structure, which predict a smaller emitting region observed at a shorter radio wavelength. C1 Shanghai Astron Observ, Shanghai 200030, Peoples R China. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Shen, ZQ (reprint author), Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. EM zshen@shao.ac.cn NR 29 TC 132 Z9 137 U1 2 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 3 PY 2005 VL 438 IS 7064 BP 62 EP 64 DI 10.1038/nature04205 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979XS UT WOS:000232979000040 PM 16267548 ER PT J AU Cadena, CD Ricklefs, RE Jimenez, I Bermingham, E AF Cadena, CD Ricklefs, RE Jimenez, I Bermingham, E TI Ecology - Is speciation driven by species diversity? SO NATURE LA English DT Editorial Material ID MOLECULAR PHYLOGENIES; AREA RELATIONSHIP; ISLAND; DIVERSIFICATION; AGE C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Missouri Bot Garden, Ctr Conservat & Sustainable Dev, St Louis, MO 63166 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Cadena, CD (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. EM cdc35b@umsl.edu RI Cadena, Carlos Daniel/G-1313-2010 NR 11 TC 29 Z9 32 U1 0 U2 21 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 3 PY 2005 VL 438 IS 7064 BP E1 EP E2 DI 10.1038/nature04308 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979XS UT WOS:000232979000035 PM 16267504 ER PT J AU Zotz, G AF Zotz, G TI Differences in vital demographic rates in three populations of the epiphytic bromeliad, Werauhia sanguinolenta SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY LA English DT Article DE Bromeliaceae; elasticity analysis; growth; mortality; Panama; size dependency ID PHYSIOLOGICAL ECOLOGY; GROWTH; MANAGEMENT; VEGETATION; FOREST; MEXICO; PLANTS; SIZE; RARE AB Since the response to differences in resource availability is most pronounced in smaller individuals of vascular epiphytes such as Werauhia sanguinolenta Cogn. et Marchal (Bromeliaceae), I expected variation in growth and survival of small individuals to play an important role in the dynamics of entire populations. Four annual censuses (2002-2005) of three study populations, which were located across the isthmus of Panama, allowed me to construct stage transition matrices, and to conduct growth analysis and elasticity analysis. Differences between populations were highly consistent through time, but, contrary to expectations, hardly related to the comportment of smaller plants. For example, although average mortality rates were highest at the driest site, close to the Pacific, small plants were not predominantly affected. Similarly, although the highest relative growth rates (RGR) of individuals and the highest population growth rates (lambda) were found in the population with the highest moisture input, which was located close to the Atlantic coast, this was not due to a particularly strong stimulation of RGR in small plants. Elasticity analysis indicated rather small differences in the importance of the three demographic processes growth, survival, and reproduction for population growth in the three populations, but invariably identified the survival of large tanks as the single most important process determining lambda. (c) 2005 Elsevier SAS. All rights reserved. C1 Univ Basel, Inst Bot, CH-4053 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4053 Basel, Switzerland. EM gerhard.zotz@unibas.ch NR 31 TC 15 Z9 15 U1 1 U2 9 PU GAUTHIER-VILLARS/EDITIONS ELSEVIER PI PARIS PA 23 RUE LINOIS, 75015 PARIS, FRANCE SN 1146-609X J9 ACTA OECOL JI Acta Oecol.-Int. J. Ecol. PD NOV-DEC PY 2005 VL 28 IS 3 BP 306 EP 312 DI 10.1016/j.actao.2005.05.009 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 999YF UT WOS:000234427400013 ER PT J AU Skillman, JB Garcia, M Virgo, A Winter, K AF Skillman, JB Garcia, M Virgo, A Winter, K TI Growth irradiance effects on photosynthesis and growth in two co-occurring shade-tolerant neotropical perennials of contrasting photosynthetic pathways SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Bromeliaceae; chlorophyll fluorescence; Crassulacean acid metabolism; growth analysis; Panama; photoinhibition; photosynthetic acclimation; tropical forest ecology ID CRASSULACEAN ACID METABOLISM; AECHMEA-MAGDALENAE; UNDERSTORY PLANTS; CAM PLANTS; FOREST; PHOTOINHIBITION; ACCLIMATION; BROMELIACEAE; PATTERNS; CO2 AB Dieffenbachia longispatha (C3) and Aechmea rnagdalenae (Crassulacean acid metabolism, CAM) are syntopic, neotropical forest perennials in central Panama that are restricted to shaded habitats. This is of particular interest for A. magdalenae because, like other understory CAM bromeliad species, it appears functionally and structurally to be better suited to life in full sun. Growth irradiance (GI) effects on photosynthesis and growth in both species were explored in the context of sun/shade trade-off concepts largely derived from studies of C3 plants. Potted plants were grown outdoors in 1, 55, and 100% full sun for 5 mo under well-watered conditions. While both species grew faster in high compared to low light, maximum relative growth rates (RGR) in full sun were still extremely slow with A. magdalenae showing a RGR approximately half that of D. longispatha. Photosynthetic capacity increased with GI in D. longispatha but not in A. magdalenae. Aechmea magdalenae responded to GI with shifts in the activity of the different CAM phases. Both species were photoinhibited in full sun, but more so in A. magdalenae. Despite possessing many traits considered adaptive in high light, these results suggest that A. magdalenae is unlikely to attain sufficient growth rates to thrive in productive, high-light habitats. C1 Calif State Univ San Bernardino, Dept Biol, San Bernardino, CA 92407 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Skillman, JB (reprint author), Calif State Univ San Bernardino, Dept Biol, San Bernardino, CA 92407 USA. EM skillman@csusb.edu NR 43 TC 14 Z9 19 U1 3 U2 5 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 NOV PY 2005 VL 92 IS 11 BP 1811 EP 1819 DI 10.3732/ajb.92.11.1811 PG 9 WC Plant Sciences SC Plant Sciences GA 979IE UT WOS:000232934800005 PM 21646098 ER PT J AU Sanchez, CR Murray, SZ Isaza, R Papich, MG AF Sanchez, CR Murray, SZ Isaza, R Papich, MG TI Pharmacokinetics of a single dose of enrofloxacin administered orally to captive Asian elephants (Elephas maximus) SO AMERICAN JOURNAL OF VETERINARY RESEARCH LA English DT Article ID LONG-ACTING FORMULATION; LOXODONTA-AFRICANA; METABOLITE CIPROFLOXACIN; SERUM; PHARMACODYNAMICS; HORSES; MODEL; BIOAVAILABILITY; SUSCEPTIBILITY; TISSUES AB Objective-To determine the pharmacokinetics of enrofloxacin after oral administration to captive elephants. Animals-6 clinically normal adult Asian elephants (Elephas maximus). Procedure-Each elephant received a single dose of enrofloxacin (2.5 mg/kg, PO). Three elephants received their complete diet (pellets and grain) within 2 hours after enrofloxacin administration, whereas the other 3 elephants received only hay within 6 hours after enrofloxacin administration. Serum concentrations of enrofloxacin and ciprofloxacin were measured by use of high-performance liquid chromatography. Results-Harmonic mean half-life after oral administration was 18.4 hours for all elephants. Mean +/- SD peak serum concentration of enrofloxacin was 1.31 +/- 0.40 mu g/mL at 5.0 +/- 4.2 hours after administration. Mean area under the curve was 20.72 +/- 4.25 (mu g X h)/mL. Conclusions and Clinical Relevance-Oral administration of enrofloxacin to Asian elephants has a prolonged elimination half-life, compared with the elimination half-life for adult horses. In addition, potentially therapeutic concentrations in elephants were obtained when enrofloxacin was administered orally at a dosage,of 2.5 mg/kg. Analysis of these results suggests that enrofloxacin administered with feed in the manner described in this study could be a potentially useful antimicrobial for use in treatment of captive Asian elephants with infections attributable to organisms, such as Bordetella slop, Escherichia coli, Mycoplasma spp, Pasteurella spp, Haemophilus spp, Salmonella spp, and Staphylococcus spp. C1 Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. Univ Florida, Coll Vet Med, Dept Small Anim Clin Sci, Gainesville, FL 32610 USA. N Carolina State Univ, Coll Vet Med, Dept Mol Biomed Sci, Raleigh, NC 27606 USA. RP Sanchez, CR (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 46 TC 3 Z9 3 U1 0 U2 5 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 USA SN 0002-9645 J9 AM J VET RES JI Am. J. Vet. Res. PD NOV PY 2005 VL 66 IS 11 BP 1948 EP 1953 DI 10.2460/ajvr.2005.66.1948 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA 979IS UT WOS:000232936200016 PM 16334955 ER PT J AU Jones, FA Chen, J Weng, GJ Hubbell, SP AF Jones, FA Chen, J Weng, GJ Hubbell, SP TI A genetic evaluation of seed dispersal in the neotropical tree Jacaranda copaia (Bignoniaceae) SO AMERICAN NATURALIST LA English DT Article DE Barro Colorado Island; directed dispersal; dispersal kernel; maximum likelihood estimation; microsatellite DNA; model selection ID LONG-DISTANCE DISPERSAL; RAIN-FOREST TREE; TROPICAL FOREST; RECRUITMENT LIMITATION; WIND DISPERSAL; DEPENDENT RECRUITMENT; NATURAL-POPULATIONS; DENSITY-DEPENDENCE; EVOLUTION; PATTERNS AB Seed dispersal is a critical but poorly understood life-history stage of plants. Here we use a genetic approach to describe seed dispersal patterns accurately in a natural population of the Neotropical tree species Jacaranda copaia ( Bignoniaceae). We used microsatellite genotypes from maternally derived tissue on the diaspore to identify which individual of all possible adult trees in the population was the true source of a given seed collected after it dispersed. Wind-dispersed seeds were captured in two different years in a large array of seed traps in an 84-ha mapped area of tropical forest on Barro Colorado Island, Panama. We were particularly interested in the proportion of seeds that traveled long distances and whether there was evidence for direct dispersal into gaps, which are required for successful recruitment of this pioneer tree species. Maximum likelihood procedures were used to fit single- and multiple-component dispersal kernels to the distance data. Mixture models, with separate distributions near and far, best fit the observed dispersal distances, albeit with considerable uncertainty in the tail. We discuss the results in light of different mechanisms responsible for separate distributions near the adult source and in the tail of the curve. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Univ Georgia, Dept Stat, Athens, GA 30602 USA. RP Jones, FA (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM jonesf@si.edu; jchen@stat.uga.edu; guojing@uga.edu; shubbell@plantbio.uga.edu RI Jones, Andy/C-3460-2009 NR 74 TC 87 Z9 90 U1 3 U2 22 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 NOV PY 2005 VL 166 IS 5 BP 543 EP 555 DI 10.1086/491661 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 977VX UT WOS:000232832700006 PM 16224720 ER PT J AU Solis, MA Yen, SH Goolsby, JH Wright, T Pemberton, R Winotai, A Chattrukul, U Thagong, A Rimbut, S AF Solis, MA Yen, SH Goolsby, JH Wright, T Pemberton, R Winotai, A Chattrukul, U Thagong, A Rimbut, S TI Siamusotima aranea, a new stem-boring musotimine (Lepidoptera : Crambidae) from Thailand feeding on Lygodium flexuosum (Schizaeaceae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Pyraloidea; Old World climbing fern; pteridophagy; spiders; tenebrionid beetles ID WORLD CLIMBING FERN; MICROPHYLLUM SCHIZAEACEAE; AUSTRALIA; GENUS; ASIA AB Siamusotima aranea Solis & Yen, is a new stem-boring musotimine species from Thailand. It was discovered in the stems of Lygodium flexuosum (L.) Sw. (Schizaeaceae) during exploration for biological control agents of Lygodium microphyllum (Cav.) R. Br., the Old World climbing fern. This is the first report in the Pyraloidea of a stem-boring larva with unique modifications of the anal segment resembling that of tenebrionid beetle immatures and with observations of possible mimicry between the adult moth and spiders. C1 Natl Museum Nat Hist, Smithsonian Inst, SEL, USDA, Washington, DC 20013 USA. Univ London Imperial Coll Sci & Technol, Dept Biol Sci, Ascot SL5 7YP, Berks, England. Natl Sun Yat Sen Univ, Dept Biol Sci, Kaohsiung 804, Taiwan. USDA ARS, Australian Biol Control Lab, Indooroopilly, Qld 4068, Australia. USDA ARS, Invas Plants Res Lab, Miami Beach, FL 33140 USA. Plant Protect Res & Dev Off, Dept Agr, Bangkok, Thailand. Royal Project Fdn, Chiang Mai, Thailand. RP Solis, MA (reprint author), Natl Museum Nat Hist, Smithsonian Inst, SEL, USDA, POB 37012,E-517,MRC 168, Washington, DC 20013 USA. NR 25 TC 1 Z9 1 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 NOV PY 2005 VL 98 IS 6 BP 887 EP 895 DI 10.1603/0013-8746(2005)098[0887:SAANSM]2.0.CO;2 PG 9 WC Entomology SC Entomology GA 983DD UT WOS:000233210400014 ER PT J AU Lehr, MA Kilpatrick, CW Wilkerson, RC Conn, JE AF Lehr, MA Kilpatrick, CW Wilkerson, RC Conn, JE TI Cryptic species in the Anopheles (Nyssorhynchus) albitarsis (Diptera : Culicidae) complex: Incongruence between random amplified polymorphic DNA-polymerase chain reaction identification and analysis of mitochondrial DNA COI gene sequences SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE cryptic species; Anopheles albitarsis s.l.; mtDNA COI gene; RAPD-PCR ID CYTOCHROME-OXIDASE-I; MORPHOLOGICAL CHARACTERS; PHYLOGENETIC INFERENCE; POPULATION-STRUCTURE; ARBITRARY PRIMERS; MALARIA VECTOR; RAPD MARKERS; PCR; BRAZIL; RECONSTRUCTION AB Random amplified polymorphic DNA (RAPD) diagnostic bands are one tool used to differentiate cryptic mosquito species in the Anopheles albitarsis Complex. Monophyly of four species (A. albitarsis Lynch-Arribalzaga, A. albitarsis B, A. deaneorum Rosa-Freitas, and A. marajoara Galvao & Damasceno) currently identified with the RAPD technique was assessed using sequences of the cytochrome oxidase I (COI) mitochondrial DNA (mtDNA) gene. Maximum parsimony, maximum likelihood, and Bayesian analyses support monophyly for A. albitarsis s.s., A. albitarsis B, and A. deaneorum. Anopheles marajoara, as identified by RAPD banding patterns, was either polyphyletic or paraphyletic in all phylogenetic analyses. The phylogenetic pattern and within-species genetic distances observed in A. marajoara suggest the existence of a previously unidentified species (species E) in northern Brazil and Venezuela. Diagnostic RAPD bands were unable to distinguish between A. marajoara and species E, probably because of the low number of correlated bands used to identify species and weaknesses of the RAPD technique, in particular, violations of the untested assumption of homology of comigrating bands. A. marajoara (even without species E) is paraphyletic with respect to A. deaneorum; if A. deaneorum is a separate species from A. marajoara, then A. marajoara may consist of two or more species in Amazonian Brazil. Based on mtDNA COI sequences, there are at least four phylogenetic species within the Albitarsis Complex: A. albitarsis s.s., A. albitarsis B, A. marajoara, and species E; the species status of A. deaneorum is ambiguous. C1 Univ Vermont, Dept Biol, Burlington, VT 05405 USA. Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, Washington, DC 20560 USA. New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Slingerlands, NY 12159 USA. RP Lehr, MA (reprint author), Univ Vermont, Dept Biol, 120A Marsh Life Sci Bldg, Burlington, VT 05405 USA. OI Conn, Jan/0000-0002-5301-7020 FU FIC NIH HHS [K01 TW009995]; NIAID NIH HHS [R01 AI054139] NR 60 TC 37 Z9 37 U1 0 U2 4 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 NOV PY 2005 VL 98 IS 6 BP 908 EP 917 DI 10.1603/0013-8746(2005)098[0908:CSITAN]2.0.CO;2 PG 10 WC Entomology SC Entomology GA 983DD UT WOS:000233210400016 PM 17082822 ER PT J AU Haarsma, DB Winn, JN Falco, EE Kochanek, CS Ammar, P Boersma, C Fogwell, S Muxlow, TWB McLeod, BA Lehar, J AF Haarsma, DB Winn, JN Falco, EE Kochanek, CS Ammar, P Boersma, C Fogwell, S Muxlow, TWB McLeod, BA Lehar, J TI The FIRST-Optical-VLA survey for lensed radio lobes SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (FOV J0743+1553); galaxies : spiral; gravitational lensing; radio continuum : galaxies ID DIGITAL SKY SURVEY; GRAVITATIONAL LENSES; EINSTEIN RING; FUNDAMENTAL PLANE; FIELD GALAXIES; MASS PROFILES; EVOLUTION; CONSTRAINTS; DISCOVERY; QUASAR AB We present results from a survey for gravitationally lensed radio lobes. Lensed lobes are a potentially richer source of information about galaxy mass distributions than lensed point sources, which have been the exclusive focus of other recent surveys. Our approach is to identify radio lobes in the Faint Images of the Radio Sky at Twenty cm ( FIRST) catalog and then search optical catalogs for coincident foreground galaxies, which are candidate lensing galaxies. We then obtain higher resolution images of these targets at both optical and radio wavelengths and obtain optical spectra for the most promising candidates. We present maps of several radio lobes that are nearly coincident with galaxies. We have not found any new and unambiguous cases of gravitational lensing. One radio lobe in particular, FOV J0743+1553, has two hot spots that could be multiple images produced by a z = 0.19 spiral galaxy, but the lensing interpretation is problematic. C1 Calvin Coll, Grand Rapids, MI 49546 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. RP Haarsma, DB (reprint author), Calvin Coll, 1734 Knollcrest Circle SE, Grand Rapids, MI 49546 USA. EM dhaarsma@calvin.edu OI Muxlow, Thomas/0000-0001-5797-8796 NR 55 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2005 VL 130 IS 5 BP 1977 EP 1995 DI 10.1086/466513 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 979XI UT WOS:000232977900002 ER PT J AU Trinidad, MA Curiel, S Migenes, V Patel, N Torrelles, JM Gomez, JF Rodriguez, LF Ho, PTP Canto, J AF Trinidad, MA Curiel, S Migenes, V Patel, N Torrelles, JM Gomez, JF Rodriguez, LF Ho, PTP Canto, J TI Very large array simultaneous 1.3 cm continuum and H2O maser observations toward IRAS 20126+4104 SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : individual (IRAS 20126+4104); ISM : jets and outflows; masers; stars : formation ID (PROTO)STAR IRAS 20126+4104; METHANOL MASERS; DISK; JET; OUTFLOW; SYSTEM; STAR AB We have observed simultaneously the 1.3 cm continuum and H2O maser emission toward the high-mass protostar IRAS 20126+4104 with the Very Large Array (VLA) in its A configuration, providing an angular resolution of similar or equal to 0.'' 1. We have detected an unresolved continuum source [ I20126N(1.3 cm)] nearly coinciding with the strongest peak of the northern double continuum source previously detected at 3.6 cm in the field and suggested to be a radio jet. In addition, we have detected 29 water maser spots, 21 of which are tightly grouped in a cluster of similar or equal to 0.'' 1 size displaced similar or equal to 0.'' 07 (similar or equal to 120 AU) northwest of I20126N(1.3 cm). The relative positions of the masers with respect to I20126N(1.3 cm) have been established with 10 mas of accuracy. The overall spatial distribution and line-of-sight velocity components of the water maser spots associated with I20126N( 1.3 cm) are fully consistent with those previously found by Moscadelli and collaborators through VLBI measurements and interpreted as tracing a conical outflow, with the powering source ( suggested to be traced by a one-sided radio continuum jet) located at the cone vertex. Within this very reasonable scenario, our observations would indicate that the source I20126N( 1.3 cm) is showing the position of the high-mass protostar. Analyzing the spatiokinematic distribution of the VLA water masers, we propose that their motions also show, in addition to proper motions on the order of 100 km s(-1) seen in the plane of the sky, a component of rotation with velocities on the order of 20 km s(-1). The water masers seem then to be both rotating ( as evidenced from their radial velocities) and changing their position in the plane of the sky ( from the proper motions). Within this scenario, some of the water maser spots could be within a rotating circumstellar disk of similar or equal to 170 AU size around a protostar of similar or equal to 20 M-. if it is located at the center of the water maser cluster rather than located at the position of I20126N( 1.3 cm). Then, I20126N( 1.3 cm) would trace one of the two peaks of a two-sided thermal jet, with the high-mass protostar located in between. We think that simultaneous high angular resolution and sensitive multifrequency ( from centimeter to submillimeter wavelengths) observations are the key studies to knowing both the nature of the continuum emission ( one-or two-sided jet?) and the location of the high-mass protostar, which is very relevant for modeling this important object. C1 Univ Guanajuato, Dept Astron, Guanajuato 36240, Mexico. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. INTA, Lab Astrofis Epsacial & Fis Fundamental, E-28080 Madrid, Spain. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Trinidad, MA (reprint author), Univ Guanajuato, Dept Astron, Apartado Postal 144, Guanajuato 36240, Mexico. EM trinidad@astro.ugto.mx RI Migenes, Victor/F-3157-2015; Gomez, Jose Francisco/D-8392-2016; OI Migenes, Victor/0000-0002-7990-2191; Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 19 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2005 VL 130 IS 5 BP 2206 EP 2211 DI 10.1086/452639 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 979XI UT WOS:000232977900018 ER PT J AU Hartman, JD Stanek, KZ Gaudi, BS Holman, MJ McLeod, BA AF Hartman, JD Stanek, KZ Gaudi, BS Holman, MJ McLeod, BA TI Pushing the limits of ground-based photometric precision: Submillimagnitude time-series photometry of the open cluster NGC 6791 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; delta Scuti; stars : variables : other; techniques : photometric ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; IMAGE SUBTRACTION PHOTOMETRY; EXTRASOLAR GIANT PLANET; CCD ENSEMBLE PHOTOMETRY; GALACTIC DISK; VARIABILITY SURVEY; EXTENSIVE SEARCH; VARIABLE-STARS; 2001 CAMPAIGN AB We present the results from a three-night, time-series study of the open cluster NGC 6791 using the Megacam wide-field mosaic CCD camera on the 6.5 m MMT telescope. The aim of this study was to demonstrate the ability to obtain very high precision photometry for a large number of stars. We achieved better than 1% precision for more than 8000 stars with 14.3 < R < 20.1 and submillimagnitude (as low as 0.36 mmag) precision for over 300 stars with 14: 6 < R < 16: 3 in the field of this cluster. We also discovered 10 new variable stars, including a possible delta Scuti variable with an amplitude of 2%, eight likely W UMa contact binaries, and a possible RS CVn star, and we identified seven suspected low-amplitude variables, including one star with an amplitude of 4 mmag. We comment on the implications of this study for a ground-based survey for transiting planets as small as Neptune. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jhartman@cfa.harvard.edu; kstanek@cfa.harvard.edu; sgaudi@cfa.harvard.edu; mholman@cfa.harvard.edu; bmcleod@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012; OI Hartman, Joel/0000-0001-8732-6166 NR 48 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 NOV PY 2005 VL 130 IS 5 BP 2241 EP 2251 DI 10.1086/462405 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 979XI UT WOS:000232977900023 ER PT J AU Barris, BJ Tonry, JL Novicki, MC Wood-Vasey, WM AF Barris, BJ Tonry, JL Novicki, MC Wood-Vasey, WM TI The NN2 flux difference method for constructing variable object light curves SO ASTRONOMICAL JOURNAL LA English DT Article DE methods : data analysis; supernovae : general; techniques : photometric ID HIGH-REDSHIFT SUPERNOVAE; UNIVERSE AB We present a new method for optimally extracting point-source time variability information from a series of images. Differential photometry is generally best accomplished by subtracting two images separated in time, since this removes all constant objects in the field. By removing background sources such as the host galaxies of supernovae, such subtractions make possible the measurement of the proper flux of point-source objects superposed on extended sources. In traditional difference photometry, a single image is designated as the "template'' image and is subtracted from all other observations. This procedure does not take all the available information into account and for suboptimal template images may produce poor results. Given N total observations of an object, we show how to obtain an estimate of the vector of fluxes from the individual images using the antisymmetric matrix of flux differences formed from the N( N - 1)/2 distinct possible subtractions and provide a prescription for estimating the associated uncertainties. We then demonstrate how this method improves results over the standard procedure of designating one image as a template and differencing against only that image. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barris, BJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM barris@ifa.hawaii.edu; jt@ifa.hawaii.edu; mnovicki@ifa.hawaii.edu; wmwood-vasey@cfa.harvard.edu NR 22 TC 18 Z9 18 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2005 VL 130 IS 5 BP 2272 EP 2277 DI 10.1086/491583 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 979XI UT WOS:000232977900026 ER PT J AU Dobrzycki, A Eyer, L Stanek, KZ Macri, LM AF Dobrzycki, A Eyer, L Stanek, KZ Macri, LM TI Discovery of nine quasars behind the Large Magellanic Cloud SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Magellanic Clouds; quasars : general ID GRAVITATIONAL LENSING EXPERIMENT; VARIABILITY-SELECTED QUASARS; X-RAY QUASARS; QSO CANDIDATES; FIELDS; CATALOG; SYSTEM; LMC AB We present the discovery of nine quasars behind the Large Magellanic Cloud, with emission redshifts ranging from 0.07 to 2.09. Six of them were identified as part of the systematic variability-based search for QSOs in the objects from the OGLE-II database. Combination of variability-based selection of candidates with the candidates' colours appears to be a powerful technique for identifying quasars, potentially reaching similar to 50% efficiency. We report an apparent correlation between variability magnitude and variability timescale, which - if confirmed could put even more constraints on QSO candidate selection. The remaining three quasars were identified via followup spectroscopy of optical counterparts to X-ray sources found serendipitously by the Chandra X-ray Observatory satellite. Even though the locations of the candidates were quite uniformly distributed over the LMC bar, the confirmed QSOs all appear near the bar's outskirts. C1 European So Observ, D-85748 Garching, Germany. Observ Geneva, CH-1290 Sauverny, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM adam.dobrzycki@eso.org; laurent.eyer@obs.unige.ch; kstanek@cfa.harvard.edu; lmacri@noao.edu OI Macri, Lucas/0000-0002-1775-4859 NR 20 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2005 VL 442 IS 2 BP 495 EP 500 DI 10.1051/0004-6361:20053494 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971SH UT WOS:000232404400015 ER PT J AU Fuller, GA Williams, SJ Sridharan, TK AF Fuller, GA Williams, SJ Sridharan, TK TI The circumstellar environment of high mass protostellar objects - III. Evidence of infall? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : molecules; ISM : HII regions; radio lines : ISM ID STARLESS CORES; MOLECULAR CLOUDS; DUST CONTINUUM; CS 2-1; MOTIONS; STARS; TURBULENT; REGIONS; SEARCH; LINE AB The results are presented of a molecular line survey to search for the spectral signature of infall towards 77 850 mu m continuum sources believed to be candidate high mass protostellar objects. Up to six different transitions, HCO+ J = 1 --> 0, J = 3 --> 2 and J = 4 --> 3, H2CO 2(12) - 1(11), N2H+ J = 1 --> 0 and (HCO+)-C-13 J = 3 --> 2, were observed towards each source. Towards the peak of the 850 mu m emission, N2H+ was typically strong, with a peak antenna temperature of similar to 1.5 K, with a typical linewidth of similar to 2 km s(-1). The good agreement between the velocity and velocity width of the N2H+ and (HCO+)-C-13 emission suggests that both species are tracing similar material in the sources. With respect to the velocity of the N2H+, there is a statistically significant excess of blue asymmetric line profiles in both the HCO+ J = 1 --> 0 and H2CO transitions. This excess reaches levels similar to that seen towards samples of low mass protostars, and suggests that the material around these high mass sources is infalling. We identify 22 promising candidate infall sources which show at least one blue asymmetric line profile and no red asymmetric profiles. The infall velocity is estimated to be in the range of 0.1 km s(-1) to 1 km s(-1) with an implied mass accretion rate of between 2 x 10(-4) M-./yr and 10(-3) M-./yr. C1 UMIST, Dept Phys, Manchester M60 1QD, Lancs, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fuller, GA (reprint author), UMIST, Dept Phys, POB 88, Manchester M60 1QD, Lancs, England. EM Gary.Fuller@manchester.ac.uk; Stewart.Williams@manchester.ac.uk; tksridha@cfa.harvard.edu NR 39 TC 82 Z9 82 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 NOV PY 2005 VL 442 IS 3 BP 949 EP + DI 10.1051/0004-6361:20042110 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974AC UT WOS:000232562700024 ER PT J AU Petitpas, GR Taylor, CL AF Petitpas, GR Taylor, CL TI A high-resolution mosaic of molecular gas in Stephan's quintet SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (HCG 92; Stephan's Quintet); galaxies : interactions; galaxies : ISM; intergalactic medium ID TIDAL DWARF GALAXIES; SYSTEM; STARBURST; CO; EMISSION AB We present high-resolution (CO)-C-12 J = 1-0 observations of the molecular gas in the Hickson compact group Stephan's Quintet (HCG 92). Our observations consist of multiple pointings and mosaics covering all the regions where CO and star formation have been detected. Within the 10000 field of view centered on the easternmost tidal tail, we detect three clumps of emission that may be partially resolved at our resolution of 800; two of these are new detections not previously seen in ISM studies of this region. Two of these clumps lie in the optical tidal tail, while the third lies to the southeast and is coincident with a large H I feature, but it does not correspond to any features at other wavelengths. We also tentatively detect CO emission from the star-forming regions in the "old tail'' corresponding to recent star formation activity detected in recent UV and H alpha observations. Observations of the rest of the compact group do not show detections, even though strong emission was detected with single-dish telescopes, which suggests that the CO emission originates from a diffuse molecular gas cloud or from at least three separate clumps with separations greater than around 3 kpc. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Calif State Univ Sacramento, Sacramento, CA 95819 USA. RP Harvard Smithsonian Ctr Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA. EM gpetitpas@cfa.harvard.edu; ctaylor@csus.edu NR 30 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2005 VL 633 IS 1 BP 138 EP 147 DI 10.1086/462403 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977VV UT WOS:000232832500012 ER PT J AU Sun, M Jerius, D Jones, C AF Sun, M Jerius, D Jones, C TI A small X-ray corona of the narrow-angle tail radio galaxy NGC 1265 soaring through the perseus cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (Perseus) galaxies : individual (NGC 1265); galaxies : jets; magnetic fields; radio continuum : galaxies; X-rays : galaxies ID MULTIFREQUENCY VLA OBSERVATIONS; ELLIPTIC GALAXIES; MAGNETIC-FIELDS; CHANDRA; EMISSION; GAS; ORIGIN; ACCRETION; ROSAT; JETS AB A deep Chandra observation of NGC1265 (3C 83.1B), the prototype for the narrow-angle tail (NAT) radio galaxy, reveals a small cool X-ray thermal corona (similar to 0.6 keV) embedded in the hot ICM of the Perseus cluster (similar to 6.7 keV). The corona is asymmetric with a sharp edge (similar to 2."2, or 0.8 kpc from the nucleus) to the south and an extension to the north ( at least similar to 800 from the nucleus), which are interpreted as the result of ram pressure, as it cannot be explained solely by the static ICM confinement. We estimate that the corona is moving with a velocity of similar to 2.4 - 4.2 times the local sound speed to the south. The presence of the sharp edge on this small corona indicates that the transport processes are largely suppressed by the magnetic field there. The magnetic field around the corona also suppresses heat conduction by at least a factor of similar to 60 across the corona boundary. We conclude that it is unrealistic to study the interaction between the small X-ray coronae and the hot ICM without considering the roles played by the magnetic field, a factor not included in current simulations. An absorbed (N-H 1.5-3 x 10(22) cm(-2)) nucleus is also detected, which is not usual for FR I radio galaxies. Weak X-ray emission from three inner radio knots in the jets is also detected. Indentations at the east and west of the corona indicate interaction between the jets and the X-ray corona. Narrow jets carry great amounts of energy out of the central AGN and release the energy outside the corona, preserving the tiny and vulnerable corona. This case reveals that the inner kiloparsec core of the corona of massive galaxies can survive both high-speed stripping and powerful AGN feedback. Thus, the cooling of the X-ray coronae potentially provides fuel to the central SMBH in rich environments in which the amount of galactic cold gas is at a minimum. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msun@cfa.harvard.edu NR 34 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2005 VL 633 IS 1 BP 165 EP 173 DI 10.1086/452620 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977VV UT WOS:000232832500015 ER PT J AU Rodriguez-Rico, CA Goss, WM Viallefond, F Zhao, JH Gomez, Y Anantharamaiah, KR AF Rodriguez-Rico, CA Goss, WM Viallefond, F Zhao, JH Gomez, Y Anantharamaiah, KR TI VLA H53 alpha radio recombination line observations of the ultraluminous infrared galaxy Arp 220 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : general; galaxies : individual (Arp 220); galaxies : starburst; radio continuum : galaxies; radio lines : galaxies ID ARP 220; NUCLEUS; CONTINUUM; STARBURST; IC-4553; DISKS AB We present high angular resolution (0."7) observations made with the Very Large Array (VLA) of the radio recombination line (RRL) H53 alpha and radio continuum emission at 43 GHz from the ultraluminous infrared galaxy (ULIRG) Arp 220. The 43 GHz continuum emission shows a compact structure (similar to 2") with two peaks separated by similar to 1", the east (E) and west (W) components, that correspond to each galactic nucleus of the merger. The spectral indices for both the E and W components, using radio continuum images at 8.3 and 43 GHz are typical of synchrotron emission (alpha similar to 1.0). Our 43 GHz continuum and H53 alpha line observations confirm the flux densities predicted by the models proposed by Anantharamaiah et al. (2000). This agreement with the models implies the presence of high-density (similar to 10(5) cm(-3)) compact H II regions (similar to 0.1 pc) in Arp 220. The integrated H53 alpha line emission is stronger toward the nonthermal radio continuum peaks, which are also coincident with the peaks of molecular emission of the H2CO. The coincidence between the integrated H53 alpha and the H2CO maser line emission suggests that the recent star-forming regions, traced by the high-density gas, are located mainly in regions that are close to the two radio continuum peaks. Avelocity gradient of similar to 0.30 km s(-1) pc(-1) in the H53 alpha RRL is observed toward the E component, and a second velocity gradient of similar to 0.15 km s(-1) pc(-1) is detected toward the W component. The orientations of these velocity gradients are in agreement with previous CO, Hi, and OH observations. The kinematics of the high-density ionized gas traced by the H53 alpha line are consistent with two counterrotating disks as suggested by the CO and H I observations. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Natl Radio Astron Observ, Socorro, NM 87801 USA. Observ Paris, LERMA, F-75014 Paris, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Raman Res Inst, Bangalore 560080, Karnataka, India. RP Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Campus Morelia,Apartado Postal 3-72, Morelia 58089, Michoacan, Mexico. EM carlos@astrosmo.unam.mx; mgoss@nrao.edu; fviallef@maat.obspm.fr; jzhao@cfa.harvard.edu; y.gomez@astrosmo.unam.mx RI Anantharamaiah , K. R./E-5369-2012; M, Manjunath/N-4000-2014 OI M, Manjunath/0000-0001-8710-0730 NR 19 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2005 VL 633 IS 1 BP 198 EP 204 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977VV UT WOS:000232832500017 ER PT J AU Patnaude, DJ Fesen, RA AF Patnaude, DJ Fesen, RA TI Model simulations of a shock-cloud interaction in the Cygnus loop SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; ISM : individual (Cygnus Loop); ISM : kinematics and dynamics; shock waves; supernova remnants ID SUPERNOVA REMNANT; HYDRODYNAMIC INTERACTION; INTERSTELLAR CLOUDS; GAS CLOUDS AB We present optical observations and two-dimensional hydrodynamic modeling of an isolated shocked ISM cloud. H alpha images taken in 1992.6 and 2003.7 of a small optical emission cloud along the southwestern limb of the Cygnus Loop were used to measure positional displacements of similar to 0."1 yr(-1) for surrounding Balmer-dominated emission filaments and 0."025-0."055 yr(-1) for internal cloud emission features. These measurements imply transverse velocities of similar or equal to 250 and similar or equal to 80-140 km s(-1) for ambient ISM and internal cloud shocks, respectively. A lack of observed turbulent gas stripping at the cloud-ISM boundary in the H alpha images suggests that there is not an abrupt density change at the cloud-ISM boundary. Also, the complex shock structure visible within the cloud indicates that the cloud's internal density distribution is two-phased-a smoothly varying background density that is populated by higher density clumps. Guided by the H alpha images, we present model results for a shock interacting with a non-uniform ISM cloud. We find that this cloud can be well modeled by a smoothly varying power-law core with a density contrast of similar to 4 times the ambient density, surrounded by a low-density envelope with a Lorentzian profile. The lack of sharp density gradients in such a model inhibits the growth of Kelvin-Helmholtz instabilities, consistent with the cloud's appearance. Our model results also suggest that cloud clumps have densities similar to 10 times the ambient ISM density and account for similar to 30% of the total cloud volume. Moreover, the observed spacing of internal cloud shocks and model simulations indicate that the distance between clumps is similar to 4 clump radii. We conclude that this diffuse ISM cloud is best modeled by a smoothly varying, low-density distribution coupled to higher density, moderately spaced internal clumps. C1 Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Patnaude, DJ (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. NR 21 TC 19 Z9 19 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2005 VL 633 IS 1 BP 240 EP 247 DI 10.1086/452627 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977VV UT WOS:000232832500022 ER PT J AU Altamirano, D van der Klis, M Mendez, M Migliari, S Jonker, PG Tiengo, A Zhang, W AF Altamirano, D van der Klis, M Mendez, M Migliari, S Jonker, PG Tiengo, A Zhang, W TI The island state of the atoll source 4U 1820-30 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (4U 0614+09, 4U 1608-52, 4U 1728-34, 4U 1820-30, SAX J1808.4-3658); stars : neutron; X-rays : stars ID X-RAY BINARIES; CLUSTER NGC 6624; 4U 1820-30; TIMING FEATURES; POWER SPECTRA; LOW-FREQUENCY; DISCOVERY; OSCILLATIONS; VARIABILITY; EXPLORER AB We study the rapid X-ray time variability in all public data available from the Rossi X-Ray Timing Explorer Proportional Counter Array on the atoll source 4U 1820-30 in the low-luminosity island state. A total of similar to 46 ks of data were used. We compare the frequencies of the variability components of 4U 1820-30 with those in other atoll sources. These frequencies were previously found to follow a universal scheme of correlations. We find that 4U 1820-30 shows correlations that are shifted by factors of 1.13 +/- 0: 01 and 1: 21 +/- 0: 02 with respect to those in other atoll sources. These shifts are similar to, but smaller than, the shift factor of similar to 1.45 previously reported for some accreting millisecond pulsars. Therefore, 4U 1820-30 is the first atoll source that shows no significant pulsations but has a significant shift in the frequency correlations compared with the other three nonpulsating atoll sources. C1 Univ Amsterdam, Astron Inst, NL-1098 SJ Amsterdam, Netherlands. Univ Amsterdam, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAF, Ist Astrofis Spaziale & Fis Cosmica, Sez Milano G Occhialini, I-20133 Milan, Italy. Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. RP Univ Amsterdam, Astron Inst, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM diego@science.uva.nl RI Mendez, Mariano/C-8011-2012; OI Mendez, Mariano/0000-0003-2187-2708; Tiengo, Andrea/0000-0002-6038-1090 NR 38 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2005 VL 633 IS 1 BP 358 EP 366 DI 10.1086/447761 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977VV UT WOS:000232832500034 ER PT J AU Randall, SK Matthews, JM Fontaine, G Rowe, J Kuschnig, R Green, EM Brassard, P Chayer, P Guenther, DB Moffat, AFJ Rucinski, S Sasselov, D Walker, GAH Weiss, WW AF Randall, SK Matthews, JM Fontaine, G Rowe, J Kuschnig, R Green, EM Brassard, P Chayer, P Guenther, DB Moffat, AFJ Rucinski, S Sasselov, D Walker, GAH Weiss, WW TI Detection of long-period variations in the subdwarf B star PG 0101+039 on the basis of photometry from the MOST satellite SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : interiors; stars : oscillations; subdwarfs ID GRAVITY-MODE PULSATORS; DRIVING MECHANISM; CLASS PROTOTYPE; WHITE-DWARFS; SDB STARS; PARAMETERS; ASTEROSEISMOLOGY; DISCOVERY; HELIUM AB We report the detection of three discrete pulsation frequencies in the long-period variable subdwarf B star PG 0101 + 039 on the basis of similar to 400 hr of MOST wide-band photometry. The periodicities uncovered lie at 7235, 5227, and 2650 s, respectively, and are associated with amplitudes between 0.03% and 0.06% of the mean brightness, lower than those measured in any other variable of this kind. We also find evidence for luminosity variations consistent with an ellipsoidal deformation of the subdwarf in the rotationally locked short-period binary system predicted from radial velocity measurements and evolutionary models. Our atmospheric modeling of two independent time-averaged optical spectra of PG 0101 + 039 yields T-eff similar or equal to 28,300 K and log g similar or equal to 5.52, making it one of the hottest long-period variable subdwarf B stars known. The fact that we nevertheless detect brightness variations in the data is in conflict with predictions from current models, which place the theoretical blue edge for observable long-period instabilities at a temperature around 4000 K cooler than that of PG 0101 + 039. C1 Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Johns Hopkins Univ, Bloomberg Ctr Phys & Astron, Baltimore, MD 21218 USA. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Univ Montreal, Dept Phys, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM randall@astro.umontreal.ca; matthews@astro.ubc.ca; fontaine@astro.umontreal.ca; rowe@astro.ubc.ca; kuschnig@astro.ubc.ca; bgreen@as.arizona.edu; brassard@astro.umontreal.ca; chayer@pha.jhu.edu; guenther@ap.stmarys.ca; moffat@astro.umontreal.ca; rucinski@astro.utoronto.ca; sasselov@cfa.harvard.edu; walker@astro.ubc.ca; weiss@astro.univie.ac.at NR 25 TC 18 Z9 18 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2005 VL 633 IS 1 BP 460 EP 464 DI 10.1086/452628 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977VV UT WOS:000232832500047 ER PT J AU Murray, SS Kenter, A Forman, WR Jones, C Green, PJ Kochanek, CS Vikhlinin, A Fabricant, D Fazio, G Brand, K Brown, MJI Dey, A Jannuzi, BT Najita, J McNamara, B Shields, J Rieke, M AF Murray, SS Kenter, A Forman, WR Jones, C Green, PJ Kochanek, CS Vikhlinin, A Fabricant, D Fazio, G Brand, K Brown, MJI Dey, A Jannuzi, BT Najita, J McNamara, B Shields, J Rieke, M TI XBootes: An X-ray survey of the NDWFS Bootes field. I. Overview and initial results SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : active; surveys; X-rays : galaxies ID CHANDRA MULTIWAVELENGTH PROJECT; ACTIVE GALACTIC NUCLEI; REDSHIFT SURVEY; SOUTH; EVOLUTION; CATALOGS; 2-POINT; NUMBER; GOODS; SKY AB We obtained a 5 ks deep Chandra X-ray Observatory ACIS-I map of the 9.3 deg(2) Bootes field of the NOAO Deep Wide-Field Survey. Here we describe the data acquisition and analysis strategies leading to a catalog of 4642 ( 3293) point sources with 2 or more ( 4 or more) counts, corresponding to a limiting flux of roughly 4(8) x 10(-15) ergs cm(-2) s(-1) in the 0.5 - 7 keV band. These Chandra XBootes data are unique in that they constitute the widest contiguous X-ray field yet observed to such a faint flux limit. Because of the extraordinarily low background of the ACIS, we expect only 14% (0.7%) of the sources to be spurious. We also detected 43 extended sources in this survey. The distribution of the point sources among the 126 pointings (ACIS-I has a 16' x 16' field of view) is consistent with Poisson fluctuations about the mean of 36.8 sources per pointing. While a smoothed image of the point source distribution is clumpy, there is no statistically significant evidence of large-scale filamentary structure. We do find however, that for theta > 1', the angular correlation function of these sources is consistent with previous measurements, following a power law in angle with slope similar to - 0.7. In a 1.4 deg(2) sample of the survey, approximately 87% of the sources with 4 or more counts have an optical counterpart to R similar to 26 mag. As part of a larger program of optical spectroscopy of the NDWFS Bootes area, spectra have been obtained for similar to 900 of the X-ray sources, most of which are quasars or active galactic nuclei. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Univ Arizona, Steward Observ, Tucson, AZ USA. RP Murray, SS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Forman, William/0000-0002-9478-1682 NR 32 TC 106 Z9 106 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 NOV PY 2005 VL 161 IS 1 BP 1 EP 8 DI 10.1086/444378 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 979XH UT WOS:000232977800001 ER PT J AU Kenter, A Murray, SS Forman, WR Jones, C Green, P Kochanek, CS Vikhlinin, A Fabricant, D Fazio, G Brand, K Brown, MJI Dey, A Jannuzi, BT Najita, J McNamara, B Shields, J Rieke, M AF Kenter, A Murray, SS Forman, WR Jones, C Green, P Kochanek, CS Vikhlinin, A Fabricant, D Fazio, G Brand, K Brown, MJI Dey, A Jannuzi, BT Najita, J McNamara, B Shields, J Rieke, M TI XBootes: An X-ray survey of the NDWFS Bootes field. II. The X-ray source catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies : active; surveys; X-rays : general ID NUMBER; GALAXIES; CLUSTERS; NOISE AB We present results from a Chandra survey of the 9 deg(2) Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). This XBootes survey consists of 126 separate contiguous ACIS-I observations each of approximately 5000 s in duration. These unique Chandra observations allow us to search for large-scale structure and to calculate X-ray source statistics over a wide, contiguous field of view with arcsecond angular resolution and uniform coverage. Optical spectroscopic follow-up observations and the rich NDWFS data set will allow us to identify and classify these X- ray - selected sources. Using wavelet decomposition, we detect 4642 point sources with n >= 2 counts. In order to keep our detections similar to 99% reliable, we limit our list to sources with n >= 4 counts. For a 5000 s observation and assuming a canonical unabsorbed active galactic nucleus (AGN) type X-ray spectrum, a 4 count on-axis source corresponds to a flux of 4.7 x 10(-15) ergs cm(-2) s(-1) in the soft (0.5 - 2 keV) band, 1.5 x 10(-14) ergs cm(-2) s(-1) in the hard (2 - 7 keV) band, and 7.8 x 10(-15) ergs cm(2) s(-1) in the full (0.5 - 7 keV) band. The full 0.5 - 7 keV band n >= 4 count list has 3293 point sources. In addition to the point sources, 43 extended sources have been detected, consistent with the depth of these observations and the number counts of clusters. We present here the X- ray catalog for the XBootes survey, including source positions, X- ray fluxes, hardness ratios, and their uncertainties. We calculate and present the differential number of sources per flux density interval, N(S), for the point sources. In the soft (0.5 - 2 keV) band, N(S) is well fitted by a broken power law with slope of 2.60(-0.12)(+0.11) at bright fluxes and 1.74(-0.22)(+0.28) for faint fluxes. The hard source N(S) is well described by a single power law with an index of -2.93(-0.09)(+0.09). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Univ Arizona, Steward Observ, Tucson, AZ 85751 USA. RP Kenter, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Forman, William/0000-0002-9478-1682 NR 25 TC 89 Z9 89 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 NOV PY 2005 VL 161 IS 1 BP 9 EP 20 DI 10.1086/444379 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 979XH UT WOS:000232977800002 ER PT J AU Lee, JC AF Lee, JC TI Black hole systems seen at high spectral resolution: Inflow and outflow SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE galaxies; active; quasars; general; X-ray; black holes; binary; micro-quasars; individual MCG-6-30-15; IRAS 18325-5926; GRS 1915+105 ID VELOCITY IONIZED OUTFLOW; ABSORPTION-LINES; CHANDRA HETGS; CIRCINUS X-1; SPECTROSCOPY; MCG-6-30-15; NGC-3783; GALAXY; GAS AB High-resolution Chandra and XMM-Newton X-ray spectroscopic studies of stellar and supermassive black holes have revealed that these phenomenologically different systems share many common physical characteristics. The observed outflows in the micro-quasar GRS 1915+105, the Seyfert 1 galaxy MCG-6-30-15 and the Seyfert 2 galaxy IRAS 18325-5926 are the focus of this proceeding. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. EM jclee@cfa.harvard.edu RI Lee, Julia/G-2381-2015 OI Lee, Julia/0000-0002-7336-3588 NR 17 TC 3 Z9 3 U1 1 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 NOV PY 2005 VL 300 IS 1-3 BP 67 EP 70 DI 10.1007/s10509-005-1191-x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987QS UT WOS:000233533000008 ER PT J AU Narayan, R AF Narayan, R TI Low-luminosity accretion in black hole X-ray binaries and active galactic nuclei SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE accretion; accretion disks; active galactic nuclei; black hole physics; radiation mechanisms; X-rays : binaries ID ADVECTION-DOMINATED ACCRETION; NOVA XTE J1118+480; CYGNUS X-1; SPECTRAL STATE; LOW/HARD STATE; SAGITTARIUS-A; RADIO-SOURCES; 2 DIMENSIONS; JET MODEL; GX 339-4 AB At luminosities below a few percent of Eddington, accreting black holes switch to a hard spectral state which is very different from the soft blackbody-like spectral state that is found at higher luminosities. The hard state is well-described by a two-temperature, optically thin, geometrically thick, advection-dominated accretion flow (ADAF) in which the ions are extremely hot ( up to 10(12) K near the black hole), the electrons are also hot (similar to 10(9-10.5) K), and thermal Comptonization dominates the X-ray emission. The radiative efficiency of an ADAF decreases rapidly with decreasing mass accretion rate, becoming extremely low when a source reaches quiescence. ADAFs are expected to have strong outflows, which may explain why relativistic jets are often inferred from the radio emission of these sources. It has been suggested that most of the X-ray emission also comes from a jet, but this is less well established. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM narayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 80 TC 69 Z9 70 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 NOV PY 2005 VL 300 IS 1-3 BP 177 EP 188 DI 10.1007/s10509-005-1178-7 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987QS UT WOS:000233533000021 ER PT J AU Miller, JM AF Miller, JM TI Present evidence for intermediate mass black holes in ULXs and future prospects SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article ID X-RAY SOURCES; CANDIDATE; GALAXIES; EMISSION; OUTBURST; CHANDRA; NUCLEI; RADIO; DISK; X-1 AB In a number of the most luminous ULXs ( those with L-X similar to 10(40) erg s(-1)) in nearby galaxies, observations with XMM-Newton and Chandra are revealing evidence which suggests that these ULXs may harbor intermediate-mass black holes (IMBHs). The detection of accretion disk spectral components with temperatures 5-10 times lower than the temperatures observed in stellar-mass black hole binaries near to their Eddington limit may be particularly compelling evidence for IMBH primaries, since T proportional to M-1/4 for disks around black holes. In some sources, X-ray timing diagnostics also hint at IMBHs. Evidence for IMBHs in a subset of the most luminous ULXs, a discussion of the robustness of this evidence and alternatives to the IMBH interpretation, and prospects for better determining the nature of these sources in the future, are presented in this work. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jmmiller@cfa.harvard.edu NR 34 TC 11 Z9 11 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 NOV PY 2005 VL 300 IS 1-3 BP 227 EP 238 DI 10.1007/s10509-005-1181-z PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987QS UT WOS:000233533000026 ER PT J AU Kaiser, CA Sokoloski, JL Gunn, KF Brocksopp, C AF Kaiser, CA Sokoloski, JL Gunn, KF Brocksopp, C TI Is GRS 1915+105 a microquasar? SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article ID EXTRAGALACTIC RADIO-SOURCES; GRS 1915+105; SCALE STRUCTURE; CYGNUS-A; X-RAY; JETS; EJECTIONS AB The large mechanical luminosity of the jets of GRS 1915+105 should give rise to luminous emission regions, similar to those observed in radio galaxies, where the jets interact with the gas surrounding the source. However, no radio synchrotron emission of the expected morphology has been found. Here we present the results of a study suggesting that radio bremsstrahlung from the compressed and heated ISM in front of the jets should be detectable, while the synchrotron lobes may be too faint. We identify these jet impact sites with two well-known IRAS regions. This identification suggests a distance of GRS 1915+105 of 6.5 +/- 1.6 kpc, significantly closer than the usually assumed distance of 11-12 kpc. We discuss the implications of this reduced distance estimate. The non-detection of the synchrotron radio lobes implies a significant fraction of non-radiating particles, possibly protons, in the jets. The apparent motion of small-scale jet components is not superluminal, so if superluminal motion is required for an object to be termed a microquasar, GRS 1915+105 actually does not qualify. The mass of the black hole in the system is increased to 21 +/- 9 M circle dot, while the mechanical luminosity of the jets is reduced to 14% of the Eddington luminosity. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Kaiser, CA (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM c.r.kaiser@soton.ac.uk NR 23 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD NOV PY 2005 VL 300 IS 1-3 BP 283 EP 288 DI 10.1007/s10509-005-1196-5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987QS UT WOS:000233533000032 ER PT J AU Korine, C Kalko, EKV AF Korine, C Kalko, EKV TI Fruit detection and discrimination by small fruit-eating bats (Phyllostomidae): echolocation call design and olfaction SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Artibeus; Vampyressa ficus; foraging; sensory cues ID CAROLLIA-PERSPICILLATA; PREY CAPTURE; ORIENTATION; SENSITIVITY; CHIROPTERA; CLUTTER; VISION; PIPER AB We studied the role of echolocation and other sensory cues in two small frugivorous New World leaf-nosed bats (Phyllostomidae: Artibeus watsoni and Vampyressa pusilla) feeding on different types of fig fruit. To test which cues the bats need to find these fruit, we conducted behavioral experiments in a flight cage with ripe and similar-sized figs where we selectively excluded vision, olfaction, and echolocation cues from the bats. In another series of experiments, we tested the discrimination abilities of the bats and presented sets of fruits that differed in ripeness (ripe, unripe), size (small, large), and quality (intact/infested with caterpillars). We monitored the bats' foraging and echolocation behavior simultaneously. In flight, both bat species continuously emitted short (< 2 ms), multi-harmonic, and steep frequency-modulated (FM) calls of high frequencies, large bandwidth, and very low amplitude. Foraging behavior of bats was composed of two distinct stages: search or orienting flight followed by approach behavior consisting of exploration flights, multiple approaches of a selected fruit, and final acquisition of ripe figs in flight or in a brief landing. Both bat species continuously emitted echolocation calls. Structure and pattern of signals changed predictably when the bats switched from search or orienting calls to approach calls. We did not record a terminal phase before final acquisition of a fruit, as it is typical for aerial insectivorous bats prior to capture. Both bat species selected ripe over unripe fruit and non-infested over infested fruit. Artibeus watsoni preferred larger over smaller fruit. We conclude from our experiments, that the bats used a combination of odor-guided detection together with echolocation for localization in order to find ripe fruit and to discriminate among them. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Ulm, Dept Expt Ecol Bio 3, D-89069 Ulm, Germany. RP Korine, C (reprint author), Ben Gurion Univ Negev, Jacob Blaustein Inst Desert Res, Mitrani Dept Desert Ecol, IL-84990 Sede Boqer, Israel. RI Korine, Carmi/F-4116-2012 NR 44 TC 59 Z9 63 U1 2 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD NOV PY 2005 VL 59 IS 1 BP 12 EP 23 DI 10.1007/s00265-005-0003-1 PG 12 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 983OS UT WOS:000233242600003 ER PT J AU Eltz, T Roubik, D Lunau, K AF Eltz, T Roubik, D Lunau, K TI Experience-dependent choices ensure species-specific fragrance accumulation in male orchid bees SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article ID MALE EUGLOSSINE BEES; LONG-TERM HABITUATION; FLORAL FRAGRANCES; WITHDRAWAL REFLEX; MATING-BEHAVIOR; APIS-MELLIFERA; HYMENOPTERA; APIDAE; EVOLUTION; POLLINATORS AB Male neotropical orchid bees (Euglossini) collect volatile chemicals from orchid flowers and other sources and store them in hind leg cavities. The accumulated fragrance bouquets are later emitted at mating sites. Although most other insects synthesize pheromone blends de novo, specific euglossine perfumes are derived from active choices in a changing fragrance market. Male bees of three species of Euglossa possessed distinctive fragrance phenotypes showing little variation by locality and habitat in mainland Central America. In cage experiments, fragrance choice by male Euglossa imperialis was influenced markedly by a bee's collection history. Collection of a given chemical strongly reduced its attractiveness on subsequent occasions, an effect that was retained over days. Experimentally adding the chemicals directly to bee hind legs produced no effect. We conclude that bees learn and remember chemicals they collect. Innate odor preferences, memory and the avoidance of overcollecting by negative feedback may be the primary mechanisms that ensure unique blends of pheromone analogs in these tropical forest bees. C1 Univ Dusseldorf, Dept Neurobiol, Sensory Ecol Grp, D-40225 Dusseldorf, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Eltz, T (reprint author), Univ Dusseldorf, Dept Neurobiol, Sensory Ecol Grp, Univ Str 1, D-40225 Dusseldorf, Germany. EM eltz@uni-duesseldorf.de NR 60 TC 40 Z9 40 U1 2 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD NOV PY 2005 VL 59 IS 1 BP 149 EP 156 DI 10.1007/s00265-005-0021-z PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 983OS UT WOS:000233242600020 ER PT J AU Kite, GC Hoffmann, P Lees, DC Wurdack, KJ Gillespie, LJ AF Kite, GC Hoffmann, P Lees, DC Wurdack, KJ Gillespie, LJ TI alpha-Homonojirimycin and other polyhydroxyalkaloids in Suregada Roxb. ex Rottl. (Euphorbiaceae) SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article DE Suregada; Euphorbiaceae; polyhydroxyalkaloids; alpha-homonojirimycin ID GENERA C1 Royal Bot Gardens, Richmond TW9 2AB, Surrey, England. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Smithsonian Inst, Lab Analyt Biol, Washington, DC 20013 USA. Canadian Museum Nat, Ottawa, ON K1P 6P4, Canada. RP Kite, GC (reprint author), Royal Bot Gardens, Richmond TW9 2AB, Surrey, England. EM g.kite@kew.org NR 16 TC 4 Z9 4 U1 2 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD NOV PY 2005 VL 33 IS 11 BP 1183 EP 1186 DI 10.1016/j.bse.2005.06.001 PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 983EU UT WOS:000233214800009 ER PT J AU Torchin, ME Byers, JE Huspeni, TC AF Torchin, ME Byers, JE Huspeni, TC TI Differential parasitism of native and introduced snails: Replacement of a parasite fauna SO BIOLOGICAL INVASIONS LA English DT Article DE Batillaria attramentaria; Batillaria cumingi; Cerithidea californica; fish parasites; invasion ecology; local extinctions; non-indigenous species; trematodes ID CERITHIDEA-CALIFORNICA; MEDIATED COMPETITION; NORTH-AMERICA; LIFE-CYCLE; HOST; ECHINOSTOMATIDAE; COEXISTENCE; ESTUARINE; TREMATODA; SUSCEPTIBILITY AB The role of parasites in a marine invasion was assessed by first examining regional patterns of trematode parasitism in the introduced Japanese mud snail, Batillaria cumingi (= B. attramentaria), in nearly all of its introduced range along the Pacific Coast of North America. Only one parasite species, which was itself a non-native species, Cercaria batillariae was recovered. Its prevalence ranged from 3 to 86%. Trematode diversity and prevalence in B. cumingi and a native sympatric mud snail, Cerithidea californica, were also compared in Bolinas Lagoon, California. Prevalence of larval trematodes infecting snails as first intermediate hosts was not significantly different (14% in B. cumingi vs 15% in C. californica). However, while the non-native snail was parasitized only by one introduced trematode species, the native snail was parasitized by 10 native trematode species. Furthermore, only the native, C. californica, was infected as a second intermediate host, by Acanthoparyphium spinulosum(78% prevalence). Given the high host specificity of trematodes for first intermediate hosts, in marshes where B. cumingi is competitively excluding C. californica, 10 or more native trematodes will also become locally extinct. C1 Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP Torchin, ME (reprint author), Smithsonian Trop Res Inst, Apartado Postal 2072, Balboa, Ancon, Panama. EM torchinm@si.edu NR 62 TC 49 Z9 53 U1 1 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD NOV PY 2005 VL 7 IS 6 BP 885 EP 894 DI 10.1007/s10530-004-2967-6 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 980RI UT WOS:000233035500001 ER PT J AU Olson, SL AF Olson, SL TI Correction of erroneous records of Cormorants from archeological sites in Alaska SO CONDOR LA English DT Article DE Alaska; Amchitka; cormorant; Kodiak; Phalacrocorax; zooarcheology AB In previous studies, bones from archeological midden deposits on Kodiak and Amchitka Islands, Aleutians, were erroneously identified as belonging to Great Cormorant (Phalacrocorax carbo), Pallas's Cormorant (P. perspicillatus), and Japanese Cormorant (P. capillatus), none of which is otherwise known from Alaska. These specimens are all re-identified as having come from the Double-crested Cormorant (P. auritus), which is much larger in Alaska than in middle and southern latitudes in North America. C1 Natl Museum Nat Hist, Div Birds, Smithsonian Inst, Washington, DC 20560 USA. RP Olson, SL (reprint author), Natl Museum Nat Hist, Div Birds, Smithsonian Inst, Washington, DC 20560 USA. EM olsons@si.edu NR 12 TC 0 Z9 0 U1 0 U2 1 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 NOV PY 2005 VL 107 IS 4 BP 930 EP 933 DI 10.1650/7818.1 PG 4 WC Ornithology SC Zoology GA 985PQ UT WOS:000233390700020 ER PT J AU Carrasco-Nunez, G Righter, K Chesley, J Siebert, L Aranda-Gomez, J AF Carrasco-Nunez, G Righter, K Chesley, J Siebert, L Aranda-Gomez, J TI Contemporaneous eruption of calc-alkaline and alkaline lavas in a continental arc (Eastern Mexican Volcanic Belt): chemically heterogeneous but isotopically homogeneous source SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Article DE Mexican Volcanic Belt; assimilation and fractional crystallization; hawaiite; calc-alkaline lavas; degree of melting; mantle source ID SUBDUCTION ZONE MAGMATISM; TRACE-ELEMENT; BASALTIC ANDESITES; WESTERN MEXICO; PB-ISOTOPE; COMPOSITIONAL DIVERSITY; QUATERNARY VOLCANISM; MANTLE METASOMATISM; WASHINGTON CASCADES; SOUTHERN WASHINGTON AB Nearly contemporaneous eruption of alkaline and calc-alkaline lavas occurred about 900 years BP from El Volcancillo paired vent, located behind the volcanic front in the Mexican Volcanic Belt (MVB). Emission of hawaiite (Toxtlacuaya) was immediately followed by calc-alkaline basalt (Rio Naolinco). Hawaiites contain olivine microphenocrysts (Fo(67-72)), plagioclase (An(56-60)) phenocrysts, have 4-5 wt% MgO and 49.6-50.9 wt% SiO(2). In contrast, calc-alkaline lavas contain plagioclase (An(64-72)) and olivine phenocrysts (Fo(81-84)) with spinel inclusions, and have 8-9 wt% MgO and 48.4-49.4 wt% SiO(2). The most primitive lavas in the region (Rio Naolinco and Cerro Colorado) are not as primitive as parental melts in other arcs, and could represent either (a) variable degrees of melting of a subduction modified, garnet-bearing depleted mantle source, followed by AFC process, or (b) melting of two distinct mantle sources followed by AFC processes. These two hypotheses are evaluated using REE, HFSE, and Sr, Os and Pb isotopic data. The Toxtlacuaya flow and the Y & I lavas can be generated by combined fractional crystallization and assimilation of gabbroic granulite, starting with a parental liquid similar to the Cerro Colorado basalt. Although calc-alkaline and alkaline magmas commonly occur together in other areas of the MVB, evidence for subduction component in El Volcancillo magmas is minimal and limited to < 1%, which is a unique feature in this region further from the trench. El Volcancillo lavas were produced from two different magma batches: we surmise that the injection of calc-alkaline magma into an alkaline magma chamber triggered the eruption of hawaiites. Our results suggest that the subalkaline and hawaiitic lavas were formed by different degrees of partial melting of a similar, largely depleted mantle source, followed by later AFC processes. This model is unusual for arcs, where such diversity is usually explained by melting of heterogeneous (enriched and depleted) and subduction-modified mantle. C1 Univ Nacl Autonoma Mexico, Ctr Geociencias, Queretaro 76230, Mexico. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. Smithsonian Inst, Global Volcanism Program, Washington, DC 20013 USA. RP Carrasco-Nunez, G (reprint author), Univ Nacl Autonoma Mexico, Ctr Geociencias, Campus Juriquilla, Queretaro 76230, Mexico. EM gerardoc@geociencias.unam.mx NR 69 TC 17 Z9 17 U1 0 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0010-7999 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD NOV PY 2005 VL 150 IS 4 BP 423 EP 440 DI 10.1007/s00410-005-0015-x PG 18 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 977HC UT WOS:000232793000004 ER PT J AU Fukami, H Knowlton, N AF Fukami, H Knowlton, N TI Analysis of complete mitochondrial DNA sequences of three members of the Montastraea annularis coral species complex (Cnidaria, Anthozoa, Scleractinia) SO CORAL REEFS LA English DT Article DE Montastraea; species complex; coral; mitochondrion; Cnidaria ID METRIDIUM-SENILE CNIDARIA; STANDARD GENETIC-CODE; REEF BUILDING CORAL; SEA-ANEMONE; PHYLOGENETIC-RELATIONSHIPS; REPRODUCTIVE ISOLATION; PHYLUM CNIDARIA; RIBOSOMAL-RNA; EVOLUTION; GENOME AB Complete mitochondrial nucleotide sequences of two individuals each of Montastraea annularis, Montastraea faveolata, and Montastraea franksi were determined. Gene composition and order differed substantially from the sea anemone Metridium senile, but were identical to that of the phylogenetically distant coral genus Acropora. However, characteristics of the non-coding regions differed between the two scleractinian genera. Among members of the M. annularis complex, only 25 of 16,134 base pair positions were variable. Sixteen of these occurred in one colony of M. franksi, which (together with additional data) indicates the existence of multiple divergent mitochondrial lineages in this species. Overall, rates of evolution for these mitochondrial genomes were extremely slow (0.03-0.04% per million years based on the fossil record of the M. annularis complex). At higher taxonomic levels, patterns of genetic divergence and synonymous/nonsynonymous substitutions suggest non-neutral and unequal rates of evolution between the two lineages to which Montastraea and Acropora belong. C1 Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Knowlton, N (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. EM nknowlton@ucsd.edu NR 34 TC 49 Z9 52 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD NOV PY 2005 VL 24 IS 3 BP 410 EP 417 DI 10.1007/s00338-005-0023-3 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 992VX UT WOS:000233913200011 ER PT J AU Santiago-Blay, JA Anderson, SR Buckley, RT AF Santiago-Blay, JA Anderson, SR Buckley, RT TI Possible implications of two new angiosperm flowers from Burmese amber (Lower Cretaceous) for well-established-and diversified insect-plant associations SO ENTOMOLOGICAL NEWS LA English DT Article DE Lower Cretaceous; fossil; Burmese amber; insect-plant associations; angiosperms; pseudopolycentropodidae ID NORTH-AMERICA; SP-NOV; OLD AB Two undescribed flowers in Burmese amber, and additional evidence herein discussed, support the inference that substantially diverse forests, possibly with well-established and diversified insect-plant associations, were already established and preserved by 100 Ma. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Smithsonian Inst, Museo Nacl Hist Nat, Dept Entomol, Washington, DC 20013 USA. Tetra Tech NUS Inc, Pittsburgh, PA 15220 USA. RP Santiago-Blay, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121,POB 37012, Washington, DC 20013 USA. EM blayj@si.edu; AndersonS@ttnus.com; ronbuckley@fuse.net NR 39 TC 5 Z9 8 U1 1 U2 3 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0013-872X J9 ENTOMOL NEWS JI Entomol. News PD NOV-DEC PY 2005 VL 116 IS 5 BP 341 EP 346 PG 6 WC Entomology SC Entomology GA 015NI UT WOS:000235557700009 ER PT J AU Zigler, KS McCartney, MA Levitan, DR Lessios, HA AF Zigler, KS McCartney, MA Levitan, DR Lessios, HA TI Sea urchin bindin divergence predicts gamete compatibility SO EVOLUTION LA English DT Article DE bindin; gamete compatibility; reproductive isolation; sea urchin; speciation ID GENUS ECHINOMETRA; SEXUAL ISOLATION; REPRODUCTIVE ISOLATION; ADAPTIVE EVOLUTION; MITOCHONDRIAL-DNA; RAPID EVOLUTION; PROTEIN BINDIN; SPERM BINDIN; SPECIATION; DROSOPHILA AB Studies on the evolution of reproductive proteins have shown that they tend to evolve more rapidly than other proteins, frequently under positive selection. Progress on understanding the implications of these patterns is possible for marine invertebrates, where molecular evolution can be linked to gamete compatibility. In this study, we surveyed data from the literature from five genera of sea urchins for which there was information on gamete compatibility, divergence of the sperm-egg recognition protein bindin, and mitochondrial divergence. We draw three conclusions: (1) bindin divergence at nonsynonymous sites predicts gamete compatibility, whereas (2) bindin divergence at synonymous sites and mitochondrial DNA divergence do not, and (3) as few as 10 amino acid changes in bindin can lead to complete gamete incompatibility between species. Using mitochondrial divergence as a proxy for time, we find that complete gamete incompatibility can evolve in approximately one and a half million years, whereas sister species can maintain complete gamete compatibility for as long as five million years. C1 Smithsonian Trop Res Inst, Balboa, Panama. Friday Harbor Labs, Friday Harbor, WA 98250 USA. Univ N Carolina, Dept Biol Sci, Wilmington, NC 28403 USA. Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. RP Zigler, KS (reprint author), Univ South, Dept Biol, 735 Univ Rd, Sewanee, TN 37383 USA. EM kzigler@sewanee.edu; mccartneym@uncw.edu; levitan@bio.fsu.edu; lessiosh@si.edu NR 48 TC 54 Z9 56 U1 2 U2 14 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD NOV PY 2005 VL 59 IS 11 BP 2399 EP 2404 PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 990UP UT WOS:000233769000011 PM 16396180 ER PT J AU Baron-Szabo, RC AF Baron-Szabo, RC TI Geographic and stratigraphic distributions of the Caribbean species of Cladocora (Scleractinia, Faviidae) SO FACIES LA English DT Article DE Scleractinia; Cladocora; cretaceous; cenozoic; Caribbean; paleobiogeography ID CORALS AB A complete account of the faviid genus Clado-cora within the Caribbean is presented. In the Caribbean this genus represents an extant group that had its earliest occurrence during the Campanian-Maastrichtian of Jamaica. Recent forms have been reported throughout the Caribbean. The following forms were found (with stratigraphic ranges in the Caribbean): C. arbus-cula (Pliocene-Recent), C. debilis (Pleistocene-Recent), C. gracilis (Middle-Upper Maastrichtian), C. jamaicaensis (Campanian-Maastrichtian and Eocene), C. johnsoni (Pliocene), and C. recrescens (Middle-Upper Oligocene). The occurrence of the genus Cladocora in the Caribbean is largely continuous from the Campanian to Recent, during the majority of the Caribbean species show affinities to European assemblages. For the time intervals Paleocene, Lower Oligocene, and Miocene the taxon has not been reported from the Caribbean. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Baron-Szabo, RC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,W-329,MRC 163, Washington, DC 20013 USA. EM RoseBaron@web.de NR 70 TC 1 Z9 1 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0172-9179 J9 FACIES JI Facies PD NOV PY 2005 VL 51 IS 1-4 BP 185 EP 196 DI 10.1007/s10347-005-0004-6 PG 12 WC Geology; Paleontology SC Geology; Paleontology GA 007XQ UT WOS:000235005200018 ER PT J AU Pelican, KM Brown, JL Wildt, DE Ottinger, MA Howard, JG AF Pelican, KM Brown, JL Wildt, DE Ottinger, MA Howard, JG TI Short term suppression of follicular recruitment and spontaneous ovulation in the cat using levonorgestrel versus a GnRH antagonist SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE cat; GnRH antagonist; levonorgestrel; antide; fecal steroid; estrous cycle ID GONADOTROPIN-RELEASING-HORMONE; LAPAROSCOPIC ARTIFICIAL-INSEMINATION; CONTROLLED OVARIAN HYPERSTIMULATION; LEOPARD NEOFELIS-NEBULOSA; EXOGENOUS GONADOTROPINS; LUTEINIZING-HORMONE; DOMESTIC CAT; SEXUAL-BEHAVIOR; CHORIONIC-GONADOTROPIN; CLOUDED LEOPARD AB Suppression and subsequent rebound of ovarian activity using a progestin (levonorgestrel; Norplant) versus a GnRH antagonist (antide) was assessed in the domestic cat via fecal estradiol and progesterone metabolite analyses. Following an initial dose-response trial, queens were assigned to one of four treatments: (1) antide, two 6 mg/kg injections 15 days apart (n = 8 cats); (2) levonorgestrel, six silastic rods (36 mg levonorgestrel/rod) implanted for 30 days (n = 8); (3) control injections (n = 5); and (4) control implants (n = 5). Steroid metabolites were quantified from daily fecal samples for 90 days before, 30 days during, and 90 days after treatment. Antide and levonorgestrel inhibited estrous cyclicity in contrast to continued cyclicity in controls. Cats already at estradiol baseline in antide (n = 7) and levonorgestrel (n = 4) groups remained inhibited during treatment. In females with elevated estradiol levels at treatment onset (Day 0), a normal estradiol surge was completed before concentrations declined to baseline (similar to Days 5-7) and remained suppressed throughout the remaining treatment period. Additionally, 56% of treatment animals exhibited at least one spontaneous ovulation during the pre-treatment period, but no female ovulated during treatment with levonorgestrel or antide. Antide-treated cats exhibited lower (P < 0.05) baseline estradiol concentrations during treatment compared to pre- and post-treatment. In contrast, levonorgestrel induced elevations in baseline estradiol following treatment compared to pre- and during treatment intervals. Control females showed no change (P > 0.05) in baseline estradiol throughout the study period. All levonorgestrel and antide cats returned to estrus after treatment withdrawal. Results demonstrate that: (1) both antide and levonorgestrel are effective for inducing short-term suppression of follicular recruitment and ovulation in the cat; (2) inhibition is reversible; and (3) GnRH antagonists and progestins differentially regulate basal estradiol secretion. This study also confirmed a relatively high incidence of spontaneous ovulation in the cat, a species generally considered to be an induced ovulator. Published by Elsevier Inc. C1 Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. RP Pelican, KM (reprint author), Conservat & Res Ctr, Dept Reprod Sci, Smithsonians Natl Zool Pk, Front Royal, VA 22630 USA. EM kpelican@si.edu FU NCRR NIH HHS [1 K01 01 RR17310-01] NR 85 TC 33 Z9 34 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 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD NOV PY 2005 VL 144 IS 2 BP 110 EP 121 DI 10.1016/j.ygcen.2005.04.014 PG 12 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 975PT UT WOS:000232675100002 PM 15979618 ER PT J AU Benedix, GK Lauretta, DS McCoy, TJ AF Benedix, GK Lauretta, DS McCoy, TJ TI Thermodynamic constraints on the formation conditions of winonaites and silicate-bearing IAB irons SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID CHONDRITIC METEORITES; PETROLOGY; COMPLEX; CLASSIFICATION; SEGREGATION; EQUILIBRIA; MINERALOGY; INCLUSIONS; IIICD AB Silicate inclusions in IAB irons and related winonaite meteorites have textures, mineralogies and mineral chemistries that indicate a complex formation history of heating, followed by brecciation and metamorphism. Using olivine-orthopyroxene-chromite assemblages in five IAB iron silicate inclusions (Caddo County, Campo del Cielo, Copiapo, Lueders, and Udei Station) and one winonaite (Winona), we calculated closure temperatures and oxygen fugacities for these meteorites. Calculated olivine-chromite Fe-Mg exchange temperatures are compared to two-pyroxene temperatures. Olivine-chromite closure temperatures range from similar to 590 degrees C to similar to 700 degrees C, while two-pyroxene temperatures range from similar to 900 degrees C to similar to 1200 degrees C. Oxygen fugacities of these meteorites, determined for the first time in this study, range from 2.3 to 3.2 log units below the Fe-FeO buffer and define a line between the Fe-FeO and Cr-Cr2O3 buffers. Highly variable temperatures were experienced by these rocks on the hand sample, and sometimes even the thin section, scale consistent with the idea that the winonaite-IAB iron parent body experienced collisional fragmentation and reassembly after peak temperatures were reached. Although modest reduction likely occurred during cooling, the oxygen fugacities and mineral compositions recorded at peak metamorphic temperatures suggest that the chondritic precursor for this parent body was initially more reduced than ordinary chondrites. Copyright (c) 2005 Elsevier Ltd C1 Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Benedix, GK (reprint author), Nat Hist Museum, Dept Mineral, Cromwell Rd, London SW7 5BD, England. EM gbenedix@levee.wustl.edu OI Benedix, Gretchen/0000-0003-0990-8878 NR 27 TC 32 Z9 32 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2005 VL 69 IS 21 BP 5123 EP 5131 DI 10.1016/j.gca.2005.03.048 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 991WW UT WOS:000233846300015 ER PT J AU Lapointe, BE Barile, PJ Littler, MM Littler, DS Bedford, BJ Gasque, C AF Lapointe, BE Barile, PJ Littler, MM Littler, DS Bedford, BJ Gasque, C TI Macroalgal blooms on southeast Florida coral reefs I. Nutrient stoichiometry of the invasive green alga Codium isthmocladum in the wider Caribbean indicates nutrient enrichment SO HARMFUL ALGAE LA English DT Article DE nitrogen; phosphorus; macroalgae; coral reefs; eutrophication ID GREAT-BARRIER-REEF; TOMENTOSOIDES CHLOROPHYTA; SPECIES COMPOSITION; COMMUNITY STRUCTURE; COASTAL ECOSYSTEMS; INORGANIC NITROGEN; FUCUS-VESICULOSUS; LIMITED GROWTH; PHASE-SHIFTS; GLOVERS REEF AB Invasive blooms of the siphonaceous green algae Codium spp. have been considered a symptom of coastal eutrophication but, to date, only limited biochemical evidence supports a linkage to land-based nutrient pollution. Beginning in the summer of 1990, spectacular blooms of unattached Codium isthmocladum developed on deep coral reef habitats in southern Palm Beach County and northern Broward County, and in subsequent years, attached populations formed on reefs in northern Palm Beach County. To better understand the nutrition of these HABs, we collected C. isthmocladum and other reef macroalgae from various locations in southeast Florida as well as the wider Caribbean region for tissue C:N:P analysis in order to gauge variability in the type and degree of N- and/or P-limited growth. Widespread nutrient enrichment in floridian C. isthmocladum populations was evidenced by significantly higher tissue P (0.06% versus 0.04% of dry weight) and lower C:N (12 versus 19), C:P (425 versus 980), and N:P (35 versus 50) ratios compared to more nutrient-depleted Caribbean populations. To determine nutrient availability on southeast Florida's reefs, we sampled near-bottom waters at a variety of locations for DIN (=NH4+ + NO3- + NO2-) and SRP analysis. In general, concentrations of NH4+, NO3- and SRP were all high on southeast Florida's reefs compared to values reported for Caribbean coral reefs. Although summertime upwelling provides episodic NO3- and SRP enrichment to reefs in southeast Florida, these transient nutrient pulses have not historically supported C. isthmocladum blooms. We suggest that the widespread P enrichment of C. isthinocladum tissue and water column DIN:SRP ratios < 16:1 in southeast Florida drive this system toward N limitation where low level NH4+ enrichment becomes of paramount importance. Hence, the recent C isthmocladum blooms appear to be supported by increasing land-based nutrient pollution, particularly, sewage that is enriched in NH4+ and SRP at a low N:P ratio (< 10:1) critical to sustaining balanced growth during bloom formation. (c) 2005 Published by Elsevier B.V. C1 Harbor Branch Oceanog Inst Inc, Ft Pierce, FL 34946 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Florida Atlantic Univ, Dept Environm Sci, Boca Raton, FL 33431 USA. RP Lapointe, BE (reprint author), Harbor Branch Oceanog Inst Inc, 5600 US 1 N, Ft Pierce, FL 34946 USA. EM lapointe@hboi.edu NR 83 TC 63 Z9 74 U1 3 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 J9 HARMFUL ALGAE JI Harmful Algae PD NOV PY 2005 VL 4 IS 6 BP 1092 EP 1105 DI 10.1016/j.hal.2005.06.004 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 984SZ UT WOS:000233325900012 ER PT J AU Lapointe, BE Barile, PJ Littler, MM Littler, DS AF Lapointe, BE Barile, PJ Littler, MM Littler, DS TI Macroalgal blooms on southeast Florida coral reefs II. Cross-shelf discrimination of nitrogen sources indicates widespread assimilation of sewage nitrogen SO HARMFUL ALGAE LA English DT Article DE nitrogen; macroalgae; stable isotopes; coral reefs; eutrophication ID INORGANIC NITROGEN; CAULERPA-TAXIFOLIA; AMMONIUM UPTAKE; STABLE CARBON; DELTA-N-15; SEAGRASS; CHLOROPHYTA; ENRICHMENT; ISOTOPES; N-15 AB Since 1990, coral reefs off southeast Florida have experienced an unprecedented succession of macroalgal blooms and invasions. To determine if anthropogenic land-based nitrogen (N) sources support these HABs, we collected macroalgal tissue for stable nitrogen isotope (815 N) analysis at three spatially distinct depths ranging from the shallow subtidal to the shelf break (similar to 43 m) along seven transects from Jupiter to Deerfield Beach, Florida, USA. This sampling was initiated during a historically significant drought in the spring of 2001 when rainfall, stormwater runoff, and upwelling were at a minimum. The sampling was repeated in the summer wet season following significant stormwater runoff and during a strong upwelling event. Despite significant seasonal changes in N source availability, delta(15) N values did not vary between samplings. Collectively, delta(15) N values were significantly higher on inshore shallow reefs (+8.1 parts per thousand) compared to mid (+6.1 parts per thousand) and deep reefs (+6.7 parts per thousand). Values were also elevated in the southern portion of the study area (e.g., Boca Raton, +8.5 parts per thousand) where nearly 1.5 billion 1/day of secondarily treated wastewater is discharged into the ocean via coastal outfalls. Codium isthmocladum, a macroalga that assimilates its nutrients entirely from the water column, was the dominant bloom species in the southern study area, where tissue delta(15) N values matched source values of nearby sewage outfalls. The northern study area was dominated by species of the genus Caulerpa, particularly the invasive Pacific native C brachypus var. parvifolia, which are capable of accessing benthic nutrient sources (e.g., submarine groundwater discharge, SGD) by means of root-like rhizoids. The northern area does not have sewage outfalls but features a highly transmissive geologic zone where SGD may be enriched with septic tank leachate and effluent from municipal deep injection wells. Multiple lines of evidence supported the hypothesis that land-based sewage N was more important than upwelling as a N source to these HABs: (1)delta(15) N values were highest on shallow reefs and decreased with increasing depth, indicating land-based sources of enrichment; (2) elevated delta(15) N values occurred in these HABs during the dry season, prior to the onset of the summer upwelling; (3) elevated NH4+ concentrations occur on these reefs during both upwelling and non-upwelling periods and are kinetically preferred by macroalgae compared to upwelled NO3-. These findings provide a case study of a coupling between increasing anthropogenic activities and the development of macroalgal HABs, including invasive species that threaten economically important reef resources in southeast Florida. (c) 2005 Published by Elsevier B.V. C1 Harbor Branch Oceanog Inst Inc, Div Marine Sci, Ft Pierce, FL 34946 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Lapointe, BE (reprint author), Harbor Branch Oceanog Inst Inc, Div Marine Sci, 5600 US 1 N, Ft Pierce, FL 34946 USA. EM lapointe@hboi.edu NR 72 TC 93 Z9 101 U1 2 U2 29 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 J9 HARMFUL ALGAE JI Harmful Algae PD NOV PY 2005 VL 4 IS 6 BP 1106 EP 1122 DI 10.1016/j.hal.2005.06.002 PG 17 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 984SZ UT WOS:000233325900013 ER PT J AU Pardo, JR Serabyn, E Wiedner, MC AF Pardo, JR Serabyn, E Wiedner, MC TI Broadband submillimeter measurements of the full Moon center brightness temperature and application to a lunar eclipse SO ICARUS LA English DT Article DE Moon; surface; radio observations; data reduction techniques ID FOURIER-TRANSFORM SPECTROMETER; ATMOSPHERIC TRANSMISSION; MAUNA-KEA; CALIBRATION; MICROWAVE; OPACITY; SURFACE; PHASE AB We report oil observations of the full Moon brightness temperature covering the frequency range of 300-950 GHz, and also on observations of the lunar eclipse of July 16, 2000, though only covering the frequency range of 165-365 GHz due to poor atmospheric transmission at higher frequencies. All observations were performed from the summit of Mauna Kea (HI) using a Fourier Transform Spectrometer mounted on the Caltech Submillimeter Observatory and Supplemented by measurements of the atmospheric opacity using a 183 GHz Water Vapor Monitor. The telescope was pointed to the center of the lunar disk (with a footprint of similar to 45-15 km on the Moon at 300 through 900 GHz). In order to obtain the correct values of the Moon brightness temperatures at all frequencies we carefully corrected for the atmospheric absorption, which varies across the submillimeter domain. This correction is fully described. The measured pre-eclipse brightness temperature is around 337 K in the 165-365 GHz range. This temperature slightly increases with frequency to reach similar to 353 K at 950 GHz, according to previous broader band data. The magnitude of the temperature drop observed during the eclipse at 265 GHz (central frequency of the band covered) was about similar to 70 K, in very good agreement with previous millimeter-wave measurements of other lunar eclipses. We detected, in addition, a clear frequency trend in the temperature drop that. has been compared to a thermal and microwave emission model of the lunar regolith, with the result of a good match of the relative flux drop at different frequencies between model and measurements. (c) 2005 Elsevier Inc. All rights reserved. C1 CSIC, Dept Astrofis Mol & Infrarroja, IEM, E-28006 Madrid, Spain. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Univ Cologne, Inst Phys, D-50937 Cologne, Germany. RP Pardo, JR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pardo@damir.iem.csic.es NR 19 TC 5 Z9 6 U1 0 U2 1 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 NOV 1 PY 2005 VL 178 IS 1 BP 19 EP 26 DI 10.1016/j.icarus.2005.04.005 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977ZA UT WOS:000232840800003 ER PT J AU Gingerich, O AF Gingerich, O TI The church and Galileo. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD NOV PY 2005 VL 36 BP 443 EP 447 PN 4 PG 5 WC History & Philosophy Of Science SC History & Philosophy of Science GA 978MN UT WOS:000232877800005 ER PT J AU Gingerich, O AF Gingerich, O TI Retrying Galileo, 1633-1992. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD NOV PY 2005 VL 36 BP 443 EP 447 PN 4 PG 5 WC History & Philosophy Of Science SC History & Philosophy of Science GA 978MN UT WOS:000232877800004 ER PT J AU Reed, DN AF Reed, DN TI Taphonomic implications of roosting behavior and trophic habits in two species of African owl SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE micromammals; Serengeti; Tarangire; taphonomy; Bubo africanus; Tyto alba ID SOUTH-AFRICA; TYTO-ALBA; BARN OWL; ASSEMBLAGES; PREY; PALEOENVIRONMENTS; ACCUMULATIONS; PALEOECOLOGY AB As some of the most common predators of micromammals, owls are implicated in the formation of many fossil assemblages. Actualistic research on owl-accumulated assemblages has tended to focus on owls roosting in caves. Comparatively few data are available on the roosting behavior, and prey preference of owls in open habitats. This paper presents observations on the roosting and prey habits of two sympatric species of owl in the Serengeti region of northern Tanzania, the Barn Owl, Tyto alba affinis, and the Spotted Eagle Owl, Bubo africanus. The Barn Owl and Spotted Eagle Owl are found to segregate by roosting habit, with Barn Owls occupying cavity roosts and Eagle Owls appearing on the ground or in tree crowns. Previous studies comparing these two species suggested a close similarity in trophic habits. A comparison of large samples (MNI = 1012) at cavity and exposed roosts shows identical taxonomic representation, though differences are found in the relative abundance of some taxa and significant differences in prey body mass. (c) 2005 Elsevier Ltd. All rights reserved. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Reed, DN (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, 10th & Constitut Ave NW,MRC NHB 121, Washington, DC 20013 USA. EM reedd@nmnh.si.edu NR 68 TC 18 Z9 20 U1 0 U2 6 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD NOV PY 2005 VL 32 IS 11 BP 1669 EP 1676 DI 10.1016/j.jas.2005.05.007 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 970XG UT WOS:000232345100010 ER PT J AU Keita, SOY AF Keita, SOY TI Early Nile Valley farmers from El-Badari - Aboriginals or "European" agronostratic immigrants? Craniometric affinities considered with other data SO JOURNAL OF BLACK STUDIES LA English DT Article DE biological distance; phenetic; cluster analysis; agriculture; Afro-Asiatic; predynastic ID HUMAN-POPULATIONS; GENETIC-EVIDENCE; AGRICULTURE; EGYPT AB Male Badarian crania were analyzed using the generalized distance of Mahalanobis in a comparative analysis with other African and European series from the Howells's database. The study was carried out to examine the affinities of the Badarians to evaluate, in preliminary fashion, a demic diffusion hypothesis that postulates that horticulture and the Afro-Asiatic language family were brought ultimately from southern Europe. (The assumption was made that the southern Europeans would be more similar to the central and northern Europeans than to any indigenous African populations.) The Badarians show a greater affinity to indigenous Africans while not being identical. This suggests that the Badarians were more affiliated with local and an indigenous African population than with Europeans. It is more likely that Near Eastern/southern European domesticated animals and plants were adopted by indigenous Nile Valley people without a major immigration of non-Africans. There was more of cultural transfer. C1 Howard Univ, Smithsonian Inst, Sch Med, Natl Human Genome Ctr, Washington, DC USA. RP Keita, SOY (reprint author), Howard Univ, Smithsonian Inst, Sch Med, Natl Human Genome Ctr, Washington, DC USA. NR 44 TC 2 Z9 2 U1 0 U2 1 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0021-9347 J9 J BLACK STUD JI J. Black Stud. PD NOV PY 2005 VL 36 IS 2 BP 191 EP 208 DI 10.1177/0021934704265912 PG 18 WC Ethnic Studies; Social Sciences, Interdisciplinary SC Ethnic Studies; Social Sciences - Other Topics GA 973NL UT WOS:000232529800002 ER PT J AU Lokvam, J Kursar, TA AF Lokvam, J Kursar, TA TI Divergence in structure and activity of phenolic defenses in young leaves of two co-occurring Inga species SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Inga goldmanii; Inga umbellifera; Heliothis virescens; epicatechin-4 beta -> 8-catechin-4 alpha -> 8-epicatechin; flavan-3-ol glycoside; procyanidin; condensed tannin; polyphenol; phenolic; protein precipitation; bioassay; bioactivity; chemical defense evolution ID CONDENSED TANNINS; PLANT PROANTHOCYANIDINS; DIGESTIVE ENZYMES; PROCYANIDINS; PROTEIN; PRECIPITATION AB The leaves of tropical forest trees are most likely to suffer herbivore damage during the period of expansion. Herbivore selection on young leaves has given rise to a variety of leaf developmental strategies and age-specific chemical defense modes. We are studying correlations between leaf developmental types and chemical defenses in the Neotropical genus Inga. We have characterized defense metabolites in Inga goldmanii and Inga umbellifera, two species that co-occur in the lowland moist forest of Panama. These congeners have markedly different young-leaf developmental phenotypes but suffer approximately equal rates of herbivory. Bioassays of whole and fractionated leaf extracts using larvae of Heliothis virescens show that I. goldmanii chemical defenses are nearly three times more inhibitory than those of I. umbellifera. In both species, most of the inhibitory activity resides in complex mixtures of monomeric and polymeric flavan-3-ols. This group comprises > 30% of young leaf dry weight in both I. goldmanii and I. umbellifera. The species' phenolic chemistry differs markedly, however, both in the structure of the monomeric units and in the distribution of polymer sizes. The differences in chemical structure have pronounced effects on their bioactivities, with I. goldmanii flavans being twice as inhibitory to H. virescens larvae as I. umbellifera flavans, and more than three times more efficient at protein binding. Given the extraordinarily high polyphenol concentrations that are found in the young leaves of these species, protein precipitation could be an important mechanism of growth inhibition. Nevertheless, our data show that another mode of phenolic action, possibly oxidative stress, occurs simultaneously. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Lokvam, J (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM lokvam@biology.utah.edu NR 27 TC 22 Z9 24 U1 0 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD NOV PY 2005 VL 31 IS 11 BP 2563 EP 2580 DI 10.1007/s10886-005-7614-x PG 18 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 981QG UT WOS:000233102500005 PM 16273429 ER PT J AU Cipriani, R Collin, R AF Cipriani, R Collin, R TI Life-history invariants with bounded variables cannot be distinguish from data generated by random processes using standard analyses SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE hypothesis testing; linear regression; L(x(m))/L-inf; Protandry; sex change ID PARASITIC NEMATODES; SEX-CHANGE; SIZE; AGE; EVOLUTION; GROWTH; REPRODUCTION; ANIMALS; MODELS; FISH AB A dimensionless approach to the study of life-history evolution has been applied to a wide variety of variables in the search for life-history invariants. This approach usually employs ordinary least squares (OLS) regressions of log-transformed data. In several well-studied combinations of variables the range of values of one parameter is bounded or limited by the value of the other. In this situation, the null hypothesis normally applied to regression analysis is not appropriate. We generate the null expectations and confidence intervals (CI) for OLS and reduced major axis (RMA) regressions using random variables that are bounded in this way. Comparisons of these CI show that, for log-transformed data, the patterns generated by random data and those predicted by life history invariant theory often could not be distinguished because both predict a slope of 1. We recommend that tests based on the putative invariant ratios and not the correlations between the two variables be used in the exploration of life-history invariants using bounded data. Because empirical data are often not normally distributed randomization test may be more appropriate than standard statistical tests. C1 Univ Simon Bolivar, Dept Estudios Ambientales, Caracas 1080, Venezuela. Smithsonian Trop Res Inst, Balboa, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 43002 USA. EM colllinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 17 TC 10 Z9 10 U1 0 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD NOV PY 2005 VL 18 IS 6 BP 1613 EP 1618 DI 10.1111/j.1420-9101.2005.00949.x PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 982GL UT WOS:000233146000023 PM 16313472 ER PT J AU Pearlman, M Noll, C Dunn, P Horvath, J Husson, V Stevens, P Torrence, M Vo, H Wetzel, S AF Pearlman, M Noll, C Dunn, P Horvath, J Husson, V Stevens, P Torrence, M Vo, H Wetzel, S TI The International Laser Ranging Service and its support for IGGOS SO JOURNAL OF GEODYNAMICS LA English DT Article; Proceedings Paper CT 23rd General Assembly of the International-Union-of-Geodesy-and Geophysics CY JUL, 2003 CL Sapporo, JAPAN SP Int Union Geodesy & Geophys DE European Data Center; International Laser Ranging Service; International Earth Rotation Service AB The International Laser Ranging Service (ILRS) was established in September 1998 as a service within the IAG to support programs in geodetic, geophysical, and lunar research activities and to provide data products to the International Earth Rotation Service (IERS) in support of its prime objectives. Now in operation for 5 years,the ILRS develops: (1)the standards and specifications necessary for product consistency and (2) the priorities and tracking strategies required to maximize network efficiency. The service collects, merges, analyzes, archives and distributes satellite and lunar laser ranging data to satisfy a variety of scientific. engineering, and operational needs and encourages the application of new technologies to enhance the quality, quantity. and cost effectiveness of its data products. The ILRS works with: (1) the global network to improve station performance (2) new satellite missions in the design and building of retroreflector targets to maximize data quality and quantity and (3) science programs to optimize scientific data yield. The ILRS Central Bureau maintains a comprehensive web site as the primary vehicle for the distribution of information within the ILRS community. The site, which can be accessed at: http://ilrs.gsfc.nasa.gov is also available at mirrored sites at the Communications Research Laboratory (CRL) in Tokyo and the European Data Center (1,DC) in Munich. During the last 2 years, the ILRS has addressed very important challenges: (1) data from the field stations are now submitted hourly and made available immediately through the data centers for access by the user community (2) tracking on low satellites has been significantly improved through the sub-daily issue of predictions. drag functions. and the real-time exchange of time biases (3) analysis products are now submitted in SINEX format for compatibility with the other space geodesy techniques; (4) the Analysis Working Group is heavily engaged in Pilot Projects as it works toward an ILRS "standard" global solution and (5) SLR has significantly increased its participation in the International Terrestrial Reference Frame (ITRF) activity, which is important to the success of IGGOS. (c) 2005 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Raytheon Informat Technol & Sci Serv, Lanham, MD 20706 USA. Honeywell Tech Solut Inc, Lanham, MD 20706 USA. RP Pearlman, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mpearlman@cfa.harvard.edu; Carey.E.Noll@nasa.gov RI Noll, Carey/D-8884-2012 NR 0 TC 3 Z9 6 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0264-3707 J9 J GEODYN JI J. Geodyn. PD NOV-DEC PY 2005 VL 40 IS 4-5 BP 470 EP 478 DI 10.1016/j.jog.2005.06.009 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 998OA UT WOS:000234327200013 ER PT J AU Boardman, RS Buttler, CJ AF Boardman, RS Buttler, CJ TI Zooids and extrazooidal skeleton in the order trepostomata (Bryozoa) SO JOURNAL OF PALEONTOLOGY LA English DT Article ID MORPHOLOGY; FAMILY AB Reconsideration of the nature of zooids in trepostornate Bryozoa defines them as physically connected and asexually replicated colony members that housed systems of organs necessary to perform vital functions for the colonies. Zooids known to contain organs in trepostomes are limited to autozooids, the requisite feeding and sexual units, and polymorphs, including macrozooids and two rare zooids of unknown function. Other colony structures are extrazooidal and remain outside zooidal boundaries throughout colony life. They include the commonly occurring mesopores, exilapores, and styles. This two-part morphologic division of colonies reveals two correlated functions. The essential autozooids dominated the growth patterns and physiology of trepostome colonies; the extrazooidal parts grew concurrently and passively to connect autozooids and to support and strengthen colonies. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Natl Museums & Galleries Wales, Dept Geol, Cardiff CF10 3NP, Wales. RP Boardman, RS (reprint author), 3612 E Forest Lake Dr, Sarasota, FL 34232 USA. EM richbryozoa@comcast.net; caroline.buttler@nmgw.ac.uk NR 47 TC 4 Z9 4 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD NOV PY 2005 VL 79 IS 6 BP 1088 EP 1104 DI 10.1666/0022-3360(2005)079[1088:ZAESIT]2.0.CO;2 PG 17 WC Paleontology SC Paleontology GA 976IW UT WOS:000232727900004 ER PT J AU Niro, F Jucks, K Hartmann, JM AF Niro, F Jucks, K Hartmann, JM TI Spectra calculations in central and wing regions of CO2IR bands. IV: Software and database for the computation of atmospheric spectra SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CO2 atmospheric spectra; line-mixing; spectral shape ID 20 MU-M; SOLAR OCCULTATION SPECTRA; LIMB EMISSION-SPECTRA; INFRARED Q BRANCHES; RADIATIVE-TRANSFER; TEMPERATURE-DEPENDENCE; LINE-SHAPE; MODEL; ABSORPTION; RETRIEVAL AB In the preceding companion papers a model, based on the impact and the Energy-Corrected Sudden approximations, was proposed for the calculation of the absorption shape of CO2 in both central and wing regions of infrared bands. It was successfully tested using laboratory measurements as well as atmospheric transmission and emission spectra in the 10-20 mu m interval. In the present paper, this approach is used to generate a set of suitable parameters and FORTRAN software for the calculation of absorption by CO2 under atmospheric conditions which can be easily included in radiance/transmission computer codes. This package which includes all bands of significant contribution to atmospheric spectra, is an extension, now accounting for all P, Q, and R lines, of the tools proposed previously for Q branches only. Comparisons between balloon-borne limb emission stratospheric spectra and the results of forward calculations confirm the quality of the tools proposed. (c) 2005 Elsevier Ltd. All rights reserved. C1 CNRS, Photophys Mol Lab, UPR 3361, F-91405 Orsay, France. Univ Paris 11, F-91405 Orsay, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartmann, JM (reprint author), CNRS, Photophys Mol Lab, UPR 3361, Bat 425, F-91405 Orsay, France. EM jean-michel.hartmann@ppm.u-psud.fr NR 39 TC 48 Z9 52 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV 1 PY 2005 VL 95 IS 4 BP 469 EP 481 DI 10.1016/j.jqsrt.2004.11.011 PG 13 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 937KE UT WOS:000229922200002 ER PT J AU Tai, RH Sadler, PM Loehr, JF AF Tai, RH Sadler, PM Loehr, JF TI Factors influencing success in introductory college chemistry SO JOURNAL OF RESEARCH IN SCIENCE TEACHING LA English DT Article ID HIGH-SCHOOL; DECISION-MAKING; SCIENCE; STUDENTS; PHYSICS; GENDER; ACHIEVEMENT; PERCEPTIONS; EDUCATION; MEMORY AB Previous research has found a wide range of predictors of student performance in introductory college chemistry. These predictors are associated with both the students' backgrounds and their high school learning experiences. The purpose of this research study was to examine the link between high school chemistry pedagogical experiences and performance in introductory college chemistry while accounting for individual educational and demographic differences. The researchers surveyed 1531 students enrolled in first-semester introductory college chemistry courses for science and engineering majors at 12 different U.S. colleges and universities. Using multiple regression analysis, the researchers uncovered several interesting high school pedagogical experiences that appeared to be linked with varying levels of performance in college chemistry. Most notably, the researchers found that repeating chemistry labs for understanding was associated with higher student grades, whereas overemphasis on lab procedure in high school chemistry was associated with lower grades in college. These results suggest that high school teachers' pedagogical choices may have a link to future student performance. (c) 2005 Wiley Periodicals, Inc. C1 Univ Virginia, Curry Sch Educ, Charlottesville, VA 22904 USA. Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Philips Auditorium, Cambridge, MA USA. RP Tai, RH (reprint author), Univ Virginia, Curry Sch Educ, 405 Emmet St S, Charlottesville, VA 22904 USA. EM rht6h@virginia.edu NR 67 TC 32 Z9 34 U1 2 U2 20 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0022-4308 J9 J RES SCI TEACH JI J. Res. Sci. Teach. PD NOV PY 2005 VL 42 IS 9 BP 987 EP 1012 DI 10.1002/tea.20082 PG 26 WC Education & Educational Research SC Education & Educational Research GA 981ZZ UT WOS:000233127800002 ER PT J AU Riley, S AF Riley, S TI A time to run. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 1 PY 2005 VL 130 IS 18 BP 63 EP 63 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 031PV UT WOS:000236717400038 ER PT J AU Rocha, LA Robertson, DR Rocha, CR Van Tassell, JL Craig, MT Bowens, BW AF Rocha, LA Robertson, DR Rocha, CR Van Tassell, JL Craig, MT Bowens, BW TI Recent invasion of the tropical Atlantic by an Indo-Pacific coral reef fish SO MOLECULAR ECOLOGY LA English DT Article DE agulhas leakage; biogeography; dispersal; mtDNA; phylogeography ID MITOCHONDRIAL-DNA; GNATHOLEPIS TELEOSTEI; GLOBAL PHYLOGEOGRAPHY; POPULATION-STRUCTURE; MOLECULAR PHYLOGENY; EVOLUTION; SPECIATION; PERCIFORMES; COALESCENT; PATTERNS AB The last tropical connection between Atlantic and Indian-Pacific habitats closed c. 2 million years ago (Ma), with the onset of cold-water upwelling off southwestern Africa. Yet comparative morphology indicates more recent connections in several taxa, including reefassociated gobies (genus Gnatholepis). Coalescence and phylogenetic analyses of mtDNA cytochrome b sequences demonstrate that Gnatholepis invaded the Atlantic during an interglacial period similar to 145 000 years ago (d = 0.0054), colonizing from the Indian Ocean to the western Atlantic, and subsequently to the central (similar to 100 000 years ago) and eastern Atlantic (similar to 30 000 years ago). Census data show a contemporary range expansion in the northeastern Atlantic linked to global warming. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Hofstra Univ, Dept Biol, Hempstead, NY 11549 USA. Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. RP Rocha, LA (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO,AA, Miami, FL 34002 USA. EM rochal@naos.si.edu RI Rocha, Luiz/C-5107-2011 NR 45 TC 86 Z9 92 U1 1 U2 12 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD NOV PY 2005 VL 14 IS 13 BP 3921 EP 3928 DI 10.1111/j.1365-294X.2005.02698.x PG 8 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 977AE UT WOS:000232774000002 PM 16262848 ER PT J AU Perdices, A Doadrio, I Bermingham, E AF Perdices, A Doadrio, I Bermingham, E TI Evolutionary history of the synbranchid eels (Teleostei : Synbranchidae) in Central America and the Caribbean islands inferred from their molecular phylogeny SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE neotropical freshwater fishes; mitochondrial DNA; ATP synthase 8/6; cytochrome b; RAG-1; Synbranchus; Ophisternon; swamp eels; Mesoamerica ID MITOCHONDRIAL-DNA SEQUENCES; FRESH-WATER FISHES; ICE AGES; BIOGEOGRAPHY; CONGRUENCE; DIVERGENCE; PATTERNS; CATFISH AB Swamp eels of the genera Synbranchus and Ophisternon are secondary freshwater fishes whose biogeography provides evidence of their long residence in Mesoamerica, while their impoverished species-level taxonomy might suggest a more recent diversification or a conservative morphology. We have inferred the phylogenetic relationships of Synbranchus marmoratus and Ophisternon aenigmaticum from 45 drainages throughout South, Central America, and Cuba based on mitochondrial genes (cytochrome b and ATPase 8/ 6). Phylogeographic analysis supported the monophyly of Mesoamerican O. aenigmaticum although our results suggest that S. marmoratus is not a monophyletic group. We found a evolutionary differentiated Synbranchus mtDNA lineage inhabiting Las Perlas islands (Pacific Panama) that appeared to be taxonomically distinct and separated for a long period of time from the main Synbranchus clade. Major synbranchid clades were also corroborated with the nuclear RAG-I gene (1171-bp). Application of two fish-based mtDNA clocks (1.05 - 1.3 % pairwise divergence/million year (Ma)), is in accordance with the Godwanian origin suggested for the Synbranchidae. The mtDNA lineages exhibited a remarkable geographic structure in Central America suggesting that vicariance has most likely promoted the Synbranchus and Ophisternon mtDNA diversification. Although our data indicate the importance of the Pacific area in Synbranchus differentiation, the mtDNA divergence between South and Central American Synbranchus is too small to support Cretaceous colonization via the proto-Antillean bridge suggested by Rosen [Syst. Zool. 24 (1976) 43 1]. Instead, our phylogeographic results suggest that Ophisternon and Synbranchus mtDNA clades most likely colonized Central America during the Miocene (12.7 - 23 Ma) prior the final closure of the Isthmus of Panama (3.3 Ma). (c) 2005 Elsevier Inc. All rights reserved. C1 CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. Smithsonian Trop Res Inst, Balboa, Panama. RP Perdices, A (reprint author), Univ Lisbon, Fac Ciencias, Dept Anim Biol, Ctr Biol Ambiental, Bloco C-2,30 Piso,Campo Grande, P-1749016 Lisbon, Portugal. EM aperdices@fc.ul.pt OI Doadrio, Ignacio/0000-0003-4863-9711 NR 45 TC 50 Z9 51 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 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD NOV PY 2005 VL 37 IS 2 BP 460 EP 473 DI 10.1016/j.ympev.2005.01.020 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 979VS UT WOS:000232973700011 PM 16223677 ER PT J AU Grindlay, JE AF Grindlay, JE TI EXIST: All-sky hard X-ray imaging and spectral-temporal survey for black holes SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Conference on Wide-Field Imaging from Space CY MAY 16-18, 2004 CL Lawrence Berkeley Natl Lab, Berkeley, CA HO Lawrence Berkeley Natl Lab AB The energetic X-ray imaging survey telescope (EXIST) is under study for the proposed Black Hole Finder Probe, one of the three Einstein Probe missions in NASA's proposed Beyond Einstein Program. EXIST would have unique capabilities: it would survey the full sky at 5-600 keV each 95 min orbit with 0.9-5', 10 mu s-45 min and similar to 0.5-5 keV resolution to locate sources to 10" and enable black holes to be surveyed and studied on all scales. With a 1y/5 sigma survey sensitivity F-x (40-80 keV) similar to 5 x 10(-13) erg cm(-2) s(-1), comparable to the ROSAT soft X-ray (0.3-2.5 keV) sky survey, a large sample (greater than or similar to 2-4 x 10(4)) of obscured AGN will be identified and a complete sample of accreting stellar mass BHs in the Galaxy will be found. The all-sky/all-time coverage will allow rare events to be measured, such as possible stellar disruption flares from dormant AGN out to similar to 100 Mpc. A large sample (similar to 2-3/day) of GRBs will be located (less than or similar to 10") at sensitivities and bandwidths much greater than previously and likely yield the highest redshift events and constraints on Pop III BHs. An outline of the mission design from the ongoing concept study is presented. (c) 2005 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM josh@cfa.harvard.edu NR 11 TC 20 Z9 20 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD NOV PY 2005 VL 49 IS 7-9 BP 436 EP 439 DI 10.1016/j.newar.2005.08.019 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 985NP UT WOS:000233385000019 ER PT J AU Childress, L Taylor, JM Sorensen, AS Lukin, MD AF Childress, L Taylor, JM Sorensen, AS Lukin, MD TI Fault-tolerant quantum repeaters with minimal physical resources and implementations based on single-photon emitters SO PHYSICAL REVIEW A LA English DT Article ID NOISY CHANNELS; HIGH-STABILITY; COMMUNICATION; CRYPTOGRAPHY; ENTANGLEMENT; CAVITY; TELEPORTATION; STATE; PURIFICATION; DIAMOND AB We analyze a method that uses fixed, minimal physical resources to achieve generation and nested purification of quantum entanglement for quantum communication over arbitrarily long distances and discuss its implementation using realistic photon emitters and photonic channels. In this method, we use single-photon emitters with two internal degrees of freedom formed by an electron spin and a nuclear spin to build intermediate nodes in a quantum channel. State-selective fluorescence is used for probablistic entanglement generation between electron spins in adjacent nodes. We analyze in detail several approaches which are applicable to realistic, homogeneously broadened single-photon emitters. Furthermore, the coupled electron and nuclear spins can be used to efficiently implement entanglement swapping and purification. We show that these techniques can be combined to generate high-fidelity entanglement over arbitrarily long distances. We present a specific protocol that functions in polynomial time and tolerates percent-level errors in entanglement fidelity and local operations. The scheme has the lowest requirements on physical resources of any current scheme for fully fault-tolerant quantum repeaters. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. RP Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Childress, Lilian/H-1359-2012; Taylor, Jacob/B-7826-2011; Sorensen, Anders/L-1868-2013 OI Childress, Lilian/0000-0002-0507-6392; Taylor, Jacob/0000-0003-0493-5594; Sorensen, Anders/0000-0003-1337-9163 NR 50 TC 176 Z9 178 U1 2 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 2005 VL 72 IS 5 AR 052330 DI 10.1103/PhysRevA.72.052330 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 988LT UT WOS:000233603400069 ER PT J AU Santamore, DH Timmermans, E AF Santamore, DH Timmermans, E TI Collective excitations of low-density fermion-boson quantum-liquid mixtures SO PHYSICAL REVIEW A LA English DT Article ID EINSTEIN CONDENSATE; DILUTE SOLUTIONS; HE3 ATOMS; GAS; SYSTEM AB We investigate the collective excitations of a low-temperature dilute gas mixture that consists of a Bose-Einstein condensate (BEC) and a Fermi gas that is a normal (i.e., nonsuperfluid) Fermi liquid. We find that the BEC-mediated fermion-fermion interactions, as a consequence of retardation, can become repulsive and support a zero-sound mode that is essentially undamped. In addition, we find a damped zero-sound mode that can be described as a BEC sound mode modified by fermion-mediated boson-boson interactions, and we derive its decay rate caused by Landau damping. We study the mode structure of these excitations and find avoided-crossing behavior as well as a termination point. The collective-mode dynamics also reveals that phase separation sets in when the fermion-mediated boson-boson interaction destroys the stability of the homogeneous BEC. We estimate the time and length scales of the onset of the phase separation, and we discuss the feasibility of experimentally probing these consequences of mediated interactions. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Los Alamos Natl Lab, Div Theory, Los Alamos, NM 87545 USA. RP Santamore, DH (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. NR 39 TC 4 Z9 4 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 2005 VL 72 IS 5 AR 053601 DI 10.1103/PhysRevA.72.053601 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 988LT UT WOS:000233603400134 ER PT J AU Turner, BL Mahieu, N Condron, LM Chen, CR AF Turner, BL Mahieu, N Condron, LM Chen, CR TI Quantification and bioavailability of scyllo-inositol hexakisphosphate in pasture soils SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE pasture soil; inositol phosphate; myo-inositol hexakisphosphate scyllo-inositol hexakisphosphate; phytic acid; solution P-31 NMR spectroscopy ID P-31 NMR-SPECTROSCOPY; PHOSPHATES; FUNGI AB The recent identification of scyllo-inositol hexakisphosphate in alkaline soil extracts by solution P-31 NMR spectroscopy allowed us to investigate this compound in soils by re-analyzing spectra from two previously published studies. Concentrations of scyllo-inositol hexakisphosphate in 29 temperate pasture soils from England and Wales ranged between 11 and 130 mg P kg(-1) soil and accounted for between 4 and 15% of the soil organic phosphorus. The ratio of scyllo-inositol hexakisphosphate to myo-inositol hexakisphosphate ranged between 0.29 and 0.79. In a 10 month pot experiment with six grassland soils from New Zealand, growth of pine seedlings (Pinus radiata D. Don) decreased scyllo-inositol hexakisphosphate concentrations by between 10 and 46%. Growth of ryegrass (Lolium perenne L.) decreased scyllo-inositol hexakisphosphate in three low-nutrient soils by 5-21%, but increased it in three other soils by 11-16%. We conclude that scyllo-inositol hexakisphosphate is an important component of soil organic phosphorus with potential ecological significance. (c) 2005 Elsevier Ltd. All rights reserved. C1 Smithsonian Trop Res Inst, Panama City, Panama. Queen Mary Univ London, Dept Chem, London E1 4NS, England. Lincoln Univ, Canterbury, New Zealand. Griffith Univ, Fac Environm Sci, Ctr Forestry & Hort Res, Nathan, Qld 4111, Australia. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM turnerbl@si.edu RI Turner, Benjamin/E-5940-2011; Condron, Leo/E-9458-2013; Chen, Chengrong/B-3814-2009 OI Turner, Benjamin/0000-0002-6585-0722; Chen, Chengrong/0000-0001-6377-4001 NR 15 TC 23 Z9 25 U1 0 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD NOV PY 2005 VL 37 IS 11 BP 2155 EP 2158 DI 10.1016/j.soilbio.2005.03.005 PG 4 WC Soil Science SC Agriculture GA 987EL UT WOS:000233501100020 ER PT J AU Weiss, JV Emerson, D Megonigal, JP AF Weiss, JV Emerson, D Megonigal, JP TI Rhizosphere iron(III) deposition and reduction in a Juncus effusus L.-dominated wetland SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID FE(III) OXIDE REDUCTION; IRON-OXIDIZING BACTERIA; FRESH-WATER; PHRAGMITES-AUSTRALIS; SALT-MARSH; AQUATIC SEDIMENTS; CARBON OXIDATION; FERRIC IRON; PLANT-ROOTS; FE-PLAQUE AB Iron (III) plaque forms on the roots of wetland plants from the reaction of Fe(II) with O-2 released by roots. Recent laboratory studies have shown that Fe plaque is more rapidly reduced than non-rhizosphere Fe(III) oxides. The goals of the current study were to determine in situ rates of: (i) Fe(III) reduction of root plaque and soil Fe(III) oxides, (ii) root Fe(III) deposition, and (iii) root and soil organic matter decomposition. Iron (III) reduction was investigated using a novel buried-bag technique in which roots and soil were buried in heat-sealed membrane bags (Versapor 200 membrane, pore size = 0.2 mu m) in late fall following plant senescence. Bags were retrieved at monthly intervals for 1 yr to assess changes in total C and Fe mass, Fe mineralogy, Fe(II)[Fe(III) ratio, and the abundances of Fe(II)oxidizing bacteria (FeOB) and Fe(III)-reducing bacteria (FeRB). The soil C and Fe pools did not change significantly throughout the year, but root C and total root Fe mass decreased by 40 and 70%, respectively. When total Fe losses were adjusted for changes in the ratio of Fe(II)[Fe(III), over 95% of the Fe(III) in the plaque was reduced during the 12-mo study, at a peak rate of 0.6 mg Fe(III) g dry weight(-1) d(-1) (gdw(-1) d(-1)). These estimates exceed the crude estimate of Fe(III) accumulation [0.3 mg Fe(III) g dry weight(-1) d(-1)] on bare-root plants that were transplanted into the wetland for a growing season. We concluded that root plaque has the potential to be reduced as rapidly as it is deposited under field conditions. C1 George Mason Univ, Fairfax, VA 22030 USA. Amer Type Culture Collect, Manassas, VA 20110 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Weiss, JV (reprint author), US Geol Survey, Reston, VA USA. EM jweiss@usgs.gov NR 41 TC 38 Z9 47 U1 2 U2 22 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD NOV-DEC PY 2005 VL 69 IS 6 BP 1861 EP 1870 DI 10.2136/sssaj2005.0002 PG 10 WC Soil Science SC Agriculture GA 983HZ UT WOS:000233223500022 ER PT J AU Launius, RD AF Launius, RD TI Moondust: In search of the men who fell to earth SO SPACE POLICY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20013 USA. EM launiusr@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 NOV PY 2005 VL 21 IS 4 BP 317 EP 318 DI 10.1016/j.spacepol.2005.08.002 PG 2 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 995BU UT WOS:000234075700011 ER PT J AU Miller, JA AF Miller, JA TI Cave adaptation in the spider genus Anthrobia (Araneae, Linyphiidae, Erigoninae) SO ZOOLOGICA SCRIPTA LA English DT Article ID SOUTHERN APPALACHIANS ARANEAE; NESTICIDAE; STABILITY; ASTYANAX; AMERICA; CLADE AB The genus Anthrobia Tellkampf, 1844 is revised and expanded to include two epigean species, Anthrobia acuminata (Emerton, 1913) comb. nov., and A. whiteleyae sp. nov., and two troglobites, the type species A. monmouthia Tellkampf, 1844, and A. coylei sp. nov. The female of A. acuminata is described for the first time. All four Anthrobia species were added to a phylogenetic analysis of erigonine genera. Analysis of this matrix results in a single most parsimonious tree (length = 915, CI = 0.23, RI = 0.58; uninformative characters excluded: length = 911, CI = 0.23), which places Anthrobia sister to Diplocentria Hull, 1911. Troglobitic Anthrobia and epigean Anthrobia are both monophyletic. In comparison to the epigean species, troglobitic Anthrobia exhibit the following putative adaptations to cave life: loss of eyes, elongation of the legs, and reduction of the tracheal system. The reliability of phylogenetic results indicating monophyly of cave Anthrobia are discussed in light of the fact that potentially cave adaptive synapomorphies support this relationship. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Miller, JA (reprint author), Calif Acad Sci, Dept Entomol, 875 Howard St, San Francisco, CA 94103 USA. EM zmjeremy@gwu.edu OI Miller, Jeremy/0000-0001-8918-9775 NR 82 TC 8 Z9 10 U1 1 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD NOV PY 2005 VL 34 IS 6 BP 565 EP 592 DI 10.1111/j.1463-6409.2005.00206.x PG 28 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 979XV UT WOS:000232979400003 ER PT J AU Liu, X Chance, K Sioris, CE Spurr, RJD Kurosu, TP Martin, RV Newchurch, MJ AF Liu, X Chance, K Sioris, CE Spurr, RJD Kurosu, TP Martin, RV Newchurch, MJ TI Ozone profile and tropospheric ozone retrievals from the Global Ozone Monitoring Experiment: Algorithm description and validation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ROTATIONAL RAMAN-SCATTERING; BACKSCATTERED ULTRAVIOLET RADIANCES; ABSORPTION CROSS-SECTIONS; MAPPING SPECTROMETER; RADIATIVE-TRANSFER; RAYLEIGH-SCATTERING; SAGE-II; SURFACE REFLECTIVITY; TOMS OZONE; CLIMATOLOGY AB Ozone profiles are derived from back scattered radiance spectra in the ultraviolet (289-339 nm) measured by the Global Ozone Monitoring Experiment (GOME) using the optimal estimation technique. Tropospheric Column Ozone (TCO) is directly derived using the known tropopause to divide the stratosphere and troposphere. To optimize the retrieval and improve the fitting precision needed for tropospheric ozone, we perform extensive wavelength and radiometric calibrations and improve forward model inputs. The a priori influence of retrieved TCO is similar to 15% in the tropics and increases to similar to 50% at high latitudes. The dominant error terms are the smoothing errors, instrumental random-noise errors, and systematic temperature errors. We compare our GOME retrievals with Earth-Probe Total Ozone Mapping Spectrometer (TOMS) Total column Ozone (TO), Dobson/Brewer (DB) TO, and ozonesonde TCO at 33 World Ozone and Ultraviolet Radiation Data Centre (WOUDC) stations between 71 degrees S and 75 degrees N during 1996-1999. The mean biases with TOMS and DB TO are within 6 DU (2%, 1 DU = 2.69 x 10(16) molecules cm(-2)) at most of the stations. The retrieved Tropospheric Column Ozone (TCO) captures most of the temporal variability in ozonesonde TCO; the mean biases are mostly within 3 DU (15%) and the standard deviations (1 sigma) are within 3-8 DU (13-27%). We also compare our retrieved ozone profiles above similar to 15 km against Stratospheric Aerosol and Gas Experiment II measurements from 1996 to 1999. The mean biases and standard deviations are usually within 15%. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. RT Solut Inc, Cambridge, MA USA. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. RP Liu, X (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM xliu@cfa.harvard.edu RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Liu, Xiong/P-7186-2014 OI Martin, Randall/0000-0003-2632-8402; Liu, Xiong/0000-0003-2939-574X NR 68 TC 108 Z9 112 U1 2 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 29 PY 2005 VL 110 IS D20 AR D20307 DI 10.1029/2005JD006240 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 981RV UT WOS:000233106600003 ER PT J AU Janzen, DH Hajibabaei, M Burns, JM Hallwachs, W Remigio, E Hebert, PDN AF Janzen, DH Hajibabaei, M Burns, JM Hallwachs, W Remigio, E Hebert, PDN TI Wedding biodiversity inventory of a large and complex Lepidoptera fauna with DNA barcoding SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Costa Rica; tropical; Area de Conservacion Guanacaste; Hesperiidae; Saturniidae; Sphingidae ID PHYLOGEOGRAPHY AB By facilitating bioliteracy, DNA barcoding has the potential to improve the way the world relates to wild biodiversity. Here we describe the early stages of the use of cox1 barcoding to supplement and strengthen the taxonomic platform underpinning the inventory of thousands of sympatric species of caterpillars in tropical dry forest, cloud forest and rain forest in northwestern Costa Rica. The results show that barcoding a biologically complex biota unambiguously distinguishes among 97% of more than 1000 species of reared Lepidoptera. Those few species whose barcodes overlap are closely related and not confused with other species. Barcoding also has revealed a substantial number of cryptic species among morphologically defined species, associated sexes, and reinforced identification of species that are difficult to distinguish morphologically. For barcoding to achieve its full potential, (i) ability to rapidly and cheaply barcode older museum specimens is urgent, (ii) museums need to address the opportunity and responsibility for housing large numbers of barcode voucher specimens, (iii) substantial resources need be mustered to support the taxonomic side of the partnership with barcoding, and (iv) hand-held field-friendly barcorder must emerge as a mutualism with the taxasphere and the barcoding initiative, in a manner such that its use generates a resource base for the taxonomic process as well as a tool for the user. C1 Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Janzen, DH (reprint author), Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. EM djanzen@sas.upenn.edu RI Hebert, Paul/C-4161-2013 OI Hebert, Paul/0000-0002-3081-6700 NR 21 TC 180 Z9 217 U1 5 U2 30 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD OCT 29 PY 2005 VL 360 IS 1462 BP 1835 EP 1845 DI 10.1098/rstb.2005.1715 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 976FW UT WOS:000232719300004 PM 16214742 ER PT J AU Kiel, S Campbell, KA AF Kiel, S Campbell, KA TI Lithomphalus enderlini gen. et sp nov from cold-seep carbonates in California - a Cretaceous neomphalid gastropod? SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Gastropoda; Neomphalina; cold-seep; California; Cretaceous; Valanginian ID HYDROTHERMAL VENT COMMUNITY; FRANCISCAN COMPLEX; HYDROCARBON SEEPS; SHELL STRUCTURES; ARCHAEOGASTROPOD; PELTOSPIRIDAE; PHYLOGENY; ANTIQUITY; EVOLUTION; MOLLUSCA AB The new genus and species Lithomphalus enderlini is described from two Early Cretaceous (Valanginian) suspected cold-seep carbonates in western California, USA. These carbonates were found within turbidites of the Great Valley Group, and were deposited at slope depth. Considering its shell shape and its crossed-lamellar shell structure, this species might belong to the enigmatic vent and seep endemic gastropod group Neomphaloidea. It cannot be assigned with certainty to any of the extant neomphaloidean families, and thus may represent an independent Mesozoic radiation of the Neomphalina. However, until additional and better-preserved specimens are discovered (e.g., those with protoconchs), caution is advised with regard to verifying the earliest occurrence of the Neomphalidea in the fossil record. (c) 2005 Elsevier B.V. All rights reserved. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. Univ Auckland, Dept Geol, Auckland, New Zealand. Calif Acad Sci, San Francisco, CA 94118 USA. RP Kiel, S (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, MRC 121, POB 37012, Washington, DC 20013 USA. EM kiels@si.edu RI Kiel, Steffen/C-3150-2009; OI Kiel, Steffen/0000-0001-6281-100X; Campbell, Kathleen/0000-0002-4815-2519 NR 47 TC 16 Z9 16 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD OCT 28 PY 2005 VL 227 IS 1-3 BP 232 EP 241 DI 10.1016/j.palaeo.2005.04.022 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 980OU UT WOS:000233028600014 ER PT J AU Kornicker, LS Harrison-Nelson, E AF Kornicker, LS Harrison-Nelson, E TI Two new species of Ostracoda from hydrothermal vents of Riftia pachyptila aggregations on the East Pacific Rise (Halocypridina; Cladocopina) SO ZOOTAXA LA English DT Article DE Ostracoda; Halocyprida; Halocypridina; Cladocopina; taxonomy; new species; Archiconchoecia; Polycopetta; vent ID COMMUNITY; HABITAT; GULF AB Two new species of Ostracoda, Archiconchoecia ( Archiconchoecia) chavturi (Halocypridina) and Polycopetta pax ( Cladocopina), are described from two diffuse flow vent localities (Tica Site and Riftia Field Site) within Riftia pachyptila (Siboglinidae, Vestimentifera) aggregations on the East Pacific Rise, slightly north and west of 9 degrees 50' N, 104 degrees 17' W, depth 2500 m. C1 Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, MRC 163, Washington, DC 20013 USA. EM kornickl@si.edu; nelsone@si.edu NR 15 TC 6 Z9 6 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 OCT 28 PY 2005 IS 1071 BP 19 EP 38 PG 20 WC Zoology SC Zoology GA 979SD UT WOS:000232964200002 ER PT J AU Leal, JH Harasewych, MG AF Leal, JH Harasewych, MG TI Tractolira delli, a new Volutidae (Mollusca : Gastropoda : Neogastropoda) from the abyssal plains off Antarctica SO ZOOTAXA LA English DT Article DE Antarctica; Antarctic; sub-Antarctic; Odontocymbiolinae AB A new deep-sea species of Volutidae in the genus Tractolira is named from material collected by the United States Antarctic Program in and around the Ross Sea, eastern Antarctica, and from one locality in the Subantarctic region. Tractolira delli new species is most similar to T. sparta Dall, 1896, from which it differs in having a relatively wider shell, less prominent spiral sculpture, with narrower threads, and by the absence of strong axial ribs at least on the first three teleoconch whorls. The other Antarctic congener, Tractolira germonae, has a thicker, dark-brown periostracum ( instead of a thin, light-yellow one), a proportionally smaller inductura, and lacks surface sculpture. C1 Bailey Matthews Shell Museum, Sanibel, FL 33957 USA. Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Leal, JH (reprint author), Bailey Matthews Shell Museum, POB 1580, Sanibel, FL 33957 USA. EM jleal@shellmuseum.org; Harasewych@si.edu NR 6 TC 3 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 28 PY 2005 IS 1071 BP 39 EP 45 PG 7 WC Zoology SC Zoology GA 979SD UT WOS:000232964200003 ER PT J AU Hozumi, S Hernquist, L AF Hozumi, S Hernquist, L TI Secular evolution of barred galaxies with massive central black holes SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE black hole physics; galaxies : evolution; galaxies : kinematics and dynamics; galaxies : structure; methods : n-body simulations AB The influence of central black holes on the dynamical evolution of bars in disk galaxies was examined. Once a bar formed by a dynamical instability in an infinitesimally thin stellar disk was fully developed, a black hole (BH) was adiabatically added at the center of the disk. Our results indicate that a bar can be completely destroyed, in a practical sense, in a time much smaller than the Hubble time if the central BH mass exceeds about 0.5% of the disk mass. Since this implied minimum BH mass for bar destruction is on the order of 10(8.5) Me for a typical disk galaxy, this process could occur in the real Universe. The bar amplitude decreases gradually with time after the BH has grown up to its full mass. Surface-of-section plots indicate that the bar dissolution originates from the chaotic behavior of bar-supporting orbits. In addition, the scale length and the radial velocity dispersion of the disk after bar dissolution become much larger than those of the initial axisymmetric disk. This finding suggests that it is. possible to discriminate between genuine non-barred galaxies and bar-dissolved galaxies induced by massive central BHs from the viewpoint of structural properties. C1 Shiga Univ, Fac Educ, Shiga 5200862, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shiga Univ, Fac Educ, 2-5-1 Hiratsu, Shiga 5200862, Japan. EM hozumi@sue.shiga-u.ac.jp; lars@cfa.harvard.edu NR 40 TC 16 Z9 16 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 OCT 25 PY 2005 VL 57 IS 5 BP 719 EP 731 DI 10.1093/pasj/57.5.719 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980XC UT WOS:000233050500007 ER PT J AU Brunken, S Muller, HSP Lewen, F Giesen, TF AF Brunken, S Muller, HSP Lewen, F Giesen, TF TI Analysis of the rotational spectrum of methylene (CH2) in its vibronic ground state with an Euler expansion of the Hamiltonian SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID LASER MAGNETIC-RESONANCE; POTENTIAL SURFACE; MOLECULAR-SPECTROSCOPY; INTERSTELLAR CLOUDS; COLOGNE DATABASE; RADICAL CH2; X3B1; TRANSITION; ABUNDANCES; MODELS AB We present an analysis of a global, field-free data set of the methylene radical CH2 in its X B-3(1) vibronic ground state by means of a novel Euler expansion of the Hamiltonian. The data set comprises pure rotational transitions up to 2 THz obtained with microwave accuracies of 30-500 kHz as well as nu(2) ground-state combination differences and pure rotational data obtained with infrared accuracies of 0.001-0.010 cm(-1). Highly accurate spectroscopic parameters have been determined. These include rotational, spin-spin, spin-rotation, and electron-spin-nuclear-spin coupling terms along with several centrifugal distortion corrections. The spectroscopic model has been tested and improved by recording newly three weak Delta N not equal Delta J fine-structure components of the NKaKc=2(12)-3(03) and 5(05)-4(14) transitions near 434, 454, and 581 GHz. These lines were rather close to the predictions. Overall weighted root mean squares of 1.28 and 0.83 were achieved for fits in which the Euler expansion was used only for the rotational part of the Hamiltonian or for the rotational and spin-spin terms of the Hamiltonian, respectively. The resulting spectroscopic parameters allow for precise frequency predictions of astrophysically important rotational transitions of methylene. (c) 2005 American Institute of Physics. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. 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; Giesen, Thomas /B-9476-2015; OI Brunken, Sandra/0000-0001-7175-4828; Giesen, Thomas /0000-0002-2401-0049; Mueller, Holger/0000-0002-0183-8927 NR 28 TC 11 Z9 12 U1 1 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD OCT 22 PY 2005 VL 123 IS 16 AR 164315 DI 10.1063/1.2074467 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 978EF UT WOS:000232855700036 PM 16268705 ER PT J AU Tamisiea, ME Leuliette, EW Davis, JL Mitrovica, JX AF Tamisiea, ME Leuliette, EW Davis, JL Mitrovica, JX TI Constraining hydrological and cryospheric mass flux in southeastern Alaska using space-based gravity measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CLIMATE EXPERIMENT GRACE; TIME-VARIABLE GRAVITY; ENERGY BALANCES; LAND WATER; SEA-LEVEL; MODEL; VARIABILITY; RECOVERY; GLACIERS AB Watersheds draining into the Gulf of Alaska (GoA) experience large seasonal and inter-annual variations of water in the form of rain, snow, and ice, but accurate constraints on these variations have been difficult to obtain. Over larger geographic regions, water variations can be inferred directly from the Gravity Recovery and Climate Experiment (GRACE) data. However, because GoA variations occur over such a small region, the inferred average value of water flux increases as the applied smoothing of the GRACE data decreases. We use this observed scaling together with scaling results obtained from forward models to infer a seasonal amplitude of 115 +/- 20 km(3) of water and an average contribution to sea level rise over the two years of data of 0.31 +/- 0.09 mm/yr. These results suggest that accelerated melting that began in the late 1990s, as inferred from altimetry, continues unabated. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Tamisiea, ME (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mtamisiea@cfa.harvard.edu RI Leuliette, Eric/D-1527-2010; Davis, James/D-8766-2013 OI Leuliette, Eric/0000-0002-3425-4039; Davis, James/0000-0003-3057-477X NR 16 TC 58 Z9 60 U1 1 U2 5 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 OCT 21 PY 2005 VL 32 IS 20 AR L20501 DI 10.1029/2005GL023961 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 977UK UT WOS:000232828500008 ER PT J AU Broderick, AE Loeb, A AF Broderick, AE Loeb, A TI Imaging bright-spots in the accretion flow near the black hole horizon of Sgr A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; relativity; techniques : interferometric; Galaxy : centre; submillimetre ID COVARIANT MAGNETOIONIC THEORY; ACTIVE GALACTIC NUCLEI; X-RAY BINARIES; K-ALPHA LINE; GALAXY MCG-6-30-15; POLARIZATION; EMISSION; FLARE; DISKS; VARIABILITY AB Images from the vicinity of the black hole horizon at the Galactic centre (Sgr A*) could be obtained in the near future with a Very Large Baseline Array of submillimetre telescopes. The recently observed short-term infrared and X-ray variability of the emission from Sgr A* implies that the accretion flow near the black hole is clumpy or unsteady. We calculate the appearance of a compact emission region (bright-spot) in a circular orbit around a spinning black hole as a function of orbital radius and orientation. We find that the mass and spin of the black hole can be extracted from their generic signatures on the spot image as well as on the light curves of its observed flux and polarization. The strong field distortion remains notable even when the spot image is smoothed over the expected similar to 20-mu as resolution of the future submillimetre observations. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Broderick, AE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM abroderick@cfa.harvard.edu; aloeb@cfa.harvard.edu NR 36 TC 85 Z9 86 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 OCT 21 PY 2005 VL 363 IS 2 BP 353 EP 362 DI 10.1111/j.1365-2966.2005.09458.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 972GB UT WOS:000232441200001 ER PT J AU Robertson, B Bullock, JS Font, AS Johnston, KV Hernquist, L AF Robertson, B Bullock, JS Font, AS Johnston, KV Hernquist, L TI A cold dark matter, stellar feedback, and the galactic halo abundance pattern SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : dwarf; galaxies : evolution; galaxies : formation; galaxy : abundances; galaxy : halo ID DWARF SPHEROIDAL GALAXIES; METAL-POOR STARS; LARGE-MAGELLANIC-CLOUD; AGE-METALLICITY RELATION; INITIAL MASS FUNCTION; MILKY-WAY HALO; CHEMICAL EVOLUTION; SOLAR NEIGHBORHOOD; RED GIANTS; VLT/UVES ABUNDANCES AB The hierarchical formation scenario for the stellar halo requires the accretion and disruption of dwarf galaxies, yet low-metallicity halo stars are enriched in alpha-elements compared to similar, low-metallicity stars in dwarf spheroidal (dSph) galaxies. We address this primary challenge for the hierarchical formation scenario for the stellar halo by combining chemical evolution modeling with cosmologically motivated mass accretion histories for the Milky Way dark halo and its satellites. We demonstrate that stellar halo and dwarf galaxy abundance patterns can be explained naturally within the Lambda CDM framework. Our solution relies fundamentally on the Lambda CDM model prediction that the majority of the stars in the stellar halo were formed within a few relatively massive, similar to 5 x 10(10) M-circle dot, dwarf irregular (dIrr) sized dark matter halos, which were accreted and destroyed similar to 10 Gyr in the past. These systems necessarily have short-lived, rapid star formation histories, are enriched primarily by Type II supernovae, and host stars with enhanced [ alpha/Fe] abundances. In contrast, dwarf dSph galaxies exist within low-mass dark matter hosts of similar to 10(9) M-circle dot, where supernovae winds are important in setting the intermediate [alpha/Fe] ratios observed. Our model includes enrichment from Type Ia and Type II supernovae, as well as stellar winds, and includes a physically motivated supernovae feedback prescription calibrated to reproduce the local dwarf galaxy stellarmass metallicity relation. We use representative examples of the type of dark matter halos that we expect to host a destroyed "stellar halo progenitor'' dwarf, a surviving dIrr, and a surviving dSph galaxy, and show that their derived abundance patterns, stellar masses, and gas masses are consistent with those observed for each type of system. Our model also self-consistently reproduces the observed stellar mass-v(circ) relation for local group satellites and produces the correct cumulative mass for the Milky Way stellar halo. We predict that the lowest metallicity stars in intermediate-mass dIrr galaxies such as the SMC and LMC should follow abundance patterns similar to that observed in the stellar halo. Searches for accreted, disrupted, low-mass dwarfs may be enhanced by searching for unbound stars with dSph-like chemical abundance patterns. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. Wesleyan Univ, Van Vleck Observ, Middletown, CT 06459 USA. RP Robertson, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM brobertson@cfa.harvard.edu RI Bullock, James/K-1928-2015 OI Bullock, James/0000-0003-4298-5082 NR 115 TC 137 Z9 137 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 OCT 20 PY 2005 VL 632 IS 2 BP 872 EP 881 DI 10.1086/452619 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CO UT WOS:000232569100019 ER PT J AU Quillen, AC Thorndike, SL Cunningham, A Frank, A Gutermuth, RA Blackman, EG Pipher, JL Ridge, N AF Quillen, AC Thorndike, SL Cunningham, A Frank, A Gutermuth, RA Blackman, EG Pipher, JL Ridge, N TI Turbulence driven by outflow-blown cavities in the molecular cloud of NGC 1333 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : bubbles; ISM : clouds; ISM : individual (NGC 1333); ISM : jets and outflows; ISM : kinematics and dynamics; ISM : molecules ID HERBIG-HARO FLOWS; YOUNG STELLAR OBJECTS; WIDE-ANGLE WINDS; STAR-FORMATION; NGC 1333; HIGH-RESOLUTION; CO OUTFLOWS; DARK CLOUD; BARNARD 5; (CO)-C-13 AB Outflows from young stellar objects (YSOs) have been identified as a possible source of turbulence in molecular clouds. To investigate the relationship between outflows, cloud dynamics, and turbulence, we compare the kinematics of the molecular gas associated with NGC 1333, traced in (CO)-C-13 (1-0), with the distribution of YSOs within. We find a velocity dispersion of similar to 1-1.6 km s(-1) in (CO)-C-13 that does not significantly vary across the cloud and is uncorrelated with the number of nearby young stellar outflows identified from optical and submillimeter observations. However, from velocity channel maps we identify about 20 depressions in the (CO)-C-13 intensity of scales >= 0.1-0.2 pc and velocity widths 1-3 km s(-1). The depressions exhibit limb-brightened rims in both individual velocity channel maps and position-velocity diagrams, suggesting that they are slowly expanding cavities. We interpret these depressions to be remnants of past YSO outflow activity: if these cavities are presently empty, they would fill in on timescales of similar to 10(6) yr. This can exceed the lifetime of a YSO outflow phase or the transit time of the central star through the cavity, explaining the absence of any clear correlation between the cavities and YSO outflows. We find that the momentum and energy deposition associated with the expansion of the cavities is sufficient to power the turbulence in the cloud. In this way we conclude that the cavities are an important intermediate step between the conversion of YSO outflow energy and momentum into cloud turbulent motions. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Quillen, AC (reprint author), Univ Rochester, Dept Phys & Astron, 601 Elmwood Ave, Rochester, NY 14627 USA. EM aquillen@pas.rochester.edu NR 44 TC 61 Z9 61 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 OCT 20 PY 2005 VL 632 IS 2 BP 941 EP 955 DI 10.1086/444410 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CO UT WOS:000232569100024 ER PT J AU Sloan, GC Keller, LD Forrest, WJ Leibensperger, E Sargent, B Li, A Najita, J Watson, DM Brandl, BR Chen, CH Green, JD Markwick-Kemper, F Herter, TL D'Alessio, P Morris, PW Barry, DJ Hall, P Myers, PC Houck, JR AF Sloan, GC Keller, LD Forrest, WJ Leibensperger, E Sargent, B Li, A Najita, J Watson, DM Brandl, BR Chen, CH Green, JD Markwick-Kemper, F Herter, TL D'Alessio, P Morris, PW Barry, DJ Hall, P Myers, PC Houck, JR TI Mid-infrared spectra of polycyclic aromatic hydrocarbon emission in herbig Ae/Be stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : chemically peculiar ID DIFFUSE INTERSTELLAR-MEDIUM; INFRARED SPECTROGRAPH IRS; SPITZER-SPACE-TELESCOPE; CIRCUMSTELLAR DISK; ISO SPECTROSCOPY; DUST; MOLECULES; FEATURES; PAHS; TEMPERATURES AB We present spectra of four Herbig Ae/Be stars obtained with the Infrared Spectrograph (IRS) on the Spitzer Space Telescope. All four of the sources show strong emission from polycyclic aromatic hydrocarbons (PAHs), with the 6.2 mu m emission feature shifted to 6.3 mu m and the strongest C-C skeletal-mode feature occurring at 7.9 mu m instead of at 7.7 mu m, as is often seen. Remarkably, none of the four stars has silicate emission. The strength of the 7.9 mu m feature varies with respect to the 11.3 mu m feature among the sources, indicating that we have observed PAHs with a range of ionization fractions. The ionization fraction is higher for systems with hotter and brighter central stars. Two sources, HD 34282 and HD 169142, show emission features from aliphatic hydrocarbons at 6.85 and 7.25 mu m. The spectrum of HD 141569 shows a previously undetected emission feature at 12.4 mu m that may be related to the 12.7 mu m PAH feature. The spectrum of HD 135344, the coolest star in our sample, shows an unusual profile in the 7-9 mu m region, with the peak emission to the red of 8.0 mu m and no 8.6 mu m PAH feature. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. CALTECH, Ctr Infrared Proc & Anal, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sloan, GC (reprint author), Cornell Univ, Dept Astron, 610 Space Sci Bldg, Ithaca, NY 14853 USA. EM sloan@isc.astro.cornell.edu RI Kemper, Francisca/D-8688-2011 OI Kemper, Francisca/0000-0003-2743-8240 NR 55 TC 78 Z9 78 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2005 VL 632 IS 2 BP 956 EP 963 DI 10.1086/444371 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CO UT WOS:000232569100025 ER PT J AU Lee, CF Ho, PTP AF Lee, CF Ho, PTP TI Outflow and infall in star-forming region L1221 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (L1221); ISM : jets and outflows; stars : formation ID YOUNG STELLAR OBJECTS; MOLECULAR CLOUDS; CORES; PROTOSTAR; ENVELOPE; ACCRETION; EMISSION; COLLAPSE; LINE AB We have mapped the 3.3 mm continuum, CO, HCO+, N2H+, and CS emission around a nearby Class I source, IRAS 22266 + 6845, in the L1221 cometary dark cloud. L1221 is a complicated star-forming region. It hosts three infrared sources: a close binary consisting of an east source and a west source around the IRAS source position and a southeast source similar to 45" to the southeast (T. Bourke 2004, private communication). The east source is identified as the IRAS source. Continuum emission is seen around the east and southeast sources, probably tracing the dust around them. No continuum emission is seen toward the west source, probably indicating that there is not much dust there. An east-west molecular outflow is seen in CO, HCO+, and CS originated from around the binary. It is bipolar with an east lobe and a west lobe, both appearing as a wide-opening outflow shell originated from around the binary. It is likely powered by the east source, which shows a southeast extension along the outflow axis in the K' image. A ringlike envelope is seen in N2H+ around the binary surrounding the outflow waist. It is tilted with the major axis perpendicular to the outflow axis. The kinematics is well reproduced by a thin-disk model with both infall and rotation, and a column density peak in a ring. The ringlike envelope is not rotationally supported, as the rotation velocity is smaller than the infall velocity. C1 Harvard Smithsonian Ctr Astrophys, SMA, Hilo, HI 96720 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Harvard Smithsonian Ctr Astrophys, SMA, Cambridge, MA 02138 USA. RP Lee, CF (reprint author), Harvard Smithsonian Ctr Astrophys, SMA, 645,N Aohoku Pl, Hilo, HI 96720 USA. EM cflee@cfa.harvard.edu; ho@cfa.harvard.edu NR 29 TC 8 Z9 8 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 OCT 20 PY 2005 VL 632 IS 2 BP 964 EP 972 DI 10.1086/432657 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CO UT WOS:000232569100026 ER PT J AU Jorgensen, JK Bourke, TL Myers, PC Schoier, FL van Dishoeck, EF Wilner, DJ AF Jorgensen, JK Bourke, TL Myers, PC Schoier, FL van Dishoeck, EF Wilner, DJ TI Probing the inner 200 AU of low-mass protostars with the submillimeter array: Dust and organic molecules in NGC 1333 IRAS 2A SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : molecules; stars : formation; stars : individual ( NGC 1333 IRAS 2) ID PROTOSTELLAR ENVELOPES; IRAS 16293-2422; HOT CORE; PROTOPLANETARY DISKS; H2CO ABUNDANCE; STAR-FORMATION; T-TAURI; EVOLUTION; IRAS-16293-2422; EMISSION AB The Submillimeter Array has opened a new window to study the innermost warm and dense regions of the envelopes and disks around deeply embedded protostars. This paper presents high angular resolution (< 2") submillimeter observations of the Class 0 young stellar object NGC 1333 IRAS 2A. Dust continuum emission and lines of complex organic molecules such as CH3OCH3 and CH3OCHO, high-excitation CH3OH transitions, and deuterated methanol, CH3OD, as well as lines of CO, HCN, (HCN)-C-13, SO, and SO2, are detected on less than or similar to 200 AU scales. The observations are interpreted using detailed radiative transfer models of the physical and chemical structure, consistent with both single-dish and interferometer data. The continuum emission is explained by an extended envelope and a compact but resolved component, presumably a circumstellar disk with a diameter of 200 - 300 AU and amass of similar to a few times 0.01 - 0.1M(circle dot). If it is related to the rotation of the envelope, then the size of this disk suggests a centrifugal barrier of 200 - 300 AU, which implies that the temperature in the envelope does not increase above 100 K. Its large size also suggests that the buildup of disks proceeds rapidly throughout the early protostellar stages. The smaller (< 100 AU) disks found around other deeply embedded protostars may be a result of tidal truncation. The high-resolution observations of SO can be explained with a simple constant abundance, similar to 10(-9), constrained through single-dish observations, whereas those of (HCN)-C-13 and the organic species require high abundances, increased by 1 - 2 orders of magnitude, or an additional compact source of emission at small scales. The compact molecular emission could originate in a hot-core region of the inner envelope, but a more likely reservoir is the circumstellar disk. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stockholm Observ, AlbaNova, SE-10691 Stockholm, Sweden. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Jorgensen, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 42, Cambridge, MA 02138 USA. EM jjorgensen@cfa.harvard.edu RI Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 NR 47 TC 76 Z9 76 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 OCT 20 PY 2005 VL 632 IS 2 BP 973 EP 981 DI 10.1086/433181 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CO UT WOS:000232569100027 ER PT J AU Garcia, MR Williams, BF Yuan, F Kong, AKH Primini, FA Barmby, P Kaaret, P Murray, SS AF Garcia, MR Williams, BF Yuan, F Kong, AKH Primini, FA Barmby, P Kaaret, P Murray, SS TI A possible detection of M31* with Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : individual ( M31); galaxies : nuclei ID HUBBLE-SPACE-TELESCOPE; RAY POINT SOURCES; BLACK-HOLE; CENTRAL REGION; DOUBLE NUCLEUS; SAGITTARIUS-A; M31; ACCRETION; GALAXIES; STARS AB Two independent sets of Chandra and HST images of the nuclear region of M31 allow registration of X-ray and optical images to similar to 0."1. This registration shows that none of the bright (similar to 10(37) ergs s(-1)) X- ray sources near the nucleus is coincident with the central supermassive black hole, M31*. A 50 ks Chandra HRC image shows 2.5 sigma evidence for a faint (similar to 10(36) ergs s(-1)) discrete source that is consistent with the position of M31*. The Bondi radius of M31* is 0."9, making it one of the few supermassive black holes with a resolvable accretion flow. This large radius and the previous detections of diffuse X- ray-emitting gas in the nuclear region make M31* one of the most secure cases for a radiatively inefficient accretion flow and place some of the most severe constraints on the radiative processes in such a flow. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02138 USA. Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Garcia, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM garcia@head-cfa.harvard.edu; williams@head-cfa.harvard.edu; fyuan@physics.purdue.edu; akong@space.mit.edu; fap@head-cfa.harvard.edu; pbarmby@cfa.harvard.edu; philip-kaaret@uiowa.edu; ssm@head-cfa.harvard.edu RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Primini, Francis/0000-0002-6077-0643 NR 34 TC 19 Z9 19 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2005 VL 632 IS 2 BP 1042 EP 1047 DI 10.1086/432967 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CO UT WOS:000232569100033 ER PT J AU Williams, BF Garcia, MR McClintock, JE Primini, FA Murray, SS AF Williams, BF Garcia, MR McClintock, JE Primini, FA Murray, SS TI Chandra and HST study of a new transient X-ray source in M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; galaxies : individual ( M31); X-rays : binaries; X-rays : stars ID CANDIDATE XTE J1550-564; CENTRAL REGION; XMM-NEWTON; BINARIES; OUTBURST; CAMERA AB We present X-ray and optical observations of a new transient X-ray source in M31 first detected 2004 May 23 at R.A = 00(h)43(m)09(s) 940 +/- 0"65, decl. = 41 degrees 23'32."49 +/- 0".66. The X-ray light curve shows two peaks separated by several months, reminiscent of many Galactic X-ray novae. The location and X-ray spectrum of the source suggest it is a low-mass X-ray binary. Follow-up HST ACS observations of the location both during and after the outburst provide a high-confidence detection of variability for one star within the X-ray position error ellipse. This star has Delta B approximate to 1 mag, and there is only a approximate to 1% chance of finding such a variable in the error ellipse. We consider this star a good candidate for the optical counterpart of the X-ray source. The luminosity of this candidate provides a prediction for the orbital period of the system of 2.3-(+3.7)(1.2) days. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head.cfa.harvard.edu; garcia@head.cfa.harvard.edu; jem@head.cfa.harvard.edu; fap@head.cfa.harvard.edu; ssm@head.cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 NR 23 TC 8 Z9 8 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 OCT 20 PY 2005 VL 632 IS 2 BP 1086 EP 1092 DI 10.1086/444369 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CO UT WOS:000232569100039 ER PT J AU Gelbord, JM Marshall, HL Worrall, DM Birkinshaw, M Lovell, JEJ Ojha, R Godfrey, L Schwartz, DA Perlman, ES Georganopoulos, M Murphy, DW Jauncey, DL AF Gelbord, JM Marshall, HL Worrall, DM Birkinshaw, M Lovell, JEJ Ojha, R Godfrey, L Schwartz, DA Perlman, ES Georganopoulos, M Murphy, DW Jauncey, DL TI The knotty question of the jet of PKSB1421-490 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : individual (PKS B1421-490) ID BL LACERTAE OBJECTS; DIGITAL SKY SURVEY; X-RAY-EMISSION; CATALOG; SAMPLE; MULTIWAVELENGTH; M87 AB We report the discovery of unusually strong optical and X-ray emission associated with a knot in the radio jet of PKS B1421-490. The knot is the brightest feature observed beyond the radio band, with knot/core flux ratios similar to 300 and 3.7 at optical and X-ray frequencies, respectively. We interpret the extreme optical output of the knot as synchrotron emission. The nature of the X-ray emission is unclear. We consider a second synchrotron component, inverse Compton emission from a relativistic, decelerating jet, and the possibility that this feature is a chance superposition of an unusual BL Lac object. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Epping, NSW 2122, Australia. Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 72611, Australia. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gelbord, JM (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jonathan@space.mit.edu; hermanm@space.mit.edu; d.worrall@bristol.ac.uk; mark.birkinshaw@bristol.ac.uk; jim.lovell@csiro.au; roopesh.ojha@csiro.au; lgodfrey@mso.anu.edu.au; das@head-cfa.harvard.edu; perlman@jca.umbc.edu; markos@milkyway.gsfc.nasa.gov; dwm@sgra.jpl.nasa.gov; david.jauncey@csiro.au RI Godfrey, Leith/B-5283-2013 NR 28 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 OCT 20 PY 2005 VL 632 IS 2 BP L75 EP L78 DI 10.1086/497823 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CR UT WOS:000232569400005 ER PT J AU Kong, AKH Di Stefano, R AF Kong, AKH Di Stefano, R TI An unusual spectral state of an ultraluminous very soft X-ray source during outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : individual (M101); X-rays : binaries; X-rays : galaxies ID MASS BLACK-HOLES; EXTERNAL GALAXIES; WHITE-DWARF; M101; CHANDRA; POPULATION AB We report the results of Chandra and XMM-Newton observations of a new outburst of an ultraluminous X-ray source in M101. During a Chandra monitoring observation of M101, M101 ULX-1 was found to be in outburst in 2004 December, the second outburst in 2004. The peak bolometric luminosity is about 3 x 10(40) ergs s(-1) (7 x 10(39) ergs s(-1) in 0.3-7 keV). The outburst spectra are very soft and can generally be fitted with a blackbody model, with temperatures of 40-80 eV, similar to supersoft X-ray sources in the Milky Way and in the Magellanic Clouds. In one Chandra observation, the source spectrum appears to be harder with a temperature of 150 eV. Such a spectral state is rarely seen in M101 ULX-1, and no X-ray source in the Milky Way shows this kind of spectrum. However, such an unusual spectral state very likely belongs to a new class of X-ray sources, quasi-soft X-ray sources, recently discovered in nearby galaxies. M101 ULX-1 returned to supersoft state in a subsequent XMM-Newton observation. Based on the two outbursts in 2004, the extremely high luminosity (L-bo1 = 10(40)-10(41) ergs s(-1)), very soft 40 L p 10 X-ray spectra (kT = 40-150 eV), transient behavior, and state transition provide strong evidence that M101 ULX-1 harbors an intermediate- mass black hole. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Kong, AKH (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM akong@space.mit.edu; rd@cfa.harvard.edu NR 22 TC 30 Z9 30 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 OCT 20 PY 2005 VL 632 IS 2 BP L107 EP L110 DI 10.1086/498020 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CR UT WOS:000232569400013 ER PT J AU Stanimirovic, S Bolatto, AD Sandstrom, K Leroy, AK Simon, JD Gaensler, BM Shah, RY Jackson, JM AF Stanimirovic, S Bolatto, AD Sandstrom, K Leroy, AK Simon, JD Gaensler, BM Shah, RY Jackson, JM TI Spitzer space telescope detection of the young supernova remnant 1E 0102.2-7219 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : individual (1E 0102.2-7219); Magellanic Clouds ID SMALL-MAGELLANIC-CLOUD; CASSIOPEIA-A; DUST; SPECTROSCOPY AB We present infrared observations of the young, oxygen-rich supernova remnant 1E 0102.2 - 7219 (E0102) in the Small Magellanic Cloud, obtained with the Spitzer Space Telescope. The remnant is detected at 24 mu m but not at 8 or 70 mu m and has a filled morphology with two prominent filaments. We find evidence for the existence of up to 8 x 10(-4) M circle dot of hot dust (T-d similar to 120 K) associated with the remnant. Most of the hot dust is located in the central region of E0102, which appears significantly enhanced in infrared and radio continuum emission relative to the X-ray emission. Even if all of the hot dust was formed in the explosion of E0102, the estimated mass of dust is at least 100 times lower than what is predicted by some recent theoretical models. C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. RP Stanimirovic, S (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. EM sstanimi@astro.berkeley.edu; bolatto@astro.berkeley.edu; karin@astro.berkeley.edu; aleroy@astro.berkeley.edu; jsimon@astro.berkeley.edu; bgaensler@cfa.harvard.edu; ronak@bu.edu; jackson@bu.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 20 TC 17 Z9 17 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2005 VL 632 IS 2 BP L103 EP L106 DI 10.1086/497985 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CR UT WOS:000232569400012 ER PT J AU Wu, H Cao, C Hao, CN Liu, FS Wang, JL Xia, XY Deng, ZG Young, CKS AF Wu, H Cao, C Hao, CN Liu, FS Wang, JL Xia, XY Deng, ZG Young, CKS TI PAH and mid-infrared luminosities as measures of star formation rate in Spitzer first look survey galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : starburst; infrared : galaxies; stars : formation ID DIGITAL SKY SURVEY; ARRAY CAMERA IRAC; FORMING GALAXIES; SPACE-TELESCOPE; 1ST-LOOK SURVEY; EMISSION; SPECTRA; DUST; ISOCAM; SAMPLE AB We present evidence that the 8 mm (dust) and 24 mm luminosities of star-forming galaxies are both strongly correlated with their 1.4 GHz and H alpha luminosities over a range in luminosity of 2-3 orders of magnitude. At the bright end, the correlations are found to be essentially linear over a luminosity range of about 2 orders of magnitude (corresponding to star formation rates of several tenths to several tens of solar masses per year). However, at the faint end there appears to be a slope change for dwarf galaxies, possibly due to the lower dust-to-gas ratios and lower metallicities of the dwarfs. The correlations suggest that PAH features and mid-IR continuum emissions are good measures of the star formation rates of galaxies, and we present calibrations of star formation rates based on existing radio and Ha relations. Our findings are based on a sample of star-forming galaxies selected from the main field of the Spitzer First Look Survey with the aid of spectroscopic data from the Sloan Digital Sky Survey and VLA 1.4 GHz data. C1 Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Tianjin Normal Univ, Dept Phys, Tianjin 300074, Peoples R China. Chinese Acad Sci, Grad Sch, Coll Phys Sci, Beijing 100039, Peoples R China. Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hwu@bao.ac.cn NR 41 TC 139 Z9 139 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 OCT 20 PY 2005 VL 632 IS 2 BP L79 EP L82 DI 10.1086/497961 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974CR UT WOS:000232569400006 ER PT J AU O'Sullivan, DW Neale, PJ Coffin, RB Boyd, TJ Osburn, SL AF O'Sullivan, DW Neale, PJ Coffin, RB Boyd, TJ Osburn, SL TI Photochemical production of hydrogen peroxide and methylhydroperoxide in coastal waters SO MARINE CHEMISTRY LA English DT Article DE hydrogen peroxide; organic peroxides; photochemistry; seawater ID DISSOLVED ORGANIC-MATTER; ULTRAVIOLET-RADIATION; SURFACE WATERS; NATURAL-WATERS; SOUTH FLORIDA; ORINOCO RIVER; CARBON; TROPOSPHERE; SEAWATER; ACID AB Hydrogen peroxide (H2O2) has been observed in significant concentrations in many natural waters. Because hydrogen peroxide can act as an oxidant and reductant, it participates in an extensive suite of reactions in surface waters. Hydrogen peroxide is produced as a secondary photochemical product of chromophoric dissolved organic matter (CDOM) photolysis. Apparent quantum yields for the photochemical production of hydrogen peroxide were determined in laboratory irradiations of filtered surface waters from several locations in the Chesapeake Bay and in Arctic coastal waters with varying levels of CDOM. The apparent quantum yield for H2O2 decreases by about an order of magnitude from 280 nm to 500 nm, and the majority of H2O2 production occurs at wavelengths less than 340 nm. The apparent quantum yield for H2O2 production at 290 nm ranged from 4.2 x 10(-4) to 2.1 X 10(-6) mol H2O2 (mol photons)(-1) from freshwater to marine waters. A linear relationship was found between the production of H2O2 and change in CDOM absorbance characterized as photobleaching (loss of absorbance). No significant relationship was observed between DOC concentration and peroxide production. Methylhydroperoxide (CH3O2H) was the only short chain peroxide produced during the irradiations, and its production is at least an order magnitude less than that of hydrogen peroxide. Peroxide production was greatest in waters containing significant amounts of terrigenous C in the form of humic substances. Surface waters whose synchronous fluorescence spectra indicated the presence of polyaromatic and/ or extensive conjugated compounds exhibited the greatest peroxide production. CDOM photobleaching is not significantly linked to apparent quantum yields for peroxide production. (c) 2005 Published by Elsevier B.V. C1 USN Acad, Dept Chem, Annapolis, MD 21402 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. USN, Res Lab, Marine Biogeochem Sect, Washington, DC 20375 USA. RP O'Sullivan, DW (reprint author), USN Acad, Dept Chem, 572 Holloway Rd, Annapolis, MD 21402 USA. EM osullivan@usna.edu RI Neale, Patrick/A-3683-2012; OI O'Sullivan, Daniel/0000-0001-9104-5703; Osburn, Christopher/0000-0002-9334-4202 NR 50 TC 52 Z9 56 U1 2 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-4203 J9 MAR CHEM JI Mar. Chem. PD OCT 20 PY 2005 VL 97 IS 1-2 BP 14 EP 33 DI 10.1016/j.marchem.2005.04.003 PG 20 WC Chemistry, Multidisciplinary; Oceanography SC Chemistry; Oceanography GA 978ZP UT WOS:000232912100003 ER PT J AU Riley, S AF Riley, S TI The secret lives of fortunate wives. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst Libs, 1000 Jefferson Dr SW, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 2005 VL 130 IS 17 BP 48 EP 49 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 041XO UT WOS:000237490200044 ER PT J AU Schroll, S AF Schroll, S TI Shag: The art of Josh Agle. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 2005 VL 130 IS 17 BP 53 EP 53 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 041XO UT WOS:000237490200069 ER PT J AU Hutchinson, A AF Hutchinson, A TI Venomous snakes of the world. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 2005 VL 130 IS 17 BP 77 EP 77 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 041XO UT WOS:000237490200194 ER PT J AU Laurance, W AF Laurance, W TI Razing Amazonia SO NEW SCIENTIST LA English DT Article AB Despite decades of campaigning by conservationists, the Amazon is being destroyed more rapidly than ever. C1 Smithsonian Trop Res Inst, Balboa, Panama. Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. RP Laurance, W (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 0 TC 1 Z9 1 U1 0 U2 0 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD OCT 15 PY 2005 VL 188 IS 2521 BP 34 EP 39 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 974YQ UT WOS:000232627700041 ER PT J AU Harrington, GJ Clechenko, ER Kelly, DC AF Harrington, GJ Clechenko, ER Kelly, DC TI Palynology and organic-carbon isotope ratios across a terrestrial Palaeocene/Eocene boundary section in the Williston Basin, North Dakota, USA SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Palaeocene-Eocene Thermal Maximum; organic carbon isotopes; palynology; North Dakota; Golden Valley Formation; Fort Union Formation ID PALEOCENE THERMAL MAXIMUM; GOLDEN VALLEY FORMATION; BIGHORN BASIN; EARLY EOCENE; METHANE HYDRATE; OXYGEN-ISOTOPE; CLIMATE-CHANGE; GAS HYDRATE; AMERICA; DISSOCIATION AB The Palaeocene-Eocene Thermal Maximum (PETM) at 55 Ma marks the Palaeocene/Eocene (P/E) boundary and represents a discrete period of abrupt, transient global warming. There are few vegetation records from within the PETM and such an absence of data prevents modelling of the vegetation response to climate warming. Outcrops exposing the Sentinel Butte member (upper Fort Union Formation) and the Golden Valley Formation (Bear Den and lower Camels Butte members) within the Williston Basin of western North Dakota, USA are known to span the P/E boundary. Pollen and spore floras at the Farmers Butte locality (Stark County, North Dakota; 46.92 degrees N 102.11 degrees W) record changes in abundance of some reed, fern and understorey plants across the Sentinel Butte-Bear Den contact but no other composition changes occur until the arrival of Eocene immigrants Platycarya spp. (walnut/pecan family) and Intratriporopollenites instructus (linden/sterculia/cotton tree families) at the top of the Bear Den member, c. 11 m above the change in co-occurrence and relative abundance patterns of range-through taxa. The exact stratigraphic level at which these Eocene marker taxa first occur is unclear owing to the heavily weathered nature of Bear Den strata below the Alamo Bluff lignite. This pattern of stratigraphic change may be correlative to the well documented "floral gap" of PETM records in Wyoming. Though bulk delta(13)C(org) ratios decrease by 2.4 parts per thousand across the Alamo Bluff lignite, degradation of organic carbon within the upper Bear Den member partially masks full expression of the carbon isotope excursion associated with the PETM. Hence, strata around the Alamo Bluff lignite may represent a new terrestrial record of the PETM. In agreement with terrestrial PETM records from other U.S. western interior localities, palynological data indicate no floral extinction and little composition change across the Palaeocene/Eocene boundary. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. RP Harrington, GJ (reprint author), Univ Birmingham, Sch Geog Earth & Environm Sci, Aston Webb Bldg, Birmingham B15 2TT, W Midlands, England. EM g.j.harrington@bham.ac.uk NR 76 TC 17 Z9 19 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD OCT 14 PY 2005 VL 226 IS 3-4 BP 214 EP 232 DI 10.1016/j.paleco.2005.05.013 PG 19 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 973MN UT WOS:000232527000003 ER PT J AU Meech, KJ Ageorges, N A'Hearn, MF Arpigny, C Ates, A Aycock, J Bagnulo, S Bailey, J Barber, R Barrera, L Barrena, R Bauer, JM Belton, MJS Bensch, F Bhattacharya, B Biver, N Blake, G Bocklee-Morvan, D Boehnhardt, H Bonev, BP Bonev, T Buie, MW Burton, MG Butner, HM Cabanac, R Campbell, R Campins, H Capria, MT Carroll, T Chaffee, F Charnley, SB Cleis, R Coates, A Cochran, A Colom, P Conrad, A Coulson, IM Crovisier, J deBuizer, J Dekany, R de Leon, J Dello Russo, N Delsanti, A DiSanti, M Drummond, J Dundon, L Etzel, PB Farnham, TL Feldman, P Fernandez, YR Filipovic, MD Fisher, S Fitzsimmons, A Fong, D Fugate, R Fujiwara, H Fujiyoshi, T Furusho, R Fuse, T Gibb, E Groussin, O Gulkis, S Gurwell, M Hadamcik, H Hainaut, O Harker, D Harrington, D Harwit, M Hasegawa, S Hergenrother, CW Hirst, P Hodapp, K Honda, M Howell, ES Hutsemekers, D Iono, D Ip, WH Jackson, W Jehin, E Jiang, ZJ Jones, GH Jones, PA Kadono, T Kamath, UW Kaufl, HU Kasuga, T Kawakita, H Kelley, MS Kerber, F Kidger, M Kinoshita, D Knight, M Lara, L Larson, SM Lederer, S Lee, CF Levasseur-Regourd, AC Li, JY Li, QS Licandro, J Lin, ZY Lisse, CM LoCurto, G Lovell, AJ Lowry, SC Lyke, J Lynch, D Ma, J Magee-Sauer, K Maheswar, G Manfroid, J Marco, O Martin, P Melnick, G Miller, S Miyata, T Moriarty-Schieven, GH Moskovitz, N Mueller, BEA Mumma, MJ Muneer, S Neufeld, DA Ootsubo, T Osip, D Pandea, SK Pantin, E Paterno-Mahler, R Patten, B Penprase, BE Peck, A Petitas, G Pinilla-Alonso, N Pittichova, J Pompei, E Prabhu, TP Qi, C Rao, R Rauer, H Reitsema, H Rodgers, SD Rodriguez, P Ruane, R Ruch, G Rujopakarn, W Sahu, DK Sako, S Sakon, I Samarasinha, N Sarkissian, JM Saviane, I Schirmer, M Schultz, P Schulz, R Seitzer, P Sekiguchi, T Selman, F Serra-Ricart, M Sharp, R Snell, RL Snodgrass, C Stallard, T Stecklein, G Sterken, C Stuwe, JA Sugita, S Sumner, M Suntzeff, N Swaters, R Takakuwa, S Takata, N Thomas-Osip, J Thompson, E Tokunaga, AT Tozzi, GP Tran, H Troy, M Trujillo, C Van Cleve, J Vasundhara, R Vazquez, R Vilas, F Villanueva, G von Braun, K Vora, P Wainscoat, RJ Walsh, K Watanabe, J Weaver, HA Weaver, W Weiler, M Weissman, PR Welsh, WF Wilner, D Wolk, S Womack, M Wooden, D Woodney, LM Woodward, C Wu, ZY Wu, JH Yamashita, T Yang, B Yang, YB Yokogawa, S Zook, AC Zauderer, A Zhao, X Zhou, X Zucconi, JM AF Meech, KJ Ageorges, N A'Hearn, MF Arpigny, C Ates, A Aycock, J Bagnulo, S Bailey, J Barber, R Barrera, L Barrena, R Bauer, JM Belton, MJS Bensch, F Bhattacharya, B Biver, N Blake, G Bocklee-Morvan, D Boehnhardt, H Bonev, BP Bonev, T Buie, MW Burton, MG Butner, HM Cabanac, R Campbell, R Campins, H Capria, MT Carroll, T Chaffee, F Charnley, SB Cleis, R Coates, A Cochran, A Colom, P Conrad, A Coulson, IM Crovisier, J deBuizer, J Dekany, R de Leon, J Dello Russo, N Delsanti, A DiSanti, M Drummond, J Dundon, L Etzel, PB Farnham, TL Feldman, P Fernandez, YR Filipovic, MD Fisher, S Fitzsimmons, A Fong, D Fugate, R Fujiwara, H Fujiyoshi, T Furusho, R Fuse, T Gibb, E Groussin, O Gulkis, S Gurwell, M Hadamcik, H Hainaut, O Harker, D Harrington, D Harwit, M Hasegawa, S Hergenrother, CW Hirst, P Hodapp, K Honda, M Howell, ES Hutsemekers, D Iono, D Ip, WH Jackson, W Jehin, E Jiang, ZJ Jones, GH Jones, PA Kadono, T Kamath, UW Kaufl, HU Kasuga, T Kawakita, H Kelley, MS Kerber, F Kidger, M Kinoshita, D Knight, M Lara, L Larson, SM Lederer, S Lee, CF Levasseur-Regourd, AC Li, JY Li, QS Licandro, J Lin, ZY Lisse, CM LoCurto, G Lovell, AJ Lowry, SC Lyke, J Lynch, D Ma, J Magee-Sauer, K Maheswar, G Manfroid, J Marco, O Martin, P Melnick, G Miller, S Miyata, T Moriarty-Schieven, GH Moskovitz, N Mueller, BEA Mumma, MJ Muneer, S Neufeld, DA Ootsubo, T Osip, D Pandea, SK Pantin, E Paterno-Mahler, R Patten, B Penprase, BE Peck, A Petitas, G Pinilla-Alonso, N Pittichova, J Pompei, E Prabhu, TP Qi, C Rao, R Rauer, H Reitsema, H Rodgers, SD Rodriguez, P Ruane, R Ruch, G Rujopakarn, W Sahu, DK Sako, S Sakon, I Samarasinha, N Sarkissian, JM Saviane, I Schirmer, M Schultz, P Schulz, R Seitzer, P Sekiguchi, T Selman, F Serra-Ricart, M Sharp, R Snell, RL Snodgrass, C Stallard, T Stecklein, G Sterken, C Stuwe, JA Sugita, S Sumner, M Suntzeff, N Swaters, R Takakuwa, S Takata, N Thomas-Osip, J Thompson, E Tokunaga, AT Tozzi, GP Tran, H Troy, M Trujillo, C Van Cleve, J Vasundhara, R Vazquez, R Vilas, F Villanueva, G von Braun, K Vora, P Wainscoat, RJ Walsh, K Watanabe, J Weaver, HA Weaver, W Weiler, M Weissman, PR Welsh, WF Wilner, D Wolk, S Womack, M Wooden, D Woodney, LM Woodward, C Wu, ZY Wu, JH Yamashita, T Yang, B Yang, YB Yokogawa, S Zook, AC Zauderer, A Zhao, X Zhou, X Zucconi, JM TI Deep Impact: Observations from a worldwide Earth-based campaign SO SCIENCE LA English DT Article ID COMET-9P/TEMPEL-1; 9P/TEMPEL-1 AB On 4 July 2005, many observatories around the world and in space observed the collision of Deep Impact with comet 9P/Tempet 1 or its aftermath. This was an unprecedented coordinated observational campaign. These data show that (i) there was new material after impact that was compositionally different from that seen before impact; (ii) the ratio of dust mass to gas mass in the ejecta was much larger than before impact; (iii) the new activity did not last more than a few days, and by 9 July the comet's behavior was indistinguishable from its pre-impact behavior; and (iv) there were interesting transient phenomena that may be correlated with cratering physics. C1 Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. European So Observ, Santiago 19, Chile. Univ Maryland, College Pk, MD 20742 USA. Univ Liege, B-4000 Liege, Belgium. Pomona Coll, Claremont, CA 91711 USA. Keck Observ, Kamuela, HI 96743 USA. Macquarie Univ, Australian Ctr Astrobiol, Sydney, NSW 2109, Australia. UCL, London WC1E 6BT, England. Univ Metropolitana Ciencias Educ, Santiago, Chile. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. Belton Space Initiat, Tucson, AZ 85716 USA. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. CALTECH, Pasadena, CA 91125 USA. Observ Paris, F-92195 Meudon, France. Max Planck Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. Univ Toledo, Toledo, OH 43606 USA. Inst Astron, Sofia 1784, Bulgaria. Lowell Observ, Flagstaff, AZ 86001 USA. Univ New S Wales, Sydney, NSW 2052, Australia. Joint Astron Ctr, Hilo, HI 96720 USA. Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. Univ Cent Florida, Orlando, FL 32816 USA. Inst Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. USAF, Res Lab, Kirtland AFB, NM 87117 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Texas, Austin, TX 78712 USA. Gemini Observ, Serena, Chile. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. San Diego State Univ, San Diego, CA 92182 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Univ Western Sydney, Sydney, NSW 1797, Australia. Gemini Observ N, Hilo, HI 96720 USA. Queens Univ Belfast, Belfast BT7 1NN, Antrim, North Ireland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Tokyo 1138654, Japan. Subaru Telescope, Hilo, HI 96720 USA. Waseda Univ, Tokyo 1698050, Japan. Univ Notre Dame, Notre Dame, IN 46556 USA. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. Univ Calif San Diego, La Jolla, CA 92093 USA. Cornell Univ, Ithaca, NY 14853 USA. Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. Univ Arizona, Tucson, AZ 85721 USA. Arecibo Observ, Arecibo, PR 00612 USA. Natl Cent Univ, Tao Yuan 32001, Taiwan. Univ Calif Davis, Davis, CA 95616 USA. Natl Astron Observ, Beijing 100012, Peoples R China. Australian Telescope, Natl Facil, Epping, NSW 1710, Australia. Japan Agcy Marine Earth Sci & Technol, Kanagawa 2370061, Japan. Indian Inst Astrophys, Bangalore 560034, Karnataka, India. Natl Astron Observ Japan, Tokyo 1818588, Japan. Kyoto Sangyo Univ, Kyoto 6038555, Japan. Univ Minnesota, Minneapolis, MN 55455 USA. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Calif State Univ San Bernardino, San Bernardino, CA 92407 USA. Isaac Newton Grp Telescopes, E-38700 La Palma, Spain. Agnes Scott Coll, Decatur, GA 30030 USA. Aerosp Corp, Los Angeles, CA 90009 USA. Rowan Univ, Glassboro, NJ 08028 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Nagoya Univ, Nagoya, Aichi 4648601, Japan. Las Campanas Observ, Pasadena, CA 91101 USA. CEA, Serv Astron, F-91191 Gif Sur Yvette, France. Fdn Galileo Galilei & Telescopio Nazl Galileo, La Palma 38700, Spain. Deutsch Zentrum Luft & Raumfahrt, D-12489 Berlin, Germany. Ball Aerosp, Boulder, CO 80306 USA. European Space Agcy, Madrid 28080, Spain. Univ Michigan, Ann Arbor, MI 48109 USA. Brown Univ, Providence, RI 02912 USA. European Space Agcy, NL-2200 AG Noordwijk, Netherlands. Anglo Australian Observ, Epping, NSW 1710, Australia. Univ Massachusetts, Amherst, MA 01003 USA. Univ Brussels, B-1050 Brussels, Belgium. Leiden Observ, NL-2300 RA Leiden, Netherlands. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Nacl Autonoma Mexico, Ensenada 22800, Baja California, Mexico. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Carnegie Inst Sci, Washington, DC 20015 USA. Coll William & Mary, Williamsburg, VA 23187 USA. St Cloud State Univ, St Cloud, MN 56301 USA. Observ Besancon, F-25010 Besancon, France. RP Meech, KJ (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM meech@ifa.hawaii.edu RI Pinilla-Alonso, Noemi/B-8583-2008; Charnley, Steven/C-9538-2012; Lisse, Carey/B-7772-2016; Vazquez, Roberto/L-3613-2016; Rujopakarn, Wiphu/E-7849-2012; Coates, Andrew/C-2396-2008; mumma, michael/I-2764-2013; Jones, Geraint/C-1682-2008; de Leon, Julia/H-7569-2015; Magee-Sauer, Karen/K-6061-2015; Dello Russo, Neil/G-2727-2015; Weaver, Harold/D-9188-2016 OI Snodgrass, Colin/0000-0001-9328-2905; Jones, Geraint/0000-0002-5859-1136; Lisse, Carey/0000-0002-9548-1526; Vazquez, Roberto/0000-0002-3279-9764; Coates, Andrew/0000-0002-6185-3125; de Leon, Julia/0000-0002-0696-0411; Magee-Sauer, Karen/0000-0002-4979-9875; Dello Russo, Neil/0000-0002-8379-7304; NR 15 TC 130 Z9 131 U1 2 U2 32 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 OCT 14 PY 2005 VL 310 IS 5746 BP 265 EP 269 DI 10.1126/science.1118978 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 975NV UT WOS:000232670100038 PM 16150977 ER PT J AU Duarte, M Robbins, RK Mielke, OHH AF Duarte, M Robbins, RK Mielke, OHH TI Immature stages of Calycopis caulonia (Hewitson, 1877) (Lepidoptera, Lycaenidae, Theclinae, Eumaeini), with notes on rearing detritivorous hairstreaks on artificial diet SO ZOOTAXA LA English DT Article DE Lycaenidae; Theclinae; Eumaeini; Calycopis; systematics; life history; biology; detritivory; myrmecophily; artificial diet; rearing ID EVOLUTION AB Details of egg, larval, and pupal morphology are described and illustrated for Calycopis caulonia (Hewitson). In particular, larval chaetotaxy is documented for the first time in Calycopis. Lab methods for inducing wild-caught Calycopis females to lay eggs and for rearing larvae on artificial diet are reported. These methods may be useful in several ways in resolving the basic taxonomy of Calycopis. Evidence concerning detritivory and myrmecophily in C. caulonia is discussed. C1 Univ Sao Paulo, Museu Zool, BR-04263000 Sao Paulo, Brazil. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil. RP Duarte, M (reprint author), Univ Sao Paulo, Museu Zool, Ave Nazare 481, BR-04263000 Sao Paulo, Brazil. EM lycaenidae@ig.com.br; robbinsr@si.edu; omhesp@ufpr.br RI Mielke, Olaf/C-4986-2013; Duarte, Marcelo/K-7633-2012 OI Mielke, Olaf/0000-0003-3655-4606; NR 62 TC 41 Z9 48 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 OCT 14 PY 2005 IS 1063 BP 1 EP 31 PG 31 WC Zoology SC Zoology GA 973RL UT WOS:000232540200001 ER PT J AU Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Robertson, B Springel, V AF Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Robertson, B Springel, V TI Luminosity-dependent quasar lifetimes: Reconciling the optical and X-ray quasar luminosity function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : active; galaxies : evolution; galaxies : nuclei; quasars : general ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; PARTICLE HYDRODYNAMICS SIMULATIONS; REGION NEARBY SURVEY; RADIO-QUIET QUASARS; QSO REDSHIFT SURVEY; INFALL REGION; DARK-MATTER; COSMOLOGICAL SIMULATIONS AB We consider implications of our new model of quasar lifetimes and light curves for the quasar luminosity function (LF) at different frequencies and redshifts. In our picture, quasars evolve rapidly and the lifetime depends on both their instantaneous and peak luminosities. The bright end of the LF traces the peak intrinsic quasar activity, but the faint end consists of quasars that are either undergoing exponential growth to much larger masses and luminosities or are in sub-Eddington quiescent states going into or coming out of a period of peak activity. The "break'' in the observed LF corresponds directly to the maximum in the intrinsic distribution of peak luminosities, which falls off at both brighter and fainter luminosities. We study this model using simulations of galaxy mergers that successfully reproduce a wide range of observed quasar phenomena, including the observed column density distribution. By combining quasar lifetimes and the distribution of maximum quasar luminosities determined from the observed hard X-ray LF with the corresponding luminosity and host system-dependent column densities, we produce the expected soft X-ray and B-band LFs. Our predictions agree exceptionally well with the observed LFs at all observed luminosities over the redshift range considered ( z <= 1) without invoking any ad hoc assumptions about an obscured population of sources. Our results also suggest that observed correlations in hard X-ray samples between the obscured fraction of quasars and luminosity can be explained in the context of our model by the expulsion of surrounding gas due to heating from accretion feedback energy as a quasar nears its peak luminosity and final black hole mass. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 79 TC 61 Z9 62 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 OCT 10 PY 2005 VL 632 IS 1 BP 81 EP 91 DI 10.1086/432755 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EZ UT WOS:000232366000006 ER PT J AU Siemiginowska, A Cheung, CC LaMassa, S Burke, DJ Aldcroft, TL Bechtold, J Elvis, M Worrall, DM AF Siemiginowska, A Cheung, CC LaMassa, S Burke, DJ Aldcroft, TL Bechtold, J Elvis, M Worrall, DM TI X-ray cluster associated with the z=1.063 CSS quasar 3C 186: The jet is not frustrated SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : individual (3C 186); X-rays : galaxies : clusters ID COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; EXTRAGALACTIC RADIO-SOURCES; DEEP CHANDRA OBSERVATION; HIGH-REDSHIFT QUASARS; XMM-NEWTON; INTRACLUSTER MEDIUM; PARAMETER-ESTIMATION; SYMMETRICAL OBJECTS AB We report the Chandra discovery of an X-ray cluster at redshift z = 1.063 associated with the compact steep spectrum (CSS) radio- loud quasar 3C 186 (Q0740 + 380). Diffuse X-ray emission is detected out to similar to 120 kpc from the quasar and contains 741 +/- 40 net counts. The X-ray spectrum of the extended emission shows strong Fe-line emission (EW = 412 eV) at the quasar redshift and confirms the thermal nature of this diffuse component. We measure a cluster temperature of 5.2(-0.9)(+1.2) keV and an X-ray luminosity L-X(0.5-2 keV) similar to 6 x 10(44) ergs s(-1), which are in agreement with the luminosity-temperature relation for high-redshift clusters. This is the first detection of a bright X-ray cluster around a luminous (L-bol similar to 10(47) ergs s(-1)) CSS quasar at high redshift and is only the fifth z > 1 X-ray cluster detected. We find that the CSS radio source is highly overpressured with respect to the thermal cluster medium by about 3 orders of magnitude. This provides direct observational evidence that the radio source is not thermally confined as posited in the ''frustrated'' scenario for CSS sources. Instead, it appears that the radio source may be young and we are observing it at an early stage of its evolution. In that case the radio source could supply the energy into the cluster and potentially prevent its cooling. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asiemiginowska@cfa.harvard.edu; ccheung@space.mit.edu OI Burke, Douglas/0000-0003-4428-7835 NR 90 TC 31 Z9 31 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2005 VL 632 IS 1 BP 110 EP 121 DI 10.1086/432871 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EZ UT WOS:000232366000008 ER PT J AU Kim, WT El-Zant, AA Kamionkowski, M AF Kim, WT El-Zant, AA Kamionkowski, M TI Dynamical friction and cooling flows in galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : interactions; galaxies : kinematics and dynamics; instabilities; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; THERMAL CONDUCTION; TEMPERATURE PROFILES; INTRACLUSTER MEDIUM; MAGNETIC-FIELDS; DENSITY PROFILE; NEARBY CLUSTERS; GASEOUS MEDIUM; XMM-NEWTON; GAS AB We investigate a model of galaxy clusters in which the hot intracluster gas is efficiently heated by dynamical friction (DF) of galaxies. We allow for both subsonic and supersonic motions of galaxies and use the gravitational drag formula in a gaseous medium presented by Ostriker. The energy lost by the galaxies is either redistributed locally or into a Gaussian centered on the galaxy. We find that the condition of hydrostatic equilibrium and strict energy balance yields a trivial isothermal solution T-iso, independent of radius, or rising temperature distributions, provided T-iso/gamma < T < T-iso, where gamma is the adiabatic index of the gas. The isothermal temperature corresponds to the usual scaling relation between the gas temperatures and the velocity dispersions of galaxies. However, the minimal temperature associated with the rising solutions is similar to 1/2 T-vir, larger than that inferred from observations, the radial distribution of galaxy masses notwithstanding. Heating by supersonically moving galaxies cannot suppress thermal instability, although it can lengthen the growth time up to the level comparable to the ages of clusters when the Mach number of galaxies is less than about 2. We show using numerical hydrodynamic simulations that DF-induced heating is generally unable to produce stable equilibrium cores by evolving arbitrary nonequilibrium clusters, although it can lengthen the cooling time. We conclude that DF-induced heating alone is an unlikely solution to the cooling flow problem, although it can still be an important heat supplier, considerably delaying the cooling catastrophe. We discuss other potential consequences of DF of galaxies in galaxy clusters. C1 Seoul Natl Univ, Astron Program, Sch Earth & Environm Sci, Seoul 151742, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. CALTECH, Pasadena, CA 91125 USA. RP Kim, WT (reprint author), Seoul Natl Univ, Astron Program, Sch Earth & Environm Sci, Seoul 151742, South Korea. EM wkim@astro.snu.ac.kr NR 82 TC 36 Z9 36 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 OCT 10 PY 2005 VL 632 IS 1 BP 157 EP 168 DI 10.1086/432976 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EZ UT WOS:000232366000011 ER PT J AU Beuther, H Zhang, Q Greenhill, LJ Reid, MJ Wilner, D Keto, E Shinnaga, H Ho, PTP Moran, JM Liu, SY Chang, CM AF Beuther, H Zhang, Q Greenhill, LJ Reid, MJ Wilner, D Keto, E Shinnaga, H Ho, PTP Moran, JM Liu, SY Chang, CM TI Line imaging of Orion KL at 865 mu m with the submillimeter array SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Orion KL); ISM : lines and bands; ISM : molecules; stars : formation; submillimeter; techniques : interferometric ID MOLECULAR CLOUD CORES; STAR-FORMING REGION; INTERSTELLAR GLYCINE; APERTURE SYNTHESIS; HOT CORE; EMISSION; BN/KL; IRC2; GHZ; MILLIMETER AB We present the first submillimeter (865 mu m) imaging spectral line survey at 1 '' resolution conducted with the Sub-millimeter Array toward Orion KL. Within the 2 x 2 GHz bandpasses ( lower and upper sidebands, 337.2 - 339.2 and 347.2 - 349.2 GHz), we find about 145 spectral lines from 13 species, six isotopologues, and five vibrational excited states. Most nitrogen-bearing molecules are strong toward the hot core, whereas the oxygen-bearing molecules peak toward the southwest in the so-called compact ridge. Imaging of spectral lines is shown to be an additional tool to improve the identifications of molecular lines. Arcsecond spatial resolution allows us to distinguish the molecular line emission of the sources I and n from that of the hot core. The only molecular species detected strongly toward source I is SiO, delineating mainly the collimated northeast- southwest low- velocity outflow. The two positions close to source I, which have previously been reported to show maser emission in the v = 0 (28)SiO (1 - 0) and (2 - 1) lines, show no detectable maser emission in the v =0 (28)SiO (8 - 7) line at our spatial resolution. SiO is weak toward source n, and thus source n may not currently be driving a molecular outflow. CH(3)OH is the molecule with the highest number of identified lines (46) in this spectral window. This ''line forest'' allows us to estimate temperatures in the region, and we find temperatures between 50 and 350 K, with the peak temperatures occurring toward the hot core. The detection of strong vibrational excited line emission from the submillimeter continuum peak SMA1 supports the interpretation that the source SMA1 is likely of protostellar nature. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Sect 4, Taipei 106, Taiwan. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu NR 43 TC 70 Z9 70 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2005 VL 632 IS 1 BP 355 EP 370 DI 10.1086/432974 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EZ UT WOS:000232366000026 ER PT J AU Gutermuth, RA Megeath, ST Pipher, JL Williams, JP Allen, LE Myers, PC Raines, SN AF Gutermuth, RA Megeath, ST Pipher, JL Williams, JP Allen, LE Myers, PC Raines, SN TI The initial configuration of young stellar clusters: A k-band number counts analysis of the surface density of stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; open clusters and associations : individual (GGD 12-; 15,IRAS 20050+2720,NGC 7129); stars : formation; stars : pre-main-sequence ID HERBIG-HARO OBJECTS; MOLECULAR CLOUDS; MONOCEROS R2; MULTIPOLAR OUTFLOW; TRAPEZIUM CLUSTER; DISC ENCOUNTERS; RADIO-SOURCES; 1 KILOPARSEC; NGC-7129; PROTOSTARS AB We present an analysis of stellar distributions for the young stellar clusters GGD 12-15, IRAS 20050+2720, and NGC 7129, which range in far-IR luminosity from 227 to 5.68x10(3) L circle dot and are all still associated with their natal molecular clouds. The data used for this analysis include near-IR data obtained with FLAMINGOS on the MMT and newly obtained wide-field 850 mu m emission maps from SCUBA on the JCMT. Cluster size and azimuthal asymmetry are measured via azimuthal and radial averaging methods, respectively. To quantify the deviation of the distribution of stars from circular symmetry, we define an azimuthal asymmetry parameter, and we investigate the statistical properties of this parameter through Monte Carlo simulations. The distribution of young stars is compared to the morphology of the molecular gas using stellar surface density maps and the 850 mu m maps. We find that two of the clusters are not azimuthally symmetric and show a high degree of structure. The GGD 12-15 cluster is elongated and is aligned with newly detected filamentary structure at 850 mu m. IRAS 20050+2720 is composed of a chain of three subclusters, in agreement with Chen and coworkers, although our results show that two of the subclusters appear to overlap. Significant 850 mu m emission is detected toward two of the subclusters but is not detected toward the central subcluster, suggesting that the dense gas may already be cleared there. In contrast to these two highly embedded subclusters, we find an anticorrelation of the stars and dust in NGC 7129, indicating that much of the parental gas and dust has been dispersed. The NGC 7129 cluster exhibits a higher degree of azimuthal symmetry, a lower stellar surface density, and a larger size than the other two clusters, suggesting that the cluster may be dynamically expanding following the recent dispersal of natal molecular gas. These analyses are further evidence that embedded, forming clusters are often not spherically symmetric structures but can be elongated and clumpy and that these morphologies may reflect the initial structure of the dense molecular gas. Furthermore, this work suggests that gas expulsion by stellar feedback results in significant dynamical evolution within the first 3 Myr of cluster evolution. We estimate peak stellar volume densities and discuss the impact of these densities on the evolution of circumstellar disks and protostellar envelopes. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Gutermuth, RA (reprint author), Univ Rochester, Dept Phys & Astron, 601 Elmwood Ave, Rochester, NY 14627 USA. EM rguter@astro.pas.rochester.edu OI Williams, Jonathan/0000-0001-5058-695X NR 73 TC 112 Z9 113 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 OCT 10 PY 2005 VL 632 IS 1 BP 397 EP 420 DI 10.1086/432460 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EZ UT WOS:000232366000028 ER PT J AU Torres, MAP Garcia, MR Steeghs, D McClintock, JE AF Torres, MAP Garcia, MR Steeghs, D McClintock, JE TI On the binary nature of 1RXS J162848.1-415241 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; stars : individual (RX J1628-41); X-rays : stars ID RS-CANUM-VENATICORUM; DIFFUSE INTERSTELLAR BANDS; LOW GALACTIC LATITUDES; LATE-TYPE STARS; ALL-SKY SURVEY; BLACK-HOLE; ACTIVE STARS; MASS-LOSS; MICROQUASAR CANDIDATES; ECHELLE SPECTROGRAPH AB We present spectroscopy of the optical counterpart to 1RXS J162848.1-41524, also known as the microquasar candidate MCQC J162847-4152. All the data indicate that this X-ray source is not a microquasar and that it is a single-lined chromospherically active binary system with a likely orbital period of 4.9 days. Our analysis supports a K3 IV spectral classification for the star, which is dominant at optical wavelengths. The unseen binary component is most likely a late-type (K7-M) dwarf or a white dwarf. Using the high-resolution spectra, we have measured the K3 star's rotational broadening to be v sin i = 43 +/- 3 km s(-1) and determined a lower limit to the binary mass ratio of q(M-2/ M-1) > 2.0. The high rotational broadening together with the strong Ca II H and K/H alpha emission and high-amplitude photometric variations indicate that the evolved star is very chromospherically active and responsible for the X-ray/radio emission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, MAP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mtorres@cfa.harvard.edu; mgarcia@cfa.harvard.edu; dsteeghs@cfa.harvard.edu; jem@cfa.harvard.edu RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 80 TC 2 Z9 2 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2005 VL 632 IS 1 BP 514 EP 522 DI 10.1086/432907 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EZ UT WOS:000232366000036 ER PT J AU Kim, JS Hines, DC Backman, DE Hillenbrand, LA Meyer, MR Rodmann, J Moro-Martin, A Carpenter, JM Silverstone, MD Bouwman, J Mamajek, EE Wolf, S Malhotra, R Pascucci, I Najita, J Padgett, DL Henning, T Brooke, TY Cohen, M Strom, SE Stobie, EB Engelbracht, CW Gordon, KD Misselt, K Morrison, JE Muzerolle, J Su, KYL AF Kim, JS Hines, DC Backman, DE Hillenbrand, LA Meyer, MR Rodmann, J Moro-Martin, A Carpenter, JM Silverstone, MD Bouwman, J Mamajek, EE Wolf, S Malhotra, R Pascucci, I Najita, J Padgett, DL Henning, T Brooke, TY Cohen, M Strom, SE Stobie, EB Engelbracht, CW Gordon, KD Misselt, K Morrison, JE Muzerolle, J Su, KYL TI Formation and evolution of planetary systems: Cold outer disks associated with sun-like stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : formation; stars : formation ID SPITZER-SPACE-TELESCOPE; MULTIBAND IMAGING PHOTOMETER; SPECTRAL IRRADIANCE CALIBRATION; INFRARED ARRAY CAMERA; EDGEWORTH-KUIPER BELT; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; DEBRIS DISKS; DUSTY DEBRIS; REDUCTION ALGORITHMS AB We present the discovery of debris systems around three Sun-like stars based on observations performed with the Spitzer Space Telescope as part of a Legacy Science Program, "The Formation and Evolution of Planetary Systems'' ( FEPS). We also confirm the presence of debris around two other stars. All the stars exhibit infrared emission in excess of the expected photospheres in the 70 mu m band but are consistent with photospheric emission at <= 33 mu m. This restricts the maximum temperature of debris in equilibrium with the stellar radiation to T < 70 K. We find that these sources are relatively old in the FEPS sample, in the age range 0.7 - 3 Gyr. On the basis of models of the spectral energy distributions, we suggest that these debris systems represent materials generated by collisions of planetesimal belts. We speculate on the nature of these systems through comparisons to our own Kuiper Belt, and on the possible presence of planet( s) responsible for stirring the system and ultimately releasing dust through collisions. We further report observations of a nearby star HD 13974 ( d 11 pc) that are indistinguishable from a bare photosphere at both 24 and 70 mu m. The observations place strong upper limits on the presence of any cold dust in this nearby system (L-IR/L-* < 10 (-5.2)). C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Space Sci Inst, Boulder, CO 80303 USA. NASA, Ames Res Ctr, SOFIA, Moffett Field, CA 94035 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Princeton Univ, Princeton, NJ 08540 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. RP Kim, JS (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. OI Malhotra, Renu/0000-0002-1226-3305; Su, Kate/0000-0002-3532-5580 NR 57 TC 62 Z9 62 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 OCT 10 PY 2005 VL 632 IS 1 BP 659 EP 669 DI 10.1086/432863 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EZ UT WOS:000232366000045 ER PT J AU Mayo, J Cooke, R AF Mayo, J Cooke, R TI Prehispanic seashell industry in Gran Cocle, Panama. Technological analysis of seashell artefacts of a dustman shop of Cerro Juan Diaz, Los Santos, Panama SO ARCHAEOFAUNA LA Spanish DT Article DE tecnology; prehispanic seashells industry; Panama ID EXCHANGE AB In America tools and beads of seashells are found frequently scattered in graves and ritual contexts and also in workshops. Studies of these workshops gives us details of the technic of manufacture used, inter-regional exchange, as well as other, like craft specialization. At Cerro Juan Diaz, Panama, a site that for several hundred years was occupied as a burial site and hamlet, a workshop of seashells, with Strombus galeatus, Spondylus spp, Anadara grandis flakes, preforms and beads are found, in addition to lithic flakes and bone. The study of these materials has allowed to evaluate the level of technical development of this industry in the final of the Middle Ceramic Period, which in our opinion is the key to estimate the presence or no of craft specialization. We believe that at this moment it was craft specialization in funtion of the high level of technical development present in this industry considering the number of beads, their rank of manufacture, and the raw material selection. In order to carry out our research it was necesary to develop an original method of analysis to obtain information about the technology applied in seashell material. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Mayo, J (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM mayoi@si.edu; cooker@si.edu NR 30 TC 5 Z9 6 U1 1 U2 5 PU LABORATORIO DE ARQUEOZOOLOGIA, DPTO. BIOLOGIA PI MADRID PA UNIVERSIDAD AUTONOMA DE MADRID, MADRID, 28049, SPAIN SN 1132-6891 J9 ARCHAEOFAUNA JI Archaeofauna PD OCT PY 2005 VL 14 BP 285 EP 298 PG 14 WC Archaeology SC Archaeology GA 980LJ UT WOS:000233019700018 ER PT J AU Rines, K Geller, MJ Kurtz, MJ Diaferio, A AF Rines, K Geller, MJ Kurtz, MJ Diaferio, A TI CAIRNS: The Cluster and Infall Region Nearby Survey. III. Environmental dependence of H alpha properties of galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (A119, A168, A194, A496, A539, A1367, A1656, A2199); galaxies : fundamental parameters; galaxies : kinematics and dynamics ID EMISSION-LINE GALAXIES; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; EARLY DATA RELEASE; VIRGO CLUSTER; COMA CLUSTER; LUMINOSITY FUNCTION; RICH CLUSTERS; REDSHIFT SURVEY; FIELD GALAXIES AB We investigate the environmental dependence of star formation in cluster virial regions and infall regions as part of the Cluster and Infall Region Nearby Survey (CAIRNS), a large spectroscopic survey of the infall regions surrounding nine nearby rich clusters of galaxies. We use complete, homogeneous spectroscopic surveys of K(s)-limited samples in eight of the CAIRNS clusters. Our long-slit spectroscopy yields estimates of star formation rates in environments from cluster cores to the general large-scale structure. Galaxies in infall regions probe whether processes affecting star formation are effective over scales larger than cluster virial regions. The fraction of galaxies with current star formation in their inner disks as traced by H alpha emission increases with distance from the cluster and converges to the "field" value only at 2-3 virial radii, in agreement with other investigations. However, among galaxies with significant current star formation (EW [H alpha] >= 2 angstrom), there is no difference in the distribution of EW[H alpha] inside and outside the virial radius. This surprising result, first seen by Carter and coworkers, suggests that (1) star formation is truncated either on very short timescales or only at moderate and high redshifts or (2) that projection effects contaminate the measurement. We quantify the possible impact of mechanisms that only affect the outer parts of galaxies and thus might not be detected in this survey or any fiber-based survey. The number density profiles of star-forming and non-star-forming galaxies indicate that, among galaxies projected inside the virial radius, at least half the former and 20% of the latter are "infall interlopers," galaxies in the infall region but outside the virial region. We show that the kinematics of star-forming galaxies in the infall region closely match those of absorption-dominated galaxies. This result shows that the star-forming galaxies in the infall regions are not interlopers from the field and excludes one model of the backsplash scenario of galaxy transformation. Finally, we quantify systematic uncertainties in estimating the global star formation in galaxies from their inner disks. C1 Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. RP Rines, K (reprint author), Yale Univ, Yale Ctr Astron & Astrophys, POB 208121, New Haven, CT 06520 USA. EM krines@astro.yale.edu; mgeller@cfa.harvard.edu; mkurtz@cfa.harvard.edu; diaferio@ph.unito.it RI KURTZ, Michael /B-3890-2009 NR 84 TC 69 Z9 69 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2005 VL 130 IS 4 BP 1482 EP 1501 DI 10.1086/433173 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969XW UT WOS:000232270200011 ER PT J AU Kim, S Walsh, W Xiao, KC Lane, AP AF Kim, S Walsh, W Xiao, KC Lane, AP TI A (CO)-C-12 J=4 -> 3 high-velocity cloud in the Large Magellanic Cloud SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : atoms; ISM : general; ISM : molecules; Magellanic Clouds ID ANTARCTIC-SUBMILLIMETER-TELESCOPE; REMOTE-OBSERVATORY OBSERVATIONS; 30 DORADUS; APERTURE SYNTHESIS; 30-DORADUS NEBULA; MOLECULAR CLOUDS; STAR-FORMATION; CO SURVEY; EMISSION; COMPLEX AB We present Antarctic Submillimeter Telescope and Remote Observatory observations of (CO)-C-12 J = 4 -> 3 and (12)[C I] emission in the 30 Doradus complex in the Large Magellanic Cloud. We detected strong (CO)-C-12 J = 4 -> 3 emission toward R140, a multiple system of Wolf-Rayet stars located on the rim of the expanding H II shell surrounding the R136 cluster. We also detected a high-velocity gas component as a separate feature in the (CO)-C-12 J = 4 -> 3 spectrum. This component probably originates from molecular material accelerated as a result of the combined motion induced by the stellar winds and explosions of supernovae, including several fast-expanding H II shells in the complex. The lower limit on the total kinetic energy of the atomic and molecular gas component is similar to 2 x 10(51) ergs, suggesting that this comprises only 20% of the total kinetic energy contained in the H II complex structure. C1 Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, S (reprint author), Sejong Univ, Dept Astron & Space Sci, KunJa Dong 98, Seoul 143747, South Korea. EM skim@arcsec.sejong.ac.kr; wwalsh@cfa.harvard.edu; kxiao@cfa.harvard.edu; adair@cfa.harvard.edu NR 27 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2005 VL 130 IS 4 BP 1635 EP 1639 DI 10.1086/432933 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969XW UT WOS:000232270200021 ER PT J AU Meixner, M McCullough, P Hartman, J Son, M Speck, A AF Meixner, M McCullough, P Hartman, J Son, M Speck, A TI The multitude of molecular hydrogen knots in the Helix Nebula SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary nebulae : individual (NGC 7293) ID PLANETARY-NEBULAE; COMETARY KNOTS; EMISSION; RING; MORPHOLOGY; EVOLUTION; NGC-7293; MODELS; DUST; CO AB We present Hubble Space Telescope NICMOS imaging of the H-2 2.12 mu m emission in five fields in the Helix Nebula ranging in radial distance from 25000 to 45000 from the central star. The images reveal arcuate structures with their apexes pointing toward the central star. These molecular hydrogen knots are most highly structured in the fields closest to the central star and become increasingly less structured with increasing radius. Comparison of these images with ground-based images of comparable resolution reveals that the molecular gas is more highly clumped than the ionized gas line tracers. From our images, we determine an average number density of knots in the molecular gas ranging from 162 knots arcmin(-2) in the denser regions to 18 knots arcmin(-2) in the lower density outer regions. The decreasing number density of H-2 knots in the outer regions creates a lower filling factor of neutral and molecular gas emission in the radio observations of CO and H I and may explain why these outer regions, where we clearly detect H-2 2.12 mu m, fall below the detection limit of the radio observations. Using this new number density, we estimate the total number of knots in the Helix to be similar to 23,000, which is a factor of 6.5 larger than previous estimates. The total neutral gas mass in the Helix is 0.35 M-circle dot assuming a mass of similar to 1.5 x 10(-5) M-circle dot for the individual knots. The H-2 emission structure of the entire Helix Nebula supports the recent interpretation of the Helix as a nearly pole-on polypolar planetary nebula (PN). The H-2 intensity, (5-9) x 10(-5) ergs s(-1) cm(-2) sr(-1), remains relatively constant with projected distance from the central star, suggesting a heating mechanism for the molecular gas that is distributed almost uniformly in the knots throughout the nebula. The temperature and H-2 2.12 mu m intensity of the knots can be approximately explained by photodissociation regions (PDRs) in the individual knots; however, theoretical PDR models of PNs underpredict the intensities of some knots by a factor of 10. The brightest H-2 emission (similar to 3 x 10(-4) ergs s(-1) cm(-2) sr(-1)) may be enhanced by a larger than unity area filling factor of H-2 knots or may be an individual H-2 knot exposed to direct starlight, causing rapid photoevaporation compared with the more embedded knots of the disk. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr, Baltimore, MD 21218 USA. Univ Missouri, Dept Phys, Columbia, MO 65211 USA. RP Meixner, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM meixner@stsci.edu; pmcc@stsci.edu; jhartman@cfa.harvard.edu; mhson@pha.jhu.edu; speckan@missouri.edu RI Son, Minho/N-9470-2015; OI Hartman, Joel/0000-0001-8732-6166 NR 32 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2005 VL 130 IS 4 BP 1784 EP 1794 DI 10.1086/444539 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969XW UT WOS:000232270200033 ER PT J AU Tiengo, A Galloway, DK di Salvo, T Mendez, M Miller, JM Sokoloski, JL van der Klis, M AF Tiengo, A Galloway, DK di Salvo, T Mendez, M Miller, JM Sokoloski, JL van der Klis, M TI Discovery of a redshifted X-ray emission line in the symbiotic neutron star binary 4U 1700+24 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : individuals : 4U 1700+24; stars : neutron; stars : binaries : symbiotic; line : identification ID XMM-NEWTON; ATOMIC DATA; CYGNUS-X-3; SPECTRA; IONS; JET AB We present the spectral analysis of an XMM-Newton observation of the X-ray binary 4U 1700+24, performed during an outburst in August 2002. The EPIC-PN spectrum above 1 keV can be modeled by a blackbody plus Comptonization model, as in previous observations. At lower energies, however, we detect a prominent soft excess, which we model with a broad Gaussian centered at similar to 0.5 keV. In the high resolution RGS spectrum we detect a single emission line, centered at 19.19(-0.09)(+0.05) angstrom We discuss two possible interpretations for this line: O VIII at redshift z=0.012(-0.004)(+0.002) or Ne IX at redshift z similar to 0.4. C1 Ist Astrofis Spaziale & Fis Cosm, Sez Milano G Occhialini INAF, I-20133 Milan, Italy. Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Palermo, Dipartimento Sci Fis & Astron, I-90123 Palermo, Italy. SRON, Natl 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. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. RP Tiengo, A (reprint author), Ist Astrofis Spaziale & Fis Cosm, Sez Milano G Occhialini INAF, Via Bassini 15, I-20133 Milan, Italy. EM tiengo@mi.iasf.cnr.it RI Di Salvo, Tiziana/F-3973-2012; Mendez, Mariano/C-8011-2012; OI Di Salvo, Tiziana/0000-0002-3220-6375; Mendez, Mariano/0000-0003-2187-2708; Tiengo, Andrea/0000-0002-6038-1090; Galloway, Duncan/0000-0002-6558-5121 NR 25 TC 12 Z9 12 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 OCT PY 2005 VL 441 IS 1 BP 283 EP 287 DI 10.1051/0004-6361:20035742 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 964IZ UT WOS:000231875600029 ER PT J AU Panessa, F Wolter, A Pellegrini, S Fruscione, A Bassani, L Della Ceca, R Palumbo, GGC Trinchieri, G AF Panessa, F Wolter, A Pellegrini, S Fruscione, A Bassani, L Della Ceca, R Palumbo, GGC Trinchieri, G TI The nature of composite Seyfert/star-forming galaxies revealed by X-ray observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : peculiar; galaxies : starburst; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; FORMATION RATE INDICATOR; XMM-NEWTON OBSERVATIONS; EMISSION-LINE GALAXIES; 2-10 KEV LUMINOSITY; ALL-SKY SURVEY; BLACK-HOLES; ELLIPTIC GALAXIES; SOURCE POPULATION AB This paper presents new Chandra and BeppoSAX observations aimed at investigating the optical-X-ray mismatch in the enigmatic class of the composite galaxies discovered by a cross-correlation of IRAS and ROSAT all-sky survey catalogs. These galaxies have been classified as star-forming objects on the basis of their optical spectra, while the detection of weak broad wings in the H alpha emission in a few of them and their high X-ray luminosity in the ROSAT band indicated the presence of an active nucleus. The analysis of Chandra observations for four composite galaxies has revealed nuclear pointlike sources, with a typical AGN spectrum (Gamma similar to 1.7-1.9) and little intrinsic absorption. A strong flux variability has been observed on different timescales; in particular, most of the sources were brighter at the ROSAT epoch. Although it is of relatively low luminosity for the AGN class (L(2-10keV)similar to 3-60x10(41) ergs s(-1)), the active nucleus is nevertheless dominant in the X-ray domain. At other wavelengths it appears to be overwhelmed by the starburst and/or host galaxy light, yielding the composite classification for these objects. C1 UC, CSIC, Inst Fis Cantabria, Santander 39005, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Brera, I-20121 Milan, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. CNR, IASF, I-40129 Bologna, Italy. RP Panessa, F (reprint author), UC, CSIC, Inst Fis Cantabria, Avenida Castros, Santander 39005, Spain. OI Wolter, Anna/0000-0001-5840-9835; Della Ceca, Roberto/0000-0001-7551-2252; Trinchieri, Ginevra/0000-0002-0227-502X; Panessa, Francesca/0000-0003-0543-3617; Bassani, Loredana/0000-0003-4858-6963 NR 60 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2005 VL 631 IS 2 BP 707 EP 719 DI 10.1086/432569 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300004 ER PT J AU Young, AJ Lee, JC Fabian, AC Reynolds, CS Gibson, RR Canizares, CR AF Young, AJ Lee, JC Fabian, AC Reynolds, CS Gibson, RR Canizares, CR TI A Chandra HETGS spectral study of the iron K bandpass in MCG-6-30-15: A narrow view of the broad iron line SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; galaxies : individual (MCG-6-30-15); galaxies : Seyfert; X-rays : galaxies ID TRANSMISSION GRATING SPECTROMETER; ACTIVE GALACTIC NUCLEI; RAY ABSORPTION-LINES; 1 GALAXY MCG-6-30-15; DUSTY WARM ABSORBER; ASCA OBSERVATIONS; BLACK-HOLE; XMM-NEWTON; ALPHA LINE; EMISSION-LINE AB We present a high-resolution X-ray spectrum of the iron K bandpass in MCG -6-30-15 based on a 522 ks observation with Chandra's High Energy Transmission Grating Spectrometer ( HETGS). The Chandra spectrum is consistent with the presence of a relativistically broadened, highly redshifted iron K alpha emission line with a profile similar to previous observations. A number of narrow features are detected above 2 keV, including a narrow Fe K alpha emission line and narrow absorption lines from H- and He-like Fe, H- like S, and H- like Si. This absorption is well described by a photoionized plasma with a column density log N-H 23: 2 and an ionization parameter log xi 3: 6, assuming the iron abundance has the solar value and a velocity dispersion parameter b = 100 km s(-1). Applying this absorption model to a high-fidelity XMM-Newton EPIC pn spectrum, we find that a broad iron line is still required with emission extending to within 1.9r(g) of the black hole. If the iron line comes from an accretion disk truncated at the innermost stable circular orbit, this indicates that the black hole must be spinning rapidly with a > 0.95. Ionized absorption models attempting to explain the 3-6 keV spectral curvature without strong gravity predict absorption lines in the 6.4-6.6 keV range that are inconsistent with the Chandra spectrum. The H- and He-like iron absorption lines in the Chandra spectrum are blueshifted by 2.0(-0.9)(+0.7) x 10(3) km s(-1) compared to the source frame and may originate in a high-velocity, high-ionization component of the warm absorber outflow. This high-ionization component may dominate the energy budget of the outflow and account for a significant fraction of the outflowing mass. Detailed modeling of the warm absorber below 2 keV will be addressed in a later paper, but our results are robust to the broader details of the warm absorber behavior. The difference spectrum between the high- and low-flux states is well described by a power law, in agreement with previous studies. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Young, AJ (reprint author), MIT, Ctr Space Res, 77 Massachuestts Ave, Cambridge, MA 02139 USA. NR 51 TC 68 Z9 68 U1 2 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2005 VL 631 IS 2 BP 733 EP 740 DI 10.1086/432607 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300007 ER PT J AU Williams, BF Garcia, MR Primini, FA McClintock, JE Murray, SS AF Williams, BF Garcia, MR Primini, FA McClintock, JE Murray, SS TI Optical constraints on an X-ray transient source in M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; galaxies : individual (M31); X-rays : binaries; X-rays : stars ID NOVA XTE J1550-564; ROSAT PSPC SURVEY; BLACK-HOLE; CENTRAL REGION; LIGHT CURVES; BINARIES; CHANDRA; MASS; OUTBURST; A0620-00 AB We have detected a transient X-ray source in the M31 bulge through a continuing monitoring campaign with the Chandra ACIS-I camera. The source was detected at R.A. 00(h)42(m)33(s).428 +/- 0".11, decl: =+41 degrees 17'03".37 +/- 0".11 in only a single observation taken 2004 May 23. Fortuitous optical HSTACS imaging of the transient location prior to the X-ray outburst, along with follow-up HSTACS imaging during and after the outburst, reveals no transient optical source brighter than B( equivalent) 25.5. The location of the source and its X-ray properties suggest that it is a low-mass X-ray binary (LMXB). Assuming the transient is similar to many Galactic X-ray novae, the X-ray luminosity of (3.9 +/- 0.4); 10(37) ergs s(-1) and the upper limit on the optical luminosity provide a prediction of <= 1.6 days for the orbital period of the binary system. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head.cfa.harvard.edu; garcia@head.cfa.harvard.edu; fap@head.cfa.harvard.edu; jem@head.cfa.harvard.edu; ssm@head.cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 NR 23 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2005 VL 631 IS 2 BP 832 EP 837 DI 10.1086/432597 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300015 ER PT J AU Williams, RJ Mathur, S Nicastro, F Elvis, M Drake, JJ Fang, TT Fiore, F Krongold, Y Wang, QD Yao, YS AF Williams, RJ Mathur, S Nicastro, F Elvis, M Drake, JJ Fang, TT Fiore, F Krongold, Y Wang, QD Yao, YS TI Probing the local group medium toward Markarian 421 with Chandra and the far ultraviolet spectroscopic explorer SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy : halo; intergalactic medium; quasars : absorption lines ID X-RAY FOREST; HOT INTERGALACTIC MEDIUM; HIGH-VELOCITY CLOUDS; GALACTIC HALO; LOW-REDSHIFT; ALPHA ABSORPTION; RESONANCE LINES; MISSING BARYONS; IONIZED-GAS; O-VI AB We report the detection of highly ionized gas at z similar to 0 seen in resonant UV and X-ray absorption lines toward the z 0: 03 blazar Mrk 421. A total of 13 X-ray and three UV lines were measured ( or upper limits derived), including three lines in the O VII K series and K alpha transitions from neon, carbon, and nitrogen. From the three O VII lines we derive a 2 sigma Doppler parameter constraint of 24 km s(-1) < b < 55 km s(-1). The FUSE spectrum shows strong Galactic low-velocity O VI lambda 1032 absorption and a possible weak O vi high-velocity component (HVC). The Doppler parameter of the low-velocity O vi measured with FUSE is similar to 3 sigma higher than that derived from the O VII line ratios, indicating that the O VII and Galactic O vi arise in different phases. This velocity dispersion along with limits on the gas temperature and density from the X-ray line ratios ( assuming a single phase with collisional ionization equilibrium plus photoionization) are all consistent with an extragalactic absorber. However, the O VII Doppler parameter is inconsistent with the high temperature required to produce the observed O VIHVC/O ratio, implying that the HVC is probably not related to the O VII. In addition, the O VIK alpha line detected by Chandra implies a column density similar to 4 times higher than the lambda 1032 absorption. Although an extragalactic absorber is fully consistent with the measured column density ratios, a Galactic origin cannot be ruled out given the uncertainties in the available data. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Williams, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM williams@astronomy.ohio-state.edu; smita@astronomy.ohio-state.edu; fnicastro@cfa.harvard.edu OI Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 49 TC 55 Z9 55 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 OCT 1 PY 2005 VL 631 IS 2 BP 856 EP 867 DI 10.1086/431343 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300017 ER PT J AU Popowski, P Griest, K Thomas, CL Cook, KH Bennett, DP Becker, AC Alves, DR Minniti, D Drake, AJ Alcock, C Allsman, RA Axelrod, TS Freeman, KC Geha, M Lehner, MJ Marshall, SL Nelson, CA Peterson, BA Quinn, PJ Stubbs, CW Sutherland, W Vandehei, T Welch, D AF Popowski, P Griest, K Thomas, CL Cook, KH Bennett, DP Becker, AC Alves, DR Minniti, D Drake, AJ Alcock, C Allsman, RA Axelrod, TS Freeman, KC Geha, M Lehner, MJ Marshall, SL Nelson, CA Peterson, BA Quinn, PJ Stubbs, CW Sutherland, W Vandehei, T Welch, D CA MACHO Collaboration TI Microlensing optical depth toward the galactic bulge using clump giants from the macho survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; Galaxy : stellar content; Galaxy : structure; gravitational lensing; surveys ID GRAVITATIONAL LENSING EXPERIMENT; DIFFERENCE IMAGE-ANALYSIS; EXTINCTION MAP; BAADES WINDOW; ZERO-POINT; PROJECT; EVENTS; PHOTOMETRY; BAR; DISCOVERY AB Using 7 yr of MACHO survey data, we present a new determination of the optical depth to microlensing toward the Galactic bulge. We select the sample of 62 microlensing events ( 60 unique) on clump giant sources and perform a detailed efficiency analysis. We use only the clump giant sources because these are bright bulge stars and are not as strongly affected by blending as other events. Using a subsample of 42 clump events concentrated in an area of 4.5 deg(2) with 739,000 clump giant stars, we find tau 2.17(-0.38)(+0.47) x 10(-6) at (l, b) (1.degrees 50; -2.degrees 68), somewhat smaller than found in most previous MACHO studies but in excellent agreement with recent theoretical predictions. We also present the optical depth in each of the 19 fields in which we detected events and find limits on optical depth for fields with no events. The errors in optical depth in individual fields are dominated by Poisson noise. We measure optical depth gradients of (1.06 +/- 0.71)x 10(-6) deg(-1) and (0.29 +/- 0.43)x 10(-6) deg(-1) in the Galactic latitude b and longitude l directions, respectively. Finally, we discuss the possibility of anomalous duration distribution of events in the field 104 centered on (l; b) (3 degrees.11, -3 degrees.01), as well as investigate spatial clustering of events in all fields. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Univ Notre Dame, Dept Phys, South Bend, IN 46556 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20781 USA. Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Carnegie Observ, Pasadena, CA 91101 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. European So Observ, D-85748 Garching, Germany. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. McMaster Univ, Hamilton, ON L8S 4M1, Canada. RP Popowski, P (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1,Postfach 1317, D-85741 Garching, Germany. EM popowski@mpa-garching.mpg.de; griest@astrophys.ucsd.edu; clt@ucsd.edu; kcook@igpp.ucllnl.org; bennett@emu.phys.nd.edu; becker@astro.washington.edu; alves@lasp680.gsfc.nasa.gov; dante@astro.puc.cl; ajd@astro.puc.cl; calcock@cfa.harvard.edu; robyn@noao.edu; cnelson@igpp.ucllnl.org; cstubbs@cfa.harvard.edu; vandehei@astrophys.ucsd.edu RI Stubbs, Christopher/C-2829-2012; Quinn, Peter/B-3638-2013 OI Stubbs, Christopher/0000-0003-0347-1724; NR 47 TC 72 Z9 74 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 OCT 1 PY 2005 VL 631 IS 2 BP 879 EP 905 DI 10.1086/432246 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300019 ER PT J AU Thomas, CL Griest, K Popowski, P Cook, KH Drake, AJ Minniti, D Myer, DG Alcock, C Allsman, RA Alves, DR Axelrod, TS Becker, AC Bennett, DP Freeman, KC Geha, M Lehner, MJ Marshall, SL Nelson, CA Peterson, BA Quinn, PJ Stubbs, CW Sutherland, W Vandehei, T Welch, DL AF Thomas, CL Griest, K Popowski, P Cook, KH Drake, AJ Minniti, D Myer, DG Alcock, C Allsman, RA Alves, DR Axelrod, TS Becker, AC Bennett, DP Freeman, KC Geha, M Lehner, MJ Marshall, SL Nelson, CA Peterson, BA Quinn, PJ Stubbs, CW Sutherland, W Vandehei, T Welch, DL CA MACHO Collaboration TI Galactic bulge microlensing events from the MACHO collaboration SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; Galaxy : bulge; Galaxy : structure; gravitational lensing; stars : dwarf novae; stars : variables : other ID GRAVITATIONAL LENSING EXPERIMENT; DIFFERENCE IMAGE-ANALYSIS; LARGE-MAGELLANIC-CLOUD; SAGITTARIUS DWARF GALAXY; OPTICAL DEPTH; MILKY-WAY; DARK MATTER; PROJECT; PHOTOMETRY; HALO AB We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars. C1 Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20781 USA. Steward Observ, Tucson, AZ 85721 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Notre Dame, Dept Phys, South Bend, IN 46556 USA. Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Carnegie Observ, Pasadena, CA 91101 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. European So Observ, D-85748 Garching, Germany. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. McMaster Univ, Hamilton, ON L8S 4M1, Canada. RP Thomas, CL (reprint author), Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. EM clt@ucsd.edu; kgriest@ucsd.edu; popowski@mpa-garching.mpg.de; kcook@igpp.ucllnl.org; ajd@astro.puc.cl; dante@astro.puc.cl; dmyer@ucsd.edu; calcock@cfa.harvard.edu; robyn@noao.edu; alves@astro.columbia.edu; taxelrod@as.arizona.edu; becker@astro.washington.edu; cnelson@igpp.ucllnl.org; cstubbs@cfa.harvard.edu; vandehei@astrophys.ucsd.edu RI Myer, David/E-1425-2011; Stubbs, Christopher/C-2829-2012; Quinn, Peter/B-3638-2013; OI Myer, David/0000-0001-8599-3694; Stubbs, Christopher/0000-0003-0347-1724; Lehner, Matthew/0000-0003-4077-0985 NR 56 TC 18 Z9 18 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 OCT 1 PY 2005 VL 631 IS 2 BP 906 EP 934 DI 10.1086/432247 PN 1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300020 ER PT J AU Cunningham, A Frank, A Hartmann, L AF Cunningham, A Frank, A Hartmann, L TI Wide-angle wind-driven bipolar outflows: High-resolution models with application to source I of the Becklin-Neugebauer/Kleinmann-Low OMC-I region SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (OMC-I BN/KL); ISM : jets and outflows; stars : formation ID YOUNG STELLAR OBJECTS; MOLECULAR-HYDROGEN; HYDRODYNAMICAL MODELS; INFRARED-EMISSION; SIO MASERS; ORION-KL; SHOCKS; DISSOCIATION; SIMULATIONS; IONIZATION AB We carry out high-resolution simulations of the inner regions of a wide-angle wind-driven bipolar outflow using an adaptive mesh refinement code. Our code follows H-He gas with molecular, atomic, and ionic components and the associated time-dependent molecular chemistry and ionization dynamics with radiative cooling. Our simulations explore the nature of the outflow when a spherical wind expands into a rotating, collapsing envelope. We compare these with key observational properties of the outflow system of source I in the BN/KL region. Our calculations show that the wind evacuates a bipolar outflow cavity in the infalling envelope. We find the head of the outflow to be unstable and that it rapidly fragments into clumps. We resolve the dynamics of the strong shear layer, which defines the side walls of the cavity. We conjecture that this layer is the likely site of maser emission and examine its morphology and rotational properties. The shell of swept-up ambient gas that delineates the cavity edge retains its angular momentum. This rotation is roughly consistent with that observed in the source I SiO maser spots. The observed proper motions and line-of-sight velocity are approximately reproduced by the model. The cavity shell at the base of the flow assumes an X-shaped morphology that is also consistent with source I. We conclude that the wide opening angle of the outflow is evidence that a wide-angle wind drives the source I outflow and not a collimated jet. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cunningham, A (reprint author), Univ Rochester, Dept Phys & Astron, Bausch & Lomb Hall, Rochester, NY 14627 USA. NR 51 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2005 VL 631 IS 2 BP 1010 EP 1021 DI 10.1086/432658 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300027 ER PT J AU Hollenbach, D Gorti, U Meyer, M Kim, JS Morris, P Najita, J Pascucci, I Carpenter, J Rodmann, J Brooke, T Hillenbrand, L Mamajek, E Padgett, D Soderblom, D Wolf, S Lunine, J AF Hollenbach, D Gorti, U Meyer, M Kim, JS Morris, P Najita, J Pascucci, I Carpenter, J Rodmann, J Brooke, T Hillenbrand, L Mamajek, E Padgett, D Soderblom, D Wolf, S Lunine, J TI Formation and evolution of planetary systems: Upper limits to the gas mass in HD 105 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; planetary systems : formation; planets and satellites : formation; solar system : formation; stars : individual (HD 105) ID T-TAURI STARS; SOLAR-TYPE STARS; SPITZER-SPACE-TELESCOPE; INFRARED SPECTROGRAPH IRS; CO FUNDAMENTAL EMISSION; MAIN-SEQUENCE STARS; HERBIG AE STARS; CIRCUMSTELLAR DISKS; GRAIN-GROWTH; PROTOPLANETARY DISKS AB We report infrared spectroscopic observations of HD 105, a nearby (similar to 40 pc) and relatively young (similar to 30 Myr) G0 star with excess infrared continuum emission, which has been modeled as arising from an optically thin circumstellar dust disk with an inner hole of size greater than or similar to 13 AU. We have used the high spectral resolution mode of the Infrared Spectrometer (IRS) on the Spitzer Space Telescope to search for gas emission lines from the disk. The observations reported here provide upper limits to the fluxes of H-2 S(0) 28 mu m, H-2 S(1) 17 mu m, H-2 S(2) 12 mu m, [Fe (II)] 26 mu m, [Si (II)] 35 mu m, and [S (I)] 25 mu m infrared emission lines. The H2 line upper limits place direct constraints on the mass of warm molecular gas in the disk: M(H-2) < 4.6, 3.8 x 10(-2), and 3.0 x 10(-3) M-J at T = 50, 100, and 200 K, respectively. We also compare the line flux upper limits to predictions from detailed thermal/chemical models of various gas distributions in the disk. These comparisons indicate that if the gas distribution has an inner hole with radius r(i,gas), the surface density at that inner radius is limited to values ranging from less than or similar to 3 g cm(-2) at r(i,gas) = 0.5 AU to 0.1 g cm(-2) at r(i,gas) = 5-20 AU. These values are considerably below the value for a minimum mass solar nebula, and suggest that less than 1 Jupiter mass (M-J) of gas (at any temperature) exists in the 1-40 AU planet-forming region. Therefore, it is unlikely that there is sufficient gas for gas giant planet formation to occur in HD 105 at this time. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. CALTECH, Pasadena, CA 91125 USA. Max Planck Inst Astron, Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Arizona, Lunar Planetary Lab, Tucson, AZ 85721 USA. RP Hollenbach, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 83 TC 34 Z9 34 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 OCT 1 PY 2005 VL 631 IS 2 BP 1180 EP 1190 DI 10.1086/432638 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300042 ER PT J AU Winn, JN Noyes, RW Holman, MJ Charbonneau, D Ohta, Y Taruya, A Suto, Y Narita, N Turner, EL Johnson, JA Marcy, GW Butler, RP Vogt, SS AF Winn, JN Noyes, RW Holman, MJ Charbonneau, D Ohta, Y Taruya, A Suto, Y Narita, N Turner, EL Johnson, JA Marcy, GW Butler, RP Vogt, SS TI Measurement of spin-orbit alignment in an extrasolar planetary system SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planetary systems : formation; stars : individual (HD 209458); stars : rotation ID RADIAL-VELOCITY CURVES; CLOSE BINARY-SYSTEMS; TRANSITING PLANET; TIDAL EVOLUTION; HOT JUPITERS; COOL STARS; 51 PEGASI; ROTATION; COMPANION; HD-209458 AB We determine the stellar, planetary, and orbital properties of the transiting planetary system HD 209458 through a joint analysis of high-precision radial velocities, photometry, and timing of the secondary eclipse. Of primary interest is the strong detection of the Rossiter-McLaughlin effect, the alteration of photospheric line profiles that occurs because the planet occults part of the rotating surface of the star. We develop a new technique for modeling this effect and use it to determine the inclination of the planetary orbit relative to the apparent stellar equator (gamma = -4 degrees.4 +/- 1 degrees.4), and the line-of-sight rotation speed of the star (vsinI(*) = 4.70 +/- 0.16 km s(-1)). The uncertainty in these quantities has been reduced by an order of magnitude relative to the pioneering measurements by Queloz and collaborators. The small but nonzero misalignment is probably a relic of the planet formation epoch, because the expected timescale for tidal coplanarization is larger than the age of the star. Our determination of vsinI(*) is a rare case in which rotational line broadening has been isolated from other broadening mechanisms. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. Univ Tokyo, Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 51, Cambridge, MA 02138 USA. RI Butler, Robert/B-1125-2009; Turner, Edwin/A-4295-2011; OI Charbonneau, David/0000-0002-9003-484X NR 45 TC 211 Z9 213 U1 1 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 OCT 1 PY 2005 VL 631 IS 2 BP 1215 EP 1226 DI 10.1086/432571 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300045 ER PT J AU Hasan, SS van Ballegooijen, AA Kalkofen, W Steiner, O AF Hasan, SS van Ballegooijen, AA Kalkofen, W Steiner, O TI Dynamics of the solar magnetic network: Two-dimensional MHD simulations SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; sun : chromosphere; sun : magnetic fields; sun : oscillations ID LONGITUDINAL-TRANSVERSE WAVES; PHOTOSPHERIC FLUX TUBES; BRIGHT POINTS; CHROMOSPHERIC NETWORK; MODE TRANSFORMATION; ALFVEN WAVES; OSCILLATIONS; ATMOSPHERE; PROPAGATION; SUN AB The aim of this work is to identify the physical processes that occur in the network and contribute to its dynamics and heating. We model the network as consisting of individual flux tubes, each with a nonpotential field structure, that are located in intergranular lanes. With a typical horizontal size of about 150 km at the base of the photosphere, they expand upward and merge with their neighbors at a height of about 600 km. Above a height of approximately 1000 km the magnetic field starts to become uniform. Waves are excited in this medium by means of motions at the lower boundary. We focus on transverse driving, which generates both fast and slow waves within a flux tube and acoustic waves at the interface of the tube and the ambient medium. The acoustic waves at the interface are due to compression of the gas on one side of the flux tube and expansion on the other. These longitudinal waves are guided upward along field lines at the two sides of the flux tube, and their amplitude increases with height due to the density stratification. Being acoustic in nature, they produce a compression and significant shock heating of the plasma in the chromospheric part of the flux tube. For impulsive excitation with a time constant of 120 s, we find that a dominant feature of our simulations is the creation of vortical motions that propagate upward. We have identified an efficient mechanism for the generation of acoustic waves at the tube edge, which is a consequence of the sharp interface of the flux concentration. We examine some broad implications of our results. C1 Indian Inst Astrophys, Bangalore 560034, Karnataka, India. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Kiepenheuer Inst Sonnenphys, D-7800 Freiburg, Germany. RP Hasan, SS (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. EM hasan@iiap.res.in RI Hasan, Siraj/C-2927-2012; OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 36 TC 49 Z9 49 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 OCT 1 PY 2005 VL 631 IS 2 BP 1270 EP 1280 DI 10.1086/432655 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EU UT WOS:000232365300049 ER PT J AU Ulmschneider, P Rammacher, W Musielak, ZE Kalkofen, W AF Ulmschneider, P Rammacher, W Musielak, ZE Kalkofen, W TI On the validity of acoustically heated chromosphere models SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : numerical; stars : chromospheres; waves ID CORONAL HEATING MECHANISMS; SOLAR CHROMOSPHERE; WAVE-PROPAGATION; ATMOSPHERE; STARS; IONIZATION; DYNAMICS; FLUXES; SUN AB Theoretical models of solar and stellar chromospheres heated by acoustic waves have so far been constructed by using time-dependent, one-dimensional, radiation-hydrodynamic numerical codes that are based on the approximation of plane-parallel geometry. The approach seems to be justified by the fact that the chromospheres of most stars extend over very narrow height ranges compared to the stellar radius. It is demonstrated that this commonly used assumption may lead to unrealistic shock mergings, to the artificial formation of unusually strong shocks and the artificial destruction of high-frequency acoustic wave power. Comparing one-dimensional calculations with observations may lead to severe misjudgment about the nature of chromospheric heating. C1 Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. Univ Texas, Dept Phys, Arlington, TX 76019 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heidelberg Univ, Inst Theoret Astrophys, Albert Uberlestr 2, D-69120 Heidelberg, Germany. EM ulmschneider@ita.uni-heidelberg.de; rammacher@kis.uni-freiburg.de; zmusielak@uta.edu; wolf@cfa.harvard.edu NR 35 TC 19 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2005 VL 631 IS 2 BP L155 EP L158 DI 10.1086/497395 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971EX UT WOS:000232365700014 ER PT J AU Getman, KV Flaccomio, E Broos, PS Grosso, N Tsujimoto, M Townsley, L Garmire, GP Kastner, J Li, J Harnden, FR Wolk, S Murray, SS Lada, CJ Muench, AA McCaughrean, MJ Meeus, G Damiani, F Micela, G Sciortino, S Bally, J Hillenbrand, LA Herbst, W Preibisch, T Feigelson, ED AF Getman, KV Flaccomio, E Broos, PS Grosso, N Tsujimoto, M Townsley, L Garmire, GP Kastner, J Li, J Harnden, FR Wolk, S Murray, SS Lada, CJ Muench, AA McCaughrean, MJ Meeus, G Damiani, F Micela, G Sciortino, S Bally, J Hillenbrand, LA Herbst, W Preibisch, T Feigelson, ED TI Chandra Orion Ultradeep Project: Observations and source lists SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : individual (Orion Nebula, OMC-1); open clusters and associations : individual (Orion Nebula Cluster); stars : early-type; stars : pre-main-sequence; X-rays : stars ID PRE-MAIN-SEQUENCE; CCD IMAGING SPECTROMETER; COUNTING DETECTOR IMAGES; X-RAY SPECTROSCOPY; NEBULA CLUSTER; TRAPEZIUM CLUSTER; WAVELET TRANSFORMS; MASS FUNCTION; BROWN DWARFS; STARS AB We present a description of the data reduction methods and the derived catalog of more than 1600 X-ray point sources from the exceptionally deep 2003 January Chandra X-Ray Observatory ( Chandra) observation of the Orion Nebula Cluster and embedded populations around OMC-1. The observation was obtained with Chandra's Advanced CCD Imaging Spectrometer (ACIS) and has been nicknamed the Chandra Orion Ultradeep Project ( COUP). With an 838 ks exposure made over a continuous period of 13.2 days, the COUP observation provides the most uniform and comprehensive data set on the X-ray emission of normal stars ever obtained in the history of X-ray astronomy. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. INAF, Oservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy. Univ Grenoble 1, Lab Astrophys Grenoble, F-38041 Grenoble, France. Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. RP Getman, KV (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. OI Flaccomio, Ettore/0000-0002-3638-5788; Micela, Giuseppina/0000-0002-9900-4751; Muench, August/0000-0003-0666-6367; Wolk, Scott/0000-0002-0826-9261; Damiani, Francesco/0000-0002-7065-3061 NR 58 TC 244 Z9 244 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2005 VL 160 IS 2 BP 319 EP 352 DI 10.1086/432092 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969YC UT WOS:000232270900001 ER PT J AU Feigelson, ED Getman, K Townsley, L Garmire, G Preibisch, T Grosso, N Montmerle, T Muench, A McCaughrean, M AF Feigelson, ED Getman, K Townsley, L Garmire, G Preibisch, T Grosso, N Montmerle, T Muench, A McCaughrean, M TI Global X-ray properties of the Orion Nebula region SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : individual (Orion Nebula); open clusters and associations : general; open clusters and associations : individual (Orion Nebula Cluster); stars : formation; stars : pre-main-sequence; X-rays : stars ID YOUNG STELLAR OBJECTS; EARLY-TYPE STARS; ULTRADEEP PROJECT; CHANDRA; CLUSTER; EMISSION; POPULATION; ABSORPTION; EVOLUTION; ASTRONOMY AB Based on the Chandra Orion Ultradeep Project ( COUP) observation, we establish the global X-ray properties of the stellar population associated with the Orion Nebula. Three components contribute roughly equally to the integrated COUP luminosity in the hard ( 2 - 8 keV) X-ray band: several OB stars, 822 lightly obscured cool stars in the Orion Nebula Cluster ( ONC), and 559 heavily obscured stars. ONC stars 0.5 - 2 pc from the center show a spatial asymmetry consistent with violent relaxation in the stellar dynamics. The obscured COUP sources concentrate around both OMC-1 molecular cores; these small-scale structures indicate ages t less than or similar to 0.1 Myr. The X-ray luminosity function (XLF) of the lightly obscured sample is roughly lognormal in shape. The obscured population is deficient in lower luminosity stars, perhaps due to localized circumstellar material. Mass-stratified XLFs show that one-third of the Orion Nebula region hard-band emission is produced by the bright O6 star theta(1) Ori C and half is produced by lower mass pre-main-sequence stars with masses 0.3 M(.) < M < 3 M(.). Very low mass stars contribute little to the cluster X-ray emission. Using the hard band emission, we show that young stellar clusters like the ONC can be readily detected and resolved with Chandra across the Galactic disk, even in the presence of heavy obscuration. The Orion Nebula sample is a valuable template for studies of distant clusters. For example, the peak of the XLF shape can serve as a standard candle for a new distance measure to distant young stellar clusters, and the presence of a neon emission line complex around 1 keV can serve as a diagnostic for young stars. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Grenoble 1, Lab Astrophys Grenoble, F-38041 Grenoble, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. RP Feigelson, ED (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. NR 41 TC 152 Z9 152 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2005 VL 160 IS 2 BP 379 EP 389 DI 10.1086/432512 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969YC UT WOS:000232270900003 ER PT J AU Wolk, SJ Harnden, FR Flaccomio, E Micela, G Favata, F Shang, H Feigelson, ED AF Wolk, SJ Harnden, FR Flaccomio, E Micela, G Favata, F Shang, H Feigelson, ED TI Stellar activity on the young suns of Orion: COUP observations of K5-7 pre-main-sequence stars SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE meteors, meteoroids; open clusters and associations : individual (Orion Nebula Cluster); stars : activity; stars : pre-main-sequence; Sun : activity; X-rays : stars ID EARLY SOLAR-SYSTEM; X-RAY-EMISSION; SHORT-LIVED NUCLIDES; TIME-SERIES ANALYSIS; NEBULA CLUSTER; EXTINCT RADIOACTIVITIES; EXTREME-ULTRAVIOLET; ENERGY-DISTRIBUTION; COSMIC-RAYS; VARIABILITY AB In 2003 January, the Chandra Orion Ultradeep Project ( COUP) detected about 1400 young stars during a 13.2 day observation of the Orion Nebula Cluster ( ONC). This paper is a study of the X-ray properties of a well-defined sample of 28 solar-mass ONC stars based on COUP data. Our goals are to characterize the magnetic activity of analogs of the young Sun and thereby to improve understanding of the effects of solar X-rays on the solar nebula during the era of planet formation. Given the length of the COUP observation we are able to clearly distinguish characteristic and flare periods for all stars. We find that active young suns spend 70% of their time in a characteristic state with relatively constant flux and magnetically confined plasma with temperatures kT(2) similar or equal to 2.1 x kT(1). During characteristic periods, the 0.5 - 8 keV X-ray luminosity is about 0.03% of the bolometric luminosity. One or two powerful flares per week with peak luminosities log L-X similar to 30 32 ergs s(-1) are typically superposed on this characteristic emission accompanied by heating of the hot plasma component from similar or equal to 2.4 to similar or equal to 7 keVat the flare peak. The energy distribution of flares superposed on the characteristic emission level follows the relationship dN/dE proportional to E-1.7. The flare rates are consistent with the production of sufficiently energetic protons to spawn a spallogenic origin of some important short-lived radionuclides found in ancient meteorites. The X-rays can ionize gas in the circumstellar disk at a rate of 6 x 10(-9) ionizations per second at 1 AU from the central star, orders of magnitude above cosmic-ray ionization rates. The estimated energetic particle fluences are sufficient to account for many isotopic anomalies observed in meteoritic inclusions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAF, Osservatorio Astron GS Vaiana, I-90134 Palermo, Italy. European Space Technol Ctr, European Space Agcy, Res & Space Sci Support Dept, Div Astrophys, NL-2200 AG Noordwijk, Netherlands. Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM swolk@cfa.harvard.edu OI Flaccomio, Ettore/0000-0002-3638-5788; Micela, Giuseppina/0000-0002-9900-4751; Wolk, Scott/0000-0002-0826-9261 NR 74 TC 134 Z9 134 U1 0 U2 2 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 OCT PY 2005 VL 160 IS 2 BP 423 EP 449 DI 10.1086/432099 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969YC UT WOS:000232270900006 ER PT J AU Flaccomio, E Micela, G Sciortino, S Feigelson, ED Herbst, W Favata, F Harnden, FR Vrtilek, SD AF Flaccomio, E Micela, G Sciortino, S Feigelson, ED Herbst, W Favata, F Harnden, FR Vrtilek, SD TI Rotational modulation of X-ray emission in Orion Nebula young stars SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE open clusters and associations : individual (Orion Nebula Cluster); stars : activity; stars : low-mass, brown dwarfs; stars : pre-main-sequence; X-rays : stars ID T-TAURI STARS; MAIN-SEQUENCE STARS; STELLAR CORONAE; ACCRETION; CLUSTER; VARIABILITY; POPULATION; PROTOSTARS; ASTRONOMY; REGIONS AB We investigate the spatial distribution of X-ray-emitting plasma in a sample of young Orion Nebula Cluster stars by modulation of their X-ray light curves due to stellar rotation. The study, part of the Chandra Orion Ultradeep Project ( COUP), is made possible by the exceptional length of the observation: 10 days of ACIS integration during a time span of 13 days, yielding a total of 1616 detected sources in the 17' x 17' field of view. We here focus on a sub-sample of 233 X-ray-bright stars with known rotational periods. We search for X-ray modulation using the Lomb Normalized Periodogram method. X-ray modulation related to the rotation period is detected in at least 23 stars with periods between 2 and 12 days and relative amplitudes ranging from 20% to 70%. In 16 cases, the X-ray modulation period is similar to the stellar rotation period, while in 7 cases it is about half that value, possibly due to the presence of X-ray-emitting structures at opposite stellar longitudes. These results constitute the largest sample of low-mass stars in which X-ray rotational modulation has been observed. The detection of rotational modulation indicates that the X-ray-emitting regions are distributed inhomogeneneously in longitude and do not extend to distances significantly larger than the stellar radius. Modulation is observed in stars with saturated activity levels (L-X/ L-bol similar to 10(-3)) showing that saturation is not due to the filling of the stellar surface with X-ray-emitting regions. C1 INAF, Osservatorio Astron Palermo Giuseppe S Vaiana, I-90134 Palermo, Italy. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. European Space Agcy, Res & Sci Support Dept, Div Astrophys, NL-2200 AG Noordwijk, Netherlands. Smithsonian Astrophys Lab, Cambridge, MA 02138 USA. NASA Headquarters, Universe Div, Sci Mission Directorate, Washington, DC USA. RP Flaccomio, E (reprint author), INAF, Osservatorio Astron Palermo Giuseppe S Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy. EM ettoref@astropa.unipa.it OI Flaccomio, Ettore/0000-0002-3638-5788 NR 48 TC 59 Z9 59 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2005 VL 160 IS 2 BP 450 EP 468 DI 10.1086/432419 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969YC UT WOS:000232270900007 ER PT J AU Grosso, N Feigelson, ED Getman, KV Townsley, L Broos, P Flaccomio, E McCaughrean, MJ Micela, G Sciortino, S Bally, J Smith, N Muench, AA Garmire, GP Palla, F AF Grosso, N Feigelson, ED Getman, KV Townsley, L Broos, P Flaccomio, E McCaughrean, MJ Micela, G Sciortino, S Bally, J Smith, N Muench, AA Garmire, GP Palla, F TI Chandra Orion Ultradeep Project census of X-ray stars in the BN-KL and OMC-1S regions SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE infrared : stars; open clusters and associations : individual (Orion BN-KL, Orion OMC-1S); stars : flare; stars : pre-main-sequence; X-rays : stars ID BECKLIN-NEUGEBAUER OBJECT; MAIN-SEQUENCE STARS; NEBULA-CLUSTER; MOLECULAR CLOUD; CIRCUMSTELLAR DISKS; TRAPEZIUM CLUSTER; YOUNG STARS; RESOLUTION MAPS; FORMING REGION; DUST EMISSION AB We present a study of the X-ray sources detected in the vicinity of two density peaks in the Orion Molecular Cloud 1 (OMC-1) behind the Orion Nebula Cluster ( ONC), as seen in the exceptionally deep ( similar to 10 days) exposure of the Chandra Orion Ultradeep Project ( COUP). We focus on a 4000; 5000 region around the Becklin-Neugebauer object and Kleinmann-Low nebula ( collectively BN-KL) and a 6000; 7500 region around OMC-1S, a secondary star-forming peak some 9000 south of BN-KL. A total of 43 and 60 X-ray sources were detected in BN-KL and OMC-1S, respectively, of which one-half and one-third, respectively, were found to be foreground members of the ONC, while the remaining sources are identified as obscured X-ray sources with column densities 22 less than or similar to log (N(H)/cm(-2)) less than or similar to 24. All but 5 and 18 of these sources have near-infrared stellar counterparts, and 22 of these appear to be young stellar objects (YSOs). X-ray sources are found close to four luminous mid-IR sources, namely, BN, IRc3-i2, IRc2-C, and source n; their X-ray variability and spectral properties are typical of coronal activity in low-mass stars rather than wind emission from massive stars, suggesting that the X-ray emission may be arising from companions. The X-ray light curve of the X-ray source close to BN shows a periodicity of similar to 8.3 days, and from an X-ray image deconvolution of the region around BN, we conclude that either BN itself or a low-mass companion with a projected separation of similar or equal to 200 AU was detected. On the other hand, no emission is seen from the bright radio source I, held by some to be the main source of luminosity in BN-KL. In OMC-1S, Chandra unveils a new subcluster of seven YSOs without infrared counterparts. We compare the hard-band X-ray luminosity functions of obscured X-ray sources in BN-KL and OMC-1S with unobscured X-ray sources in the ONC, and we estimate that the true population of obscured sources in BN-KL and OMC- 1S is similar or equal to 46 and 57 stars, with 90% confidence intervals of 34 - 71 and 42 - 82 stars, respectively. C1 Univ Grenoble 1, Lab Astrophys Grenoble, F-38041 Grenoble, France. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. RP Grosso, N (reprint author), Univ Grenoble 1, Lab Astrophys Grenoble, F-38041 Grenoble, France. EM nicolas.grosso@obs.ujf-grenoble.fr OI palla, francesco/0000-0002-3321-0456; Flaccomio, Ettore/0000-0002-3638-5788 NR 73 TC 45 Z9 45 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2005 VL 160 IS 2 BP 530 EP 556 DI 10.1086/432101 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 969YC UT WOS:000232270900011 ER PT J AU James, HF AF James, HF TI Paleogene fossils and the radiation of modern birds SO AUK LA English DT Article ID MIDDLE EOCENE; TERTIARY BIRDS; MESSEL GERMANY; RECORD; AVES; EVOLUTION; PHYLOGENY; OLIGOCENE; BRACHYPTERACIIDAE; HUMMINGBIRDS C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. RP James, HF (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, MRC-116, Washington, DC 20013 USA. EM jamesh@si.edu NR 54 TC 18 Z9 19 U1 0 U2 8 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2005 VL 122 IS 4 BP 1049 EP 1054 DI 10.1642/0004-8038(2005)122[1049:PFATRO]2.0.CO;2 PG 6 WC Ornithology SC Zoology GA 987HO UT WOS:000233509200002 ER PT J AU Rappole, JH Renner, SC Shwe, NM Sweet, PR AF Rappole, JH Renner, SC Shwe, NM Sweet, PR TI A new species of Scimitar-Babbler (Timaliidae : Jabouilleia) from the sub-himalayan region of Myanmar SO AUK LA English DT Article DE Jabouilleia naungmungensis; Myanmar; Naung Mung Scimitar-Babbler; new species; Timaliidae AB An expedition of representatives from the Myanmar Nature and Wildlife Conservation Division and the Smithsonian National Zoological Park's Conservation and Research Center visited the town of Naung Mung on the Nam Tisang River in the extreme northern portion of Kachin State, Myanmar, during February 2004. The town is located in the sub-Himalayan region of the country at 27 degrees 29'N, 97 degrees 48'E, elevation 540 m, 118 km south of the Tibetan border and 53 km west of the border with Yunnan Province, China. The purpose of the trip was to inventory the poorly known avifauna of the premontane temperate rainforest habitat at that site. On 6 February 2004, we captured two scimitar-babblers that appeared to be representatives of the genus Jabouilleia. An additional individual of the taxon was captured in the same vicinity on 8 February 2004. These were the first records for jabouilleia from Myanmar, and subsequent investigation showed that these specimens were members of a previously undescribed species, which we designate Jabouilleia naungmungensis, the Naung Mung Scimitar-Babbler. C1 Conservat & Res Ctr, Front Royal, VA 22630 USA. Dept Forestry, Nat & Wildlife Conservat Div, W Gyogone Insein Yangon, Myanmar. Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA. RP Rappole, JH (reprint author), Conservat & Res Ctr, Smithsonian Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM rappolej@crc.si.edu RI Renner, Swen/J-3502-2014 OI Renner, Swen/0000-0002-6893-4219 NR 11 TC 7 Z9 14 U1 0 U2 0 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2005 VL 122 IS 4 BP 1064 EP 1069 DI 10.1642/0004-8038(2005)122[1064:ANSOST]2.0.CO;2 PG 6 WC Ornithology SC Zoology GA 987HO UT WOS:000233509200004 ER PT J AU Maldonado, M Cortadellas, N Trillas, MI Rutzler, K AF Maldonado, M Cortadellas, N Trillas, MI Rutzler, K TI Endosymbiotic yeast maternally transmitted in a marine sponge SO BIOLOGICAL BULLETIN LA English DT Article ID CORAL-REEF SPONGES; CHONDRILLA-NUCULA; MICROBIAL ASSOCIATIONS; ELECTRON-MICROSCOPE; CYANOBACTERIAL SYMBIONT; FUSARIUM-OXYSPORUM; COLLOIDAL GOLD; DEMOSPONGIAE; BACTERIA; LOCALIZATION AB The detection of an endosymbiotic yeast in demosponges of the genus Chondrilla described here records the first such association within the phylum Porifera. The symbiont, interpreted as a yolk body in previous ultrastructural studies, is a chitinous-walled fission yeast. Chitin was detected by an immunocytochemical technique that labels its beta-1,4-N-acetyl-D-glucosamine residues. Abundant symbiotic yeast cells (4.4 +/- 2.3 cells per 10 mu m(2)) transmitted from the soma through the oocytes to the fertilized eggs are directly propagated by vertical transmission in the female. Vertically transmitted yeast were detected in three Chondrilla species with disjunct biogeographical distributions: the Mediterranean, the Caribbean, and the Australian Pacific. Apparently these yeasts are not present in other demosponge genera. Therefore, the fungal endosymbiosis most likely evolved before or during the diversification of the genus Chondrilla. C1 CSIC, Ctr Estudios Avanzados Blanes, Dept Aquat Ecol, E-17300 Blanes, Girona, Spain. Univ Barcelona, Serv Cient Tecn, E-08028 Barcelona, Spain. Univ Barcelona, Fac Biol, Dept Biol Vegetal, E-08028 Barcelona, Spain. Smithsonian Inst, MRC 163, CCRE, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Maldonado, M (reprint author), CSIC, Ctr Estudios Avanzados Blanes, Dept Aquat Ecol, Acceso Cala St Francesc 14, E-17300 Blanes, Girona, Spain. EM maldonado@ceab.csic.es RI Maldonado, Manuel/J-9331-2012; Trillas, M Isabel/L-8334-2014 NR 32 TC 52 Z9 52 U1 0 U2 12 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 OCT PY 2005 VL 209 IS 2 BP 94 EP 106 DI 10.2307/3593127 PG 13 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 981FO UT WOS:000233073100002 PM 16260769 ER PT J AU Fu, YB Coulman, BE Ferdinandez, YSN Cayouette, J Peterson, PM AF Fu, YB Coulman, BE Ferdinandez, YSN Cayouette, J Peterson, PM TI Genetic diversity of fringed brome (Bromus ciliatus) as determined by amplified fragment length polymorphism SO CANADIAN JOURNAL OF BOTANY-REVUE CANADIENNE DE BOTANIQUE LA English DT Article DE native grass; fringed brome; genetic variation; AFLP; habitat restoration ID AFLP MARKERS; WHEATGRASS CULTIVARS; NATURAL-POPULATIONS; WESTERN CANADA; BLUESTEM; DISTANCE; FLOW; RAPD AB Fringed brome (Bromus ciliatus L.) is found in native stands throughout a large area of North America. Little is known about the genetic diversity of this species. The amplified fragment length polymorphism (AFLP) technique was applied to assess the genetic diversity of 16 fringed brome populations sampled in Canada from the provinces of Alberta, British Columbia, Quebec, and Saskatchewan. Four AFLP primer pairs were employed to screen 82 samples with four to six samples per population and 83 polymorphic AFLP bands scored for each sample. The frequencies of the scored bands in all assayed samples ranged from 0.01 to 0.99 and averaged 0.53. Analysis of molecular variance revealed that 52.6% of the total AFLP variation resided among the 16 populations and 20.6% among the four provinces. The five Quebec populations appeared to be genetically the most diverse and distinct. The AFLP variability observed was significantly associated with the geographic origins of the fringed brome populations. These findings are useful for sampling fringed brome germplasm from natural populations for germplasm conservation and should facilitate the development of genetically diverse regional cultivars for habitat restoration and revegetation. C1 Agr & Agri Food Canada, Saskatoon Res Ctr, Saskatoon, SK S7N 0X2, Canada. Agr & Agri Food Canada, Natl Program Environm Hlth Biodivers, Ottawa, ON K1A 0C6, Canada. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Coulman, BE (reprint author), Agr & Agri Food Canada, Saskatoon Res Ctr, 107 Sci Pl, Saskatoon, SK S7N 0X2, Canada. EM bruce.coulman@usask.ca NR 44 TC 6 Z9 8 U1 0 U2 1 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4026 J9 CAN J BOT JI Can. J. Bot.-Rev. Can. Bot. PD OCT PY 2005 VL 83 IS 10 BP 1322 EP 1328 DI 10.1139/b05-112 PG 7 WC Plant Sciences SC Plant Sciences GA 010YH UT WOS:000235233400011 ER PT J AU Chance, K AF Chance, K TI Ultraviolet and visible spectroscopy and spaceborne remote sensing of the Earth's atmosphere SO COMPTES RENDUS PHYSIQUE LA English DT Article DE ultraviolet spectroscopy; visible spectroscopy; atmospheric remote sensing; stratospheric composition; tropospheric composition; radiative transfer modeling; chemistry and transport modeling ID RADIATIVE-TRANSFER MODEL; ROTATIONAL RAMAN-SCATTERING; OZONE MONITORING EXPERIMENT; CHEMICAL-TRANSPORT MODEL; RAYLEIGH-SCATTERING; STRATOSPHERIC NO2; SATELLITE; RETRIEVAL; PROFILES; EMISSIONS AB Current capabilities for ultraviolet and visible spectroscopic measurements of the Earth's stratosphere and troposphere are reviewed. Atmospheric spectral properties are described. The major measurement geometries and types are presented. Instrumental, spectroscopic, and radiative transfer modeling challenges are discussed. Current and planned satellite instruments for this field, with their measurement properties, spectral coverage, and target molecules are presented. Measurement examples include stratospheric and tropospheric NO(2), tropospheric BrO in the polar spring, global tropospheric HCHO, and tropospheric ozone measurements from the nadir geometry. The field is shown to be sufficiently mature that global measurements of atmospheric pollution from space may be undertaken. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM kchance@cfa.harvard.edu OI Chance, Kelly/0000-0002-7339-7577 NR 57 TC 8 Z9 9 U1 1 U2 8 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0705 J9 CR PHYS JI C. R. Phys. PD OCT PY 2005 VL 6 IS 8 BP 836 EP 847 DI 10.1016/j.crhy.2005.07.010 PG 12 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA 985PI UT WOS:000233389900004 ER PT J AU Rothman, LS Jacquinet-Husson, N Boulet, C Perrin, AM AF Rothman, LS Jacquinet-Husson, N Boulet, C Perrin, AM TI History and future of the molecular spectroscopic databases SO COMPTES RENDUS PHYSIQUE LA English DT Article DE spectroscopic database; molecular spectroscopy; line shape; absorption parameters; infrared cross-sections; HITRAN; GEISA; MIPAS ID 20 MU-M; COLLISION-INDUCED ABSORPTION; ABSOLUTE BAND INTENSITIES; SPECTRAL-LINE CATALOG; WATER-VAPOR CONTINUUM; INFRARED Q BRANCHES; WING REGIONS; TRACE GASES; ATMOSPHERIC APPLICATIONS; ACETONE (CH3)(2)CO AB A brief history and review of the development of some molecular spectroscopic databases is presented. Such databases are compilations of spectroscopic parameters whose principal purpose is to provide the necessary molecular absorption input for transmission and radiance codes. Remote sensing of the terrestrial atmosphere has advanced significantly in recent years, and this has placed greater demands on the compilations in terms of accuracy, additional species, and spectral coverage. This paper discusses current pressing issues, such as the deficiencies in line positions, intensities, and line shape, as well as the directions of future enhancements. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Ecole Polytech, Meteorol Dynam Lab, F-91128 Palaiseau, France. Univ Paris 12, LISA, F-94010 Creteil, France. Univ Paris 07, LISA, F-94010 Creteil, France. Univ Paris 11, CNRS, Photophys Mol Lab, F-91405 Orsay, France. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 80 TC 16 Z9 16 U1 0 U2 3 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0705 J9 CR PHYS JI C. R. Phys. PD OCT PY 2005 VL 6 IS 8 BP 897 EP 907 DI 10.1016/j.crhy.2005.09.001 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA 985PI UT WOS:000233389900009 ER PT J AU Aronson, RB MacIntyre, IG Lewis, SA Hilbun, NL AF Aronson, RB MacIntyre, IG Lewis, SA Hilbun, NL TI Emergent zonation and geographic convergence of coral reefs SO ECOLOGY LA English DT Article DE Acropora; Agaricia; Belize; beta diversity; biotic homogenization; coral reef; Holocene; paleoecology; Panama; phase shift; Porites; species turnover ID BOCAS DEL TORO; INTERMEDIATE DISTURBANCE HYPOTHESIS; BIOTIC HOMOGENIZATION; GAMMA-DIVERSITY; PHASE-SHIFTS; BELIZE; SCALE; PATTERNS; SYSTEMS; BIODIVERSITY AB Environmental degradation is reducing the variability of living assemblages at multiple spatial scales, but there is no a priori reason to expect biotic homogenization to occur uniformly across scales. This paper explores the scale-dependent effects of recent perturbations on the biotic variability of lagoonal reefs in Panama and Belize. We used new, and previously published core data to compare temporal patterns of species dominance between depth zones and between geographic locations. After millennia of monotypic dominance, depth zonation emerged for different reasons in the two reef systems, increasing the between-habitat component of beta diversity in both taxonomic and functional terms. The increase in between-habitat diversity caused a decline in geographic-scale variability as the two systems converged on a single, historically novel pattern of depth zonation. Twenty-four reef cores were extracted at water depths above 2 in in Bahia Almirante, a coastal lagoon in northwestern Panama. The cores showed that finger corals of the genus Porites dominated for the last 2000-3000 yr. Porites remained dominant as the shallowest portions of the reefs grew to within 0.25 in of present sea level. At intermediate depths of 5-10 m, however, declining water quality in the Bahia enabled the lettuce coral Agaricia tenuifolia to replace Porites during the last several decades. In Belize, the staghorn coral Acropora cervicornis dominated the rhomboid shoals of the central shelf lagoon for millennia. As the shallowest portions of the rhomboid shoals approached sea level around 500 years ago, Porites spp. replaced Ac. cervicornis in an intrinsically driven successional sequence. At intermediate depths, white-band disease killed Ac. cervicornis in the late 1980s, precipitating a transition to dominance by Ag. tenuifolia. Phase shifts between coral taxa and the emergence of coral zonation in both locations were mediated by the sea urchin Echinometra viridis, which controlled algal growth. Opposite trends in biotic variability at the habitat and geographic levels highlight the complex, scale-deperident nature of the response of coral reefs to intense perturbations. C1 Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. Univ S Alabama, Dept Marine Sci, Mobile, AL 36688 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Aronson, RB (reprint author), Dauphin Isl Sea Lab, 101 Bienville Blvd, Dauphin Isl, AL 36528 USA. EM raronson@disl.org NR 76 TC 31 Z9 33 U1 2 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 OCT PY 2005 VL 86 IS 10 BP 2586 EP 2600 DI 10.1890/05-0045 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 971DP UT WOS:000232361800005 ER PT J AU Coley, PD Lokvam, J Rudolph, K Bromberg, K Sackett, TE Wright, L Brenes-Arguedas, T Dvorett, D Ring, S Clark, A Baptiste, C Pennington, RT Kursar, TA AF Coley, PD Lokvam, J Rudolph, K Bromberg, K Sackett, TE Wright, L Brenes-Arguedas, T Dvorett, D Ring, S Clark, A Baptiste, C Pennington, RT Kursar, TA TI Divergent defensive strategies of young leaves in two species of inga SO ECOLOGY LA English DT Article DE Burro Colorado Island; bioassays; flavanoids; Heliothis; herbivory; Inga; leaf development; non-protein amino acids; Phoebis; plant defenses ID TROPICAL UNDERSTORY COMMUNITY; LEAF DEVELOPMENT; ANTIHERBIVORE DEFENSES; CHLOROPLAST DNA; TRADE-OFFS; HERBIVORY; COEVOLUTION; PLANTS; GLUCOSIDES; CALLIANDRA AB (I)n the recently radiated genus Inga (Fabaceae), few nucleotide substitutions have accumulated among species, yet large divergences have occurred in defensive phenotypes, suggesting strong selection by herbivores. We compared herbivory and defenses of young leaves for L goldmanii, a more derived species that follows a "defense" strategy, and L unibellifera, a more basal species that follows an "escape" strategy. The two species suffered similar rates of herbivory (22% of the leaf area eaten during expansion) but were attacked by different communities of herbivores. I. goldinanii relied heavily on extra-floral nectaries and on a diversity of effective secondary metabolites, while I. umbellfera minimized damage through rapid leaf expansion and synchronous flushing. The major classes of secondary compounds in both species were flavanoids and non-protein amino acids; however, there were large differences in structure, biosynthetic pathways, and efficacy against herbivores. Growth rates of lepidopteran larvae were significantly lower when fed artificial diets with crude extracts from L goldmanii as compared to L umbellifera. Flavanoids accounted for the majority of growth reduction in both species. L umbellifera had more unusual flavanoids and a non-protein amino acid not reported from plants, but the more common flavanoids found in L goldinanii were more bioactive against herbivores. I. goldmanii also had greater ant visitation to extrafloral nectaries, suggesting that there was no trade-off between biotic and chemical defenses. In contrast, young leaves of L umbellifera expanded more rapidly, minimizing the window of vulnerability before toughening. Resources for rapid expansion may have been reallocated from chloroplast development as L umbellifera delayed the greening process until after full leaf expansion. Leaves were also produced synchronously, which can satiate herbivores and reduce damage. These defense differences are reflected in almost completely nonoverlapping herbivore faunas and the more frequent occurrence of generalists on L umbellifera. To understand why defenses have evolved, it is important to view them in light of the herbivore community as well as in the context of the other co-occurring traits. We hypothesize that the effectiveness of chemical defenses determines whether a species follows the evolutionary path of "defense" or "escape" strategies. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Panama. McGill Univ, Dept Nat Resources Sci, Ste Anne De Bellevue, PQ, Canada. Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. RP Coley, PD (reprint author), Univ Utah, Dept Biol, 257 S 1400 E, Salt Lake City, UT 84112 USA. EM coley@biology.utah.edu RI Gedan, Keryn/A-3575-2010; Sackett, Tara/L-8910-2013 OI Gedan, Keryn/0000-0003-4020-5441; Sackett, Tara/0000-0002-3615-4170 NR 53 TC 35 Z9 39 U1 2 U2 34 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 OCT PY 2005 VL 86 IS 10 BP 2633 EP 2643 DI 10.1890/04-1283 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 971DP UT WOS:000232361800009 ER PT J AU Bourg, NA McShea, WJ Gill, DE AF Bourg, NA McShea, WJ Gill, DE TI Putting a cart before the search: Successful habitat prediction for a rare forest herb SO ECOLOGY LA English DT Article DE Appalachians; CART; classification tree; conservation; fire; GIS; habitat models; Melanthiaceae; metapopulations; rare plants; species distributions; Xerophyllum asphodeloides ID REGRESSION TREE ANALYSIS; GREAT-SMOKY-MOUNTAINS; GENETIC DIVERSITY; DECISION-TREE; GEOMORPHOLOGICAL HETEROGENEITY; CLASSIFICATION TREES; POPULATION VIABILITY; PINUS-PUNGENS; FIRE HISTORY; OAK FORESTS AB The realms of rare species conservation and metapopulation biology theory are often interrelated, and hence share several basic challenges. Two of the most important are the critical and frequently difficult tasks of distinguishing a priori between habitat and nonhabitat, and then delimiting suitable habitat patches in a study area. We combined classification tree analysis, a subset of classification and regression tree (CART) modeling, with digital data layers of environmental variables in a geographic information system (GIS) to predict suitable habitat and potential new population occurrences for turkeybeard (Xerophyllum asphodeloides), a rare liliaceous understory herb associated with southern Appalachian pine-oak (Pinus-Quercus) forests, in northwestern Virginia. Sample values from eight environmental data layers and population survey data were used in the modeling process to produce a cross-validated classification tree that predicted suitable habitat in the study area. Elevation, slope, forest type, and fire frequency were the four main explanatory variables in the model. Approximately 4% of the study area was classified into five suitable habitat classes, with a misclassification error rate of 4.74%. The final 13-leaf tree correctly classified 74% of the known presence areas and 90% of the known absence areas, and ground-truthing surveys resulted in the discovery of eight new occupied habitat patches. Results of this study are important for conservation and management of X. asphodeloides, as well as for the applicability of the habitat modeling techniques to enhancing the study of metapopulations and disturbance regimes in Appalachian forests. In addition, they confirm the potential and value of CART and GIS-based modeling approaches to species distribution problems. Our model was successful at defining suitable habitat and discovering new populations of a rare species at the landscape scale. Similar application to other rare species could prove very useful for addressing these and other ecological and conservation issues, such as planning transplantation or reintroduction experiments, identifying metapopulation fragmentation thresholds, and formulating conservation strategies. C1 Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Wildlife Conservat Soc, Joint Program Forest Ecol, Conservat Res Ctr, Front Royal, VA 22630 USA. RP Bourg, NA (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM nbourg@umd.edu OI Bourg, Norman/0000-0002-7443-1992 NR 79 TC 80 Z9 87 U1 4 U2 31 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD OCT PY 2005 VL 86 IS 10 BP 2793 EP 2804 DI 10.1890/04-1666 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 971DP UT WOS:000232361800024 ER PT J AU Philpott, SM AF Philpott, SM TI Trait-mediated effects of parasitic phorid flies (Diptera : Phoridae) on ant (Hymenoptera : Formicidae) competition and resource access in coffee agro-ecosystems SO ENVIRONMENTAL ENTOMOLOGY LA English DT Article DE Azteca instabilis; Pseudacteon sp.; multitrophic interaction; trait-mediated effect; competitive hierarchy ID IMPORTED FIRE ANT; ECOLOGICAL INTERACTIONS; SOLENOPSIS-GEMINATA; PSEUDACTEON; COMMUNITIES; HIERARCHIES; MECHANISMS; PATTERNS; IMPACTS; INVICTA AB Predator effects on prey traits change competitive interactions between prey species affecting resource use. Parasitic phorid flies limit competitive-dominant ant activity, potentially meditating competitive interactions between ant species, changing competitive hierarchies, or affecting ant communities. I considered interactions between phorids (Pseudacteon sp.), their ant host (Azteca instabilis F. Smith), and co-occurring ant species in coffee agro-ecosystems testing whether phorids (1) limit A. instabilis recruitment activity, (2) affect competitive interaction between ant species, and (3) are associated with other species' resource access and therefore have the potential to change competitive hierarchies. I monitored recruitment of A. instabilis and other ants to baits over 90 min on canopy trees with or without phorids. A. instabilis were one-half as abundant with phorids. Other species gained access to baits 12 times more often and were only able to take over baits when phorids were present. Furthermore, many more species (13 versus 2) gained access to resources when phorids were present. These results indicate that phorids mediate competitive interactions between ant species and may influence ant communities by affecting resource availability. Considering that phorids limit A. instabilis attacks on herbivores and that ant species differ in effects on arthropod communities, phorids may have strong community-level effects in coffee agro-ecosystems. C1 Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Philpott, SM (reprint author), Smithsonian Inst, Smithsonian Migratory, Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM philpotts@si.edu RI Philpott, Stacy/F-2330-2011 NR 28 TC 26 Z9 26 U1 0 U2 6 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0046-225X J9 ENVIRON ENTOMOL JI Environ. Entomol. PD OCT PY 2005 VL 34 IS 5 BP 1089 EP 1094 DI 10.1603/0046-225X(2005)034[1089:TEOPPF]2.0.CO;2 PG 6 WC Entomology SC Entomology GA 971SU UT WOS:000232405800015 ER PT J AU Marsh, AS Rasse, DP Drake, BG Megonigal, JP AF Marsh, AS Rasse, DP Drake, BG Megonigal, JP TI Effect of elevated CO2 on carbon pools and fluxes in a brackish marsh SO ESTUARIES LA English DT Article ID CHESAPEAKE BAY WETLAND; DIOXIDE ENRICHMENT; ESTUARINE MARSH; SOIL RESPIRATION; ATMOSPHERIC CO2; TEMPERATURE-DEPENDENCE; NITROGEN DYNAMICS; INORGANIC CARBON; ORGANIC-MATTER; PLANT AB The effects of long-term exposure to elevated atmospheric CO2 (ambient+ 340 ppmv) on carbon cycling were investigated for two plant communities in a Chesapeake Bay brackish marsh, one dominated by the C-3 sedge Schoenoplectus americanus and the other by the C-4 grass Spartina patens. Elevated CO2 resulted in a significant increase in porewater concentrations of DIC at 30 cm depth (p < 0.1). The CO2 treatment also yielded increases in DOC (15 to 27%) and dissolved CH4 (12-18%) in the C-3 marsh (means for several depths over the period of June 1998 and june 1999), but not at a significant level. Elevated CO2 increased mean ecosystem emissions Of CO2 (34-393 g C m(-2) yr(-1)) and CH4 (0.21-0.40 g C m(-2) yr(-1)) in the C-3 community, but the effects were only significant on certain dates. For example, CO2 enrichment increased C export to the atmosphere in the C-3 community during one of two winter seasons measured (p = 0.09). In the C-4 community, gross photosynthesis responded relatively weakly to elevated CO2 (18% increase, p > 0.1), and the concomitant effects on dissolved carbon concentrations, respiration, and CH4 emissions were small or absent. We concluded that elevated CO2 has the potential to increase dissolved inorganic carbon export to estuaries. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. INRA, INA PG, F-78850 Thiverval Grignon, France. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM megonigalp@si.edu OI Daniel, Rasse/0000-0002-5977-3863 NR 47 TC 19 Z9 21 U1 3 U2 20 PU ESTUARINE RES FEDERATION PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0160-8347 J9 ESTUARIES JI Estuaries PD OCT PY 2005 VL 28 IS 5 BP 694 EP 704 DI 10.1007/BF02732908 PG 11 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 985ZT UT WOS:000233418600006 ER PT J AU West-Eberhard, MJ AF West-Eberhard, Mary Jane TI Behavior of the primitively social wasp Montezumia cortesioides Willink (Vespidae Eumeninae) and the origins of vespid sociality SO ETHOLOGY ECOLOGY & EVOLUTION LA English DT Article DE group life; mutualism; mating behavior; intranidal prey theft; monandry; social evolution; progressive provisioning; displacement activity ID INTRASPECIFIC PARASITISM; GENETICAL EVOLUTION; KIN-SELECTION; HYMENOPTERA; INSECTS; CARE AB Montezumia cortesioides is of special interest for studies of insect social evolution because it belongs to the primarily solitary-nesting subfamily (Eumeninae) of wasps that is most closely related to the subfamilies (Stenogastrinae, Polistinae, Vespinae) that contain eusocial species. It is one of a few eumenines that are primitively, social, with more than one reproductive female on the same nest without a division of labor between sterile workers and egg-laying queens. Most of the 17 known progressively provisioning eumenines nest as solitary females, but there is an association between progressive provisioning and nest sharing: all of the three nest-sharing eumenines whose behavior has been observed progressively provision their larvae. Of those species, the behavior of M. cortesioides most closely resembles that of the eusocial (worker-containing) wasps, in nest-sharing, reuse of brood cells, progressive provisioning, and strong aggressive competition among resident females for empty cells. Observations suggest that groups are formed when offspring females remain on the maternal nest. A male repeatedly visited a nest and paired with a newly emerged female. Prey theft from the open cells of nestmates (intranidal prey theft) was associated with episodes of self-grooming and brief repetitive superficial inspections of prey-containing cells. C1 Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Pedro, Costa Rica. RP West-Eberhard, MJ (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Pedro, Costa Rica. EM mjwe@sent.com NR 41 TC 3 Z9 3 U1 0 U2 6 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 OCT PY 2005 VL 17 IS 3 BP 201 EP 215 PG 15 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 115JO UT WOS:000242730800001 ER PT J AU Jiggins, CD Mavarez, J Beltran, M McMillan, WO Johnston, JS Bermingham, E AF Jiggins, CD Mavarez, J Beltran, M McMillan, WO Johnston, JS Bermingham, E TI A genetic linkage map of the mimetic butterfly Heliconius melpomene SO GENETICS LA English DT Article ID MICROSATELLITE LOCI; WARNING-COLOR; ADAPTIVE RADIATION; MULLERIAN MIMICRY; NATURAL-SELECTION; PATTERN-FORMATION; BOMBYX-MORI; EVOLUTION; NYMPHALIDAE; LEPIDOPTERA AB Heliconius melpomene is a mimetic butterfly that exhibits great geographic variation in color pattern. We present here a genetic linkage map based on analysis of genetic markers in 73 individuals from a single F(2) family, offspring of a cross between H. m. cythera. from western Ecuador and H. m. melpomene from French Guiana. A novel "three-step method" is described for the analysis of dominant markers in an F,, cross, using outbred parental strains and taking advantage of the lack of crossing over in female Lepidoptera. This method is likely to prove useful for future mapping studies in outbred species with crossing over restricted to one sex, such as the Lepidoptera and Drosophila. The resulting linkage map has 21 linkage groups corresponding to the 21 chromosomes of H. melpomene and includes 219, AFLP markers, 23 microsatellites, 19 singlecopy nuclear genes, and the color pattern switch genes Yb and Sb. The marker density is high, averaging > 1/7 cM. The total map length is 1616 cM and the average chromosome length is 77 cM. The genome size of H. melpomene was estimated to be 292 Mb, giving a relationship of physical-to-map distance of 180 kb/cM. This map forms the basis for future comparative linkage analysis of color pattern evolution in Heliconius. C1 Univ Edinburgh, Inst Evolutionary Biol, Ashworth Labs, Edinburgh EH9 3JT, Midlothian, Scotland. Smithsonian Trop Res Inst, Balboa, Panama. UCL, Dept Biol, Galton Lab, London NW1 2HE, England. Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. Texas A&M Univ, Dept Entomol, College Stn, TX 77843 USA. RP Jiggins, CD (reprint author), Univ Edinburgh, Inst Evolutionary Biol, Ashworth Labs, W Mains Rd, Edinburgh EH9 3JT, Midlothian, Scotland. EM chris.jiggins@ed.ac.uk RI Jiggins, Chris/B-9960-2008 OI Jiggins, Chris/0000-0002-7809-062X NR 44 TC 74 Z9 77 U1 0 U2 13 PU GENETICS SOC AM PI BETHESDA PA 9650 ROCKVILLE AVE, BETHESDA, MD 20814 USA SN 0016-6731 J9 GENETICS JI Genetics PD OCT PY 2005 VL 171 IS 2 BP 557 EP 570 DI 10.1534/genetics.104.034686 PG 14 WC Genetics & Heredity SC Genetics & Heredity GA 982XF UT WOS:000233194500013 PM 15489522 ER PT J AU Hurt, CR Farzin, M Hedrick, PW AF Hurt, CR Farzin, M Hedrick, PW TI Premating, not postmating, barriers drive genetic dynamics in experimental hybrid populations of the endangered sonoran topminnow SO GENETICS LA English DT Article ID REPRODUCTIVE ISOLATION; GILA TOPMINNOW; CHARACTER DISPLACEMENT; SEXUAL ISOLATION; MHC VARIATION; SPECIATION; DROSOPHILA; EVOLUTION; GENUS; FISH AB The timing and pattern of reproductive barrier formation in allopatric populations has received much less attention than the accumulation of reproductive barriers in sympatry. The theory of allopatric speciation suggests that reproductive barriers evolve simply as by-products of overall genetic divergence. However, observations of enhanced premating barriers in allopatric populations Suggest that sexual selection driven by intraspecific competition for mates may enhance species-specific signals and accelerate the speciation process. In a previous Series of laboratory trials, we examined the strength of premating and postmating barriers in an allopatric species pair of the endangered Sonoran topininnow, Poecifiopsis occidentalis and P. sonofiensis. Behavioral observations provided evidence of asymmetrical assortative mating, while reduced brood sizes and male-biased F, sex ratios Suggest postmating incompatibilities. Here we examine the combined effects of premating and postmating barriers on the genetic makeup of mixed populations, using cytonuclear genotype frequencies of first- and second-generation offspring. Observed genotype frequencies strongly reflect the directional assortative mating observed in behavioral trials, illustrating how isolating barriers that act earlier in the reproductive cycle will have a greater effect on total reproductive isolation and may be more important to speciation than subsequent postmating reproductive barriers. C1 Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. RP Hurt, CR (reprint author), Smithsonian Trop Res Inst, Calzada Amador,Edif 356, Miami, FL 34002 USA. EM carla_asu@yahoo.com RI Hurt, Carla/A-3284-2011 NR 36 TC 9 Z9 9 U1 1 U2 12 PU GENETICS PI BALTIMORE PA 428 EAST PRESTON ST, BALTIMORE, MD 21202 USA SN 0016-6731 J9 GENETICS JI Genetics PD OCT PY 2005 VL 171 IS 2 BP 655 EP 662 DI 10.1534/genetics.105.045591 PG 8 WC Genetics & Heredity SC Genetics & Heredity GA 982XF UT WOS:000233194500020 PM 15972455 ER PT J AU Crumpler, LS Squyres, SW Arvidson, RE Bell, JF Blaney, D Cabrol, NA Christensen, PR DesMarais, DJ Farmer, JD Fergason, R Golombek, MP Grant, FD Grant, JA Greeley, R Hahn, B Herkenhoff, KE Hurowitz, JA Knudson, AT Landis, GA Li, R Maki, J McSween, HY Ming, DW Moersch, JE Payne, MC Rice, JW Richter, L Ruff, SW Sims, M Thompson, SD Tosca, N Wang, A Whelley, P Wright, SP Wyatt, MB AF Crumpler, LS Squyres, SW Arvidson, RE Bell, JF Blaney, D Cabrol, NA Christensen, PR DesMarais, DJ Farmer, JD Fergason, R Golombek, MP Grant, FD Grant, JA Greeley, R Hahn, B Herkenhoff, KE Hurowitz, JA Knudson, AT Landis, GA Li, R Maki, J McSween, HY Ming, DW Moersch, JE Payne, MC Rice, JW Richter, L Ruff, SW Sims, M Thompson, SD Tosca, N Wang, A Whelley, P Wright, SP Wyatt, MB TI Mars Exploration Rover Geologic traverse by the Spirit rover in the Plains of Gusev Crater, Mars SO GEOLOGY LA English DT Article DE Mars; planetary geology; rover; geotraverse; field geology ID SPECTROMETER; ROCKS AB The Spirit rover completed a 2.5 km traverse across gently sloping plains on the floor of Gusev crater from its location on the outer rim of Bonneville crater to the lower slopes of the Columbia Hills, Mars. Using the Athena suite of instruments in a transect approach, a systematic series of overlapping panoramic mosaics, remote sensing observations, surface analyses, and trenching operations documented the lateral variations in landforms, geologic materials, and chemistry of the surface throughout the traverse, demonstrating the ability to apply the techniques of field geology by remote rover operations. Textures and shapes of rocks within the plains are consistent with derivation from impact excavation and mixing of the upper few meters of basaltic lavas. The contact between surrounding plains and crater ejecta is generally abrupt and marked by increases in clast abundance and decimeter-scale steps in relief. Basaltic materials of the plains overlie less indurated and more altered rock types at a time-stratigraphic contact between the plains and Columbia Hills that occurs over a distance of one to two meters. This implies that regional geologic contacts are well preserved and that Earth-like field geologic mapping will be possible on Mars despite eons of overturn by small impacts. C1 New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, SETI, Div Space Sci, Moffett Field, CA 94035 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. US Geol Survey, Flagstaff, AZ 86001 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Ohio State Univ, Dept Civil & Environm Engn, Columbus, OH 43210 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NASA, Johnson Space Ctr, Houston, TX USA. Inst Space Simulat, DLR, Cologne, Germany. RP Crumpler, LS (reprint author), New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. RI Hurowitz, Joel/A-8862-2008; Moersch, Jeffrey/F-7189-2010; Whelley, Patrick/B-9560-2012 OI Whelley, Patrick/0000-0003-3266-9772 NR 21 TC 22 Z9 23 U1 1 U2 5 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD OCT PY 2005 VL 33 IS 10 BP 809 EP 812 DI 10.1130/G21673.1 PG 4 WC Geology SC Geology GA 969RM UT WOS:000232252400013 ER PT J AU Ward, M Dick, CW Gribel, R Lowe, AJ AF Ward, M Dick, CW Gribel, R Lowe, AJ TI To self, or not to self ... A review of outcrossing and pollen-mediated gene flow in neotropical trees SO HEREDITY LA English DT Review DE mating system; gene flow; neotropical trees; pollination; pollen dispersal ID CEIBA-PENTANDRA BOMBACACEAE; TROPICAL RAIN-FOREST; CORDIA-ALLIODORA BORAGINACEAE; MATING SYSTEM; DRY FOREST; BREEDING SYSTEMS; FRENCH-GUIANA; REPRODUCTIVE-BIOLOGY; POPULATION-GENETICS; FLOWERING PHENOLOGY AB Despite the typically low population densities and animal-mediated pollination of tropical forest trees, outcrossing and long-distance pollen dispersal are the norm. We reviewed the genetic literature on mating systems and pollen dispersal for neotropical trees to identify the ecological and phylogenetic correlates. The 36 studies surveyed found >90% outcrossed mating for 45 hermaphroditic or monoecious species. Self-fertilization rates varied inversely with population density and showed phylogenetic and geographic trends. The few direct measures of pollen flow (N = 11 studies) suggest that pollen dispersal is widespread among low-density tropical trees, ranging from a mean of 200 m to over 19 km for species pollinated by small insects or bats. Future research needs to examine (1) the effect of inbreeding depression on observed outcrossing rates, (2) pollen dispersal in a wide range of pollination syndromes and ecological classes, (3) and the range of variation of mating system expression at different hierarchical levels, including individual, seasonal, population, ecological, landscape and range wide. C1 Univ Queensland, Sch Integrat Biol, Brisbane, Qld 4072, Australia. Smithsonian Trop Res Inst, Balboa, Panama. INPA, Manaus, Amazonas, Brazil. RP Ward, M (reprint author), Univ Queensland, Sch Integrat Biol, Brisbane, Qld 4072, Australia. EM s4087128@student.uq.edu.au RI Dick, Christopher/A-8744-2008; Gribel, Rogerio/C-5392-2013 OI Gribel, Rogerio/0000-0002-0850-5578 NR 72 TC 139 Z9 145 U1 3 U2 29 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0018-067X J9 HEREDITY JI Heredity PD OCT PY 2005 VL 95 IS 4 BP 246 EP 254 DI 10.1038/sj.hdy.6800712 PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 968TI UT WOS:000232184900002 PM 16094304 ER PT J AU Hardesty, BD Dick, CW Kremer, A Hubbell, S Bermingham, E AF Hardesty, BD Dick, CW Kremer, A Hubbell, S Bermingham, E TI Spatial genetic structure of Simarouba amara Aubl. (Simaroubaceae), a dioecious, animal-dispersed Neotropical tree, on Barro Colorado Island, Panama SO HEREDITY LA English DT Article DE AFLP; dispersal; spatial genetic structure; microsatellites; tropical forest ID TROPICAL TREE; RAIN-FOREST; POPULATION-STRUCTURE; POLLEN DISPERSAL; SEED DISPERSAL; FRENCH-GUIANA; FLOW; DIVERSITY; DISTANCE; CONSEQUENCES AB Simarouba amara (Simaroubaceae) is a vertebrate-dispersed, insect-pollinated Neotropical tree found in lowland moist forest from upper Mesoamerica to the Amazon basin. We assessed the spatial genetic structure of S. amara within the 50-ha Forest Dynamics Plot on Barro Colorado Island in the Republic of Panama. A total of 300 individuals were genotyped using five microsatellite loci, representing 100 individuals with a dbh >= 10 cm, 100 individuals of 1-10 cm dbh, and 100 individuals of <1 cm dbh. The 200 individuals in the two larger size classes were also genotyped with 155 AFLP loci. Spatial autocorrelation analysis using Moran's Index detected significant genotypic association at the smallest distance classes for 1-10 cm dbh (0-20 m) and 410 cm dbh (0-40 m) size categories. Significant spatial autocorrelations were detected over larger scales (0-140 m) in <1 cm dbh individuals. The relatively weak genetic structure of S. amara, in comparison to other recent studies, may be explained by pollen and seed dispersal over the 50 ha plot, overlapping seed shadows, and postrecruitment mortality. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Univ Georgia, Dept Plant Biol, Athens, GA 30605 USA. INRA Stn Rech Forestieres, Lab Genet Arbres Forestiers, F-33611 Gazinet, France. Univ Michigan, Dept Ecol & Evolut, Ann Arbor, MI 48109 USA. RP Hardesty, BD (reprint author), Univ Georgia, Dept Plant Biol, 2502 Miller Plant Sci, Athens, GA 30602 USA. EM hardesty@plantbio.uga.edu RI Dick, Christopher/A-8744-2008; Hardesty, Britta Denise/A-3189-2011 OI Hardesty, Britta Denise/0000-0003-1948-5098 NR 52 TC 47 Z9 51 U1 1 U2 16 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0018-067X J9 HEREDITY JI Heredity PD OCT PY 2005 VL 95 IS 4 BP 290 EP 297 DI 10.1038/sj.hdy.6800714 PG 8 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 968TI UT WOS:000232184900006 PM 16094303 ER PT J AU Di Fiore, A Fleischer, RC AF Di Fiore, A Fleischer, RC TI Social behavior, reproductive strategies, and population genetic structure of Lagothrix poeppigii SO INTERNATIONAL JOURNAL OF PRIMATOLOGY LA English DT Article DE atelins; woolly monkeys; Lagothrix; social behavior; mating strategies; female competition; PCR; microsatellite; population structure; intragroup relatedness ID ATELES-PANISCUS-CHAMEK; NEW-WORLD PRIMATES; BRACHYTELES-ARACHNOIDES; SPIDER MONKEYS; NATIONAL-PARK; ECOLOGICAL CONSTRAINTS; LAGOTRICHA-POEPPIGII; NEOTROPICAL PRIMATES; ALOUATTA-SENICULUS; MITOCHONDRIAL-DNA AB For species of primates in which females emigrate, we would expect males within groups to be related to one another. Kin selection theory suggests that these males should associate preferentially with one another, be more affiliative and cooperative with one another than females are, and compete less overtly with one another over reproductive opportunities than males in female philopatric taxa do. Precisely these patterns of social behavior characterize well-studied populations of 2 of the 3 atelin primate genera: spider monkeys (Ateles) and muriquis (Brachyteles). For the third atelin genus, Lagothrix, patterns of intragroup social behavior have been less well-documented. We studied the social and reproductive behavior of lowland woolly monkeys (Lagothrix lagotricha poeppigii) in Ecuador during a one-year observational study and subsequently used molecular techniques to investigate population genetic structure and dispersal patterns for this taxon. Among adult male woolly monkeys, both affiliative and agonistic interactions were rare, and males were seldom in close proximity to one another. Relationships among male woolly monkeys are best characterized as tolerant, especially in the context of mating wherein direct competition among males was minimal despite the fact that females mated with multiple males. Relationships among females were likewise generally tolerant but nonaffiliative, though females often directed harassment towards copulating pairs. Affiliative interactions that did occur among woolly monkeys tended to be directed either between the sexes-primarily from female to male-or from younger towards older males, and the proximity partners of females tended to be members of the opposite sex. These results suggest that bonds between the sexes may be more important than same-sex social relationships and that direct female-female competition is an important feature of woolly monkey reproductive biology. Our genetic results indicate that, as in other atelins, dispersal by females is common, but some male dispersal likely occurs as well. In some but not all groups we studied, nonjuvenile males within social groups were more closely related to one another on average than females were, which is consistent with greater male than female philopatry. However, differences in these patterns among our study groups may reflect local variation in dispersal behavior. C1 NYU, Dept Anthropol, New York, NY 10003 USA. NYU, Ctr Study Human Origins, New York, NY 10003 USA. NYCEP, New York, NY USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Genet Program, Washington, DC 20560 USA. RP Di Fiore, A (reprint author), NYU, Dept Anthropol, Rufus Smith Hall,Room 802-803,25 Waverly Pl, New York, NY 10003 USA. EM anthony.difiore@nyu.edu NR 78 TC 42 Z9 44 U1 1 U2 52 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0164-0291 J9 INT J PRIMATOL JI Int. J. Primatol. PD OCT PY 2005 VL 26 IS 5 BP 1137 EP 1173 DI 10.1007/s10764-005-6462-4 PG 37 WC Zoology SC Zoology GA 973BK UT WOS:000232497700009 ER PT J AU Smith, SA Bermingham, E AF Smith, SA Bermingham, E TI The biogeography of lower Mesoamerican freshwater fishes SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE beta diversity; biogeography; community assembly; dispersal; freshwater fish; Mesoamerica; regional processes; species richness ID REGIONAL PROCESSES; CENTRAL-AMERICA; SPECIES-DIVERSITY; GLOBAL PATTERNS; WESTERN PANAMA; UNITED-STATES; HISTORY; BIODIVERSITY; ASSEMBLAGES; EVOLUTION AB Aim This paper examines the importance of regional processes in determining the patterns of distribution and diversity of lower Mesoamerican freshwater fishes. Location We focused our analyses on the lower Mesoamerican region, which we define to include all the rivers of Panama and Costa Rica. The geographic boundaries are the Colombian Choco to the south and Lake Nicaragua to the north. Methods We described the biogeographical provinces of lower Mesoamerica (LMA) using presence/absence data of primary and secondary LMA freshwater fishes. We conducted subsequent analyses at the spatial resolution of the biogeographical provinces and described patterns of community composition, species richness, endemism, range size, and the permeability of dispersal barriers between biogeographical provinces. Results This study represents the first attempt since that of W. A. Bussing in 1976 to investigate the biogeographical regions of Mesoamerica, and our analyses demonstrate increased regional complexity in biodiversity patterns relative to previous studies. Changes in community composition across LMA clearly highlight the importance of both extrinsic geological processes and intrinsic biological differences among freshwater fish species in shaping the dispersal and diversification histories of the LMA freshwater fish fauna. The influence of biology and geology is also exemplified by patterns of endemism and turnover between biogeographical provinces, which suggests that the relative importance of regional speciation and dispersal varies spatially across the LMA landscape. Finally, it would seem to follow that secondary freshwater fishes will have larger range sizes than primary fishes as a result of the increased salinity tolerance posited for the former group, and thus the increased probability of dispersal along coastlines. We did not, however, find a significant difference between the average range size of primary and secondary freshwater fishes, indicating that the putative differences in physiological tolerance to seawater between the two groups are not reflected in their distribution patterns at the scale of LMA. The geometric distribution of range size of LMA freshwater fishes suggests that dispersal of both primary and secondary freshwater fishes along coastlines must be infrequent. Main conclusion The observation that regional processes exerted a strong influence on the assembly and maintenance of LMA freshwater fish communities has important consequences for both theory and conservation. We suggest that large-scale biogeographical analyses are required to illuminate the backdrop upon which local interactions play themselves out, supporting a top-down approach to the study of biological diversity. Our results also identify areas of high conservation priority, providing a baseline for informing conservation strategies for freshwater fishes in LMA. We conclude by calling for conservation planning and action that acknowledges the importance that regional processes play in determining patterns of organismal diversity, and that incorporates these processes in strategies to conserve remnant biological diversity. C1 McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Smithsonian Trop Res Inst, Panama City, Panama. RP Smith, SA (reprint author), McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM ssmith3@po-box.mcgill.ca NR 64 TC 59 Z9 60 U1 1 U2 25 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD OCT PY 2005 VL 32 IS 10 BP 1835 EP 1854 DI 10.1111/j.1365-2699.2005.01317.x PG 20 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 964TR UT WOS:000231904100013 ER PT J AU Hall, MC Stiling, P Hungate, BA Drake, BG Hunter, MD AF Hall, MC Stiling, P Hungate, BA Drake, BG Hunter, MD TI Effects of elevated CO2 and herbivore damage on litter quality in a scrub oak ecosystem SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE elevated CO2; herbivory; litter quality; Quercus myrtifolia; Quercus chapmanii; Quercus geminata; Kennedy Space Center ID LEAF-LITTER; ATMOSPHERIC CO2; DECOMPOSITION; PLANT; DYNAMICS; NITROGEN; FOREST; DEFOLIATION; ABSCISSION; DEPOSITION AB Atmospheric CO2 concentrations have increased dramatically over the last century and continuing increases are expected to have significant, though currently unpredictable, effects on ecosystems. One important process that may be affected by elevated CO2 is leaf litter decomposition. We investigated the interactions among atmospheric CO2, herbivory, and litter quality within a scrub oak community at the Kennedy Space Center, Florida. Leaf litter chemistry in 16 plots of open-top chambers was followed for 3 years; eight were exposed to ambient levels of CO2, and eight were exposed to elevated levels of CO2 (ambient + 350 ppmV). We focused on three dominant oak species, Quercus geminata, Quercus myrtifolia, and Quercus chapmanii. Condensed tannin concentrations in oak leaf litter were higher under elevated CO2. Litter chemistry differed among all plant species except for condensed tannins. Phenolic concentrations were lower, whereas lignin concentrations and lignin/nitrogen ratios were higher in herbivore-damaged litter independent of CO2 concentration. However, changes in litter chemistry from year to year were far larger than effects of CO2 or insect damage, suggesting that these may have only minor effects on litter decomposition. C1 Univ Georgia, Inst Ecol, Athens, GA 30602 USA. Univ S Florida, Dept Biol, Tampa, FL 33620 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. RP Hall, MC (reprint author), Univ Georgia, Inst Ecol, Athens, GA 30602 USA. EM mchall@uga.edu RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 41 TC 14 Z9 16 U1 0 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD OCT PY 2005 VL 31 IS 10 BP 2343 EP 2356 DI 10.1007/s10886-005-7105-0 PG 14 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 969XK UT WOS:000232269000007 PM 16195847 ER PT J AU Svenning, JC Wright, SJ AF Svenning, JC Wright, SJ TI Seed limitation in a Panamanian forest SO JOURNAL OF ECOLOGY LA English DT Article DE community ecology; dispersal assembly; Panama; seed addition experiment; seed limitation; seed size; seedling ecology; seedling recruitment; tropical ecology; tropical forest ID RECRUITMENT LIMITATION; NEOTROPICAL FOREST; COMMUNITY STRUCTURE; TROPICAL FORESTS; TREE DIVERSITY; DISPERSAL; PATTERNS; GAP; CONSEQUENCES; GRASSLAND AB 1 The role of seed limitation in tropical forests remains uncertain owing to the scarcity of experimental evidence. We performed seed addition experiments to assess seed limitation for 32 shade-tolerant tropical forest species and monitored the natural seed rain of 25 of these species for 17 years. 2 One, two or five seeds were sown into 0.0079-m(2) plots for large- (n = 5 species), medium- (n = 5) and small-seeded species (n = 22), respectively. The experiment was replicated at 69 sites, placed in groups of three at 23 locations. Seedling establishment was evaluated after 1 and 2 years in paired seed addition and control plots. Natural seedling emergence and understorey plant density were also measured. 3 Median natural seed rain was 0.31 seeds m(-2) year(-1) per focal species. 4 Seed addition enhanced seedling establishment in 31 and 26 of the 32 species after 1 and 2 years, respectively. Mean number of focal species' seedlings after 2 years was 0.002 seedlings in control plots and 0.12, 0.37 and 0.60 seedlings in seed addition plots for large-, medium- and small-seeded species, respectively. 5 A 25 seeds added treatment increased seedling establishment by >= 2.0-fold over the five seeds added treatment after 2 years. 6 Community-wide recruitment and understorey plant density were strongly seed-limited. The natural density of understorey plants averaged 12 plants m(-2) and was significantly less than for seedlings of the single focal species in plots with >= 2 seeds added 2 years earlier. 7 The number of established seedlings per seed added was independent of seed size. 8 Treatment (adding zero or five seeds), species identity and location all affected seedling establishment for the 11 small-seeded species represented at all sites, with treatment and its interactions accounting for 86% of the explained variation. 9 Our results suggest that seed limitation plays a dominant role in seedling recruitment and understorey plant community assembly in tropical forests. Although strong seed limitation may set the stage for species-neutral community assembly, the species differences in seedling establishment rate and its spatial variation demonstrate an important role for species-specific processes. C1 Aarhus Univ, Dept Biol Sci, DK-8000 Aarhus C, Denmark. Smithsonian Trop Res Inst, Balboa, Panama. RP Svenning, JC (reprint author), Aarhus Univ, Dept Biol Sci, Build 540, DK-8000 Aarhus C, Denmark. EM svenning@biology.au.dk RI Svenning, Jens-Christian/C-8977-2012; Wright, Stuart/M-3311-2013 OI Svenning, Jens-Christian/0000-0002-3415-0862; Wright, Stuart/0000-0003-4260-5676 NR 51 TC 48 Z9 56 U1 2 U2 26 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD OCT PY 2005 VL 93 IS 5 BP 853 EP 862 DI 10.1111/j.1365-2745.2005.01016.x PG 10 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 962MN UT WOS:000231737000001 ER PT J AU Huber, BT Quillevere, F AF Huber, BT Quillevere, F TI Revised Paleogene planktonic foraminiferal biozonation for the Austral Realm SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID MIDDLE EOCENE; STABLE-ISOTOPE; INDIAN-OCEAN; MAUD RISE; PALEOCENE; MAGNETOBIOCHRONOLOGY; BIOSTRATIGRAPHY; STRATIGRAPHY; ANTARCTICA; OLIGOCENE AB A major revision to the Antarctic Paleogene planktonic foraminifer biozonation is presented using the latest species concepts and biostratigraphic studies of Ocean Drilling Program (ODP) sites located between 52 degrees S and 65 degrees S paleolatitude in the southern South Atlantic and southern Indian Oceans. Shorthand prefixes for the Antarctic Paleogene zones are designated as "AP" zones for the "Antarctic Paleocene", "AE" zones for the "Antarctic Eocene", and "AO" zones for the "Antarctic Oligocene". New numerical ages for Paleogene planktonic foraminiferal and calcareous nannofossil first- and last-occurrence events are estimated using new age-depth curves constructed for ODP Sites 738 and 744 in the southern Indian Ocean. The order and timing of these events are compared with bio-, magneto- and chemostratigraphic datums that have been recently published, reinterpreted, or observed in the present study. The revised zonal framework and age models will improve correlation of Paleogene planktonic foraminifer pelagic and hemipelagic carbonate sequences within and outside the Austral Realm. C1 Smithsonian Museum Nat Hist, Washington, DC 20013 USA. Univ Lyon 1, CNRS, UMR 5125, Lab Paleoenvironm & PaleobioSphere, F-69622 Villeurbanne, France. RP Huber, BT (reprint author), Smithsonian Museum Nat Hist, Washington, DC 20013 USA. EM huberb@si.edu; frederic.quillevere@univ-lyon1.fr RI Quillevere, Frederic/C-8317-2012 NR 56 TC 17 Z9 21 U1 0 U2 0 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2005 VL 35 IS 4 BP 299 EP 314 DI 10.2113/35.4.299 PG 16 WC Paleontology SC Paleontology GA 991RW UT WOS:000233832400002 ER PT J AU Alemseged, Z Wynn, JG Kimbel, WH Reed, D Geraads, D Bobe, R AF Alemseged, Z Wynn, JG Kimbel, WH Reed, D Geraads, D Bobe, R TI A new hominin from the Basal Member of the Hadar Formation, Dikika, Ethiopia, and its geological context SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE pliocene; hominin evolution; Australopithecus afarensis; hadar formation; Dikika; Ethiopia ID SIDI HAKOMA TUFF; TULU BOR TUFF; AUSTRALOPITHECUS-AFARENSIS; ALLIA BAY; AGE; PLIOPLEISTOCENE; DISCOVERIES; MORPHOLOGY; ANAMENSIS; EVOLUTION AB In this paper we report for the first time hominin remains from the Basal Member of the Hadar Formation at Dikika, in the Awash Valley of Ethiopia, dating to greater than 3.4 Ma. The new fossil, DIK-2-1, is a fragment of a left mandible and associated dentition. The mandible is attributed to Australopithecus afarensis. However, the new fossil exhibits some metric and morphological features that have not previously been seen in the A. afarensis hypodigm, increasing the already impressive degree of variation in the mandibular sample of the species. (c) 2005 Elsevier Ltd. All rights reserved. C1 Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. Univ St Andrews, Dept Geog & Geosci, St Andrews KY16 9AL, Fife, Scotland. Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. Arizona State Univ, Dept Anthropol, Tempe, AZ 85287 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20560 USA. CNRS, UPR 2147, F-75014 Paris, France. SUNY Buffalo, Dept Anthropol, Buffalo, NY 14261 USA. RP Alemseged, Z (reprint author), Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, Deutsch Pl 6, D-04103 Leipzig, Germany. EM zeray@eva.mpg.de; jonathan.wynn@st-andrews.ac.uk; wkimbel.iho@asu.edu; denne@umich.edu; dgeraads@ivry.cnrs.fr; renebobe@buffalo.edu RI Wynn, Jonathan/C-1646-2010; OI Bobe, Rene/0000-0001-9059-2203; GERAADS, Denis/0000-0003-2475-8011 NR 33 TC 35 Z9 35 U1 0 U2 8 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 OCT PY 2005 VL 49 IS 4 BP 499 EP 514 DI 10.1016/j.jhevol.2005.06.001 PG 16 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 973FV UT WOS:000232509200006 PM 16026815 ER PT J AU Lambert, TD Malcolm, JR Zimmerman, BL AF Lambert, TD Malcolm, JR Zimmerman, BL TI Variation in small mammal species richness by trap height and trap type in southeastern Amazonia SO JOURNAL OF MAMMALOGY LA English DT Article DE Amazonia; biodiversity; canopy trapping; marsupials; rodents; small mammals; Xingu Basin ID RATS PROECHIMYS-SEMISPINOSUS; ATLANTIC FOREST; SPINY RATS; VERTICAL STRATIFICATION; EUCALYPT FORESTS; EASTERN AMAZONIA; CENTRAL PANAMA; BRAZIL; ARBOREAL; DIVERSITY AB Despite its biological richness, the rodent and marsupial fauna of many parts of the Amazon Basin remains poorly known and the efficacy of different methods in assessing its diversity are poorly understood. We present results of small mammal trapping at a previously unsurveyed site in the Xingu Basin of the southeastern Amazon, Par, Brazil; provide details on a new method For arboreal trapping; and compare species richness among traps at different heights and between different trap types. Mammals were livetrapped at 3 trap heights: ground, understory (1-3 in above ground), and canopy (mean height = 11.5 in +/- 3.2 SD, range = 4.8-16.8 in, n = 76 trap stations). We recorded 1,769 captures of 1,178 individuals of 8 marsupial and 17 rodent species in 38,090 trap-nights (or 19,320 station-nights, where a station-night consisted of I Sherman and I Tomahawk live trap at l height for I night). Overall trap Success was 6.1 individuals per 100 station-nights; success by trap position was 9.0% for ground (7,850 station-nights), 4.7% for understory (7,850 station-nights), and 2.9% for canopy (3,490 station-nights). Success by trap type was 4.7% for Shermans and 5.9% for Tomahawks, with Tomahawk traps showing a more rapid accumulation of species. Rarefied species accumulation curves showed little improvement with the inclusion of canopy trapping, which we attribute to high variability in the development of vertical structure at the site. We suggest that in areas with low and often-broken canopies, only ground and understory traps need be employed for long-term studies;, however, some form of canopy trapping should be used during initial Surveys so that the utility of arboreal trapping can be evaluated. C1 Conservat Int, Brazil Program, Kayapo Project, Washington, DC 20036 USA. Univ Toronto, Fac Forestry, Ctr Earth Sci, Toronto, ON M5S 3B3, Canada. Smithsonian Trop Res Inst, BCI Unit 0948, APO, AA 34002 USA. RP Lambert, TD (reprint author), Smithsonian Trop Res Inst, BCI Unit 0948, APO, AA 34002 USA. EM thomas.lambert@u-toronto.ca NR 47 TC 30 Z9 35 U1 3 U2 15 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD OCT PY 2005 VL 86 IS 5 BP 982 EP 990 DI 10.1644/1545-1542(2005)86[982:VISMSR]2.0.CO;2 PG 9 WC Zoology SC Zoology GA 978LS UT WOS:000232875400017 ER PT J AU Britz, R Johnson, GD AF Britz, R Johnson, GD TI Leis' conundrum: Homology of the clavus of the ocean sunfishes. 1. Ontogeny of the median fins and axial skeleton of Monotrete leiurus (Teleostei, Tetraodontiformes, Tetraodontidae) SO JOURNAL OF MORPHOLOGY LA English DT Article DE vertebral column; median fins; pterygiophores; ontogeny; homology; Tetraodontidae ID RED-SEA BREAM; OSTEOLOGICAL DEVELOPMENT; VERTEBRAL COLUMN; CAUDAL SKELETON; ACTINOPTERYGIAN FISHES; PAGRUS-MAJOR; SUPPORTS; LARVAE; REEVALUATION; COMPLEX AB We describe the ontogeny of the axial skeleton and median fins of the Southeast Asian freshwater puffer Monotrete leiurus, based on a reared developmental series. Most elements of the axial skeleton in M. leiurus arise in membrane bone. Only the base of the anterior three neural arches, the base of the hemal arches of the third preural centrum, the neural and hemal arches and spines of the second preural centrum, the parhypural, the two hypural plates, and the single epural are preformed in cartilage. In contrast to most teleosts, the proximal-middle radials of the dorsal and anal fins are upright and symmetrical and their distal tips coalesce during development to form a deep band of cartilage, from which the spherical distal radials are spatially separated. C1 Nat Hist Museum, Dept Zool, London SW7 5BD, England. Smithsonian Inst, Natl Museum Amer Hist, Div Fishes, Washington, DC 20560 USA. RP Britz, R (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. EM R.Britz@nhm.ac.uk NR 55 TC 16 Z9 16 U1 4 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD OCT PY 2005 VL 266 IS 1 BP 1 EP 10 DI 10.1002/jmor.10243 PG 10 WC Anatomy & Morphology SC Anatomy & Morphology GA 969RV UT WOS:000232253300001 PM 15549688 ER PT J AU Johnson, GD Britz, R AF Johnson, GD Britz, R TI Leis' conundrum: Homology of the clavus of the ocean sunfishes. 2. Ontogeny of the median fins and axial skeleton of Ranzania laevis (Teleostei, Tetraodontiformes, Molidae) SO JOURNAL OF MORPHOLOGY LA English DT Article DE axial skeleton; median fins; pterygiophores; clavus; ontogeny; homology; Molidae ID FISHES AB One of the most conspicuous characters of the ocean sunfishes, family Molidae, is the punctuation of the body by a deep, abbreviated, caudal fin-like structure extending vertically between the posterior ends of the dorsal and anal fins, termed the clavus by Fraser Brunner. Homology of the clavus has been a matter of debate since the first studies on molid anatomy in the early 1800s. Two hypotheses have been proposed: 1) It is a highly modified caudal fin; 2) It is formed by highly modified elements of the dorsal and anal fins. To resolve this homology issue, we studied the ontogeny of the molid vertebral column and median fins and compared it to that of a less morphologically derived gymnodont (see Part I of this study), a member of the family Tetraodontidae. We show that in molids the chorda never flexes during development, that the claval rays form from the posterior ends of the dorsal and anal fins toward the middle, thus closing the gap inward, and that elements of the molid clavus have an identical development and composition as the proximal-middle and distal radials of the regular dorsal and anal fins. We thus conclude that the molid clavus is unequivocally formed by modified elements of the dorsal and anal fin and that the caudal fin is lost in molids. C1 Nat Hist Museum, Dept Zool, London SW7 5BD, England. Smithsonian Inst, Natl Museum Amer Hist, Div Fishes, Washington, DC 20560 USA. RP Britz, R (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. EM R.Britz@nhm.ac.uk NR 35 TC 24 Z9 25 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD OCT PY 2005 VL 266 IS 1 BP 11 EP 21 DI 10.1002/jmor.10242 PG 11 WC Anatomy & Morphology SC Anatomy & Morphology GA 969RV UT WOS:000232253300002 PM 15549687 ER PT J AU Woodman, N Morgan, JJP AF Woodman, N Morgan, JJP TI Skeletal morphology of the forefoot in shrews (Mammalia : Soricidae) of the genus Cryptotis, as revealed by digital x-rays SO JOURNAL OF MORPHOLOGY LA English DT Article DE carpals; digits; Insectivora; manus; skeleton; Soricinae; Soricomorpha ID SMALL-EARED SHREW; EVOLUTION; SORICOMORPHA; PATTERNS AB Variation in the forefoot skeleton of small-eared shrews (family Soricidae, genus Cryptotis) has been previously documented, but the paucity of available skeletons for most taxa makes assessment of the degrees of intraspecific and interspecific variation difficult. We used a digital X-ray system to extract images of the forefoot skeleton from 101 dried skins of eight taxa (seven species, including two subspecies of one species) of these shrews. Lengths and widths of each of the four bones of digit III were measured directly from the digital images, and we used these data to quantify variation within and among taxa. Analysis of the images and measurements showed that interspecific variation exceeds intraspecific variation. In fact, most taxa could be distinguished in multivariate and some bivariate plots. Our quantitative data helped us define a number of specific forefoot characters that we subsequently used to hypothesize evolutionary relationships among the taxa using the exhaustive search option in PAUP, a computer program for phylogenetic analysis. The resulting trees generally concur with previously published evolutionary hypotheses for small-eared shrews. Cryptotis meridensis, a taxon not previously examined in recent phylogenies, is rooted at the base of the branch leading to the C. mexicana group of species. The position of this species suggests that the mostly South American C. thomasi group shares an early ancestor with the C. mexicana group. C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. Ft Valley State Univ, Ft Valley, GA 31030 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, MRC 111,POB 37012, Washington, DC 20013 USA. EM woodmanN@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 34 TC 16 Z9 18 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD OCT PY 2005 VL 266 IS 1 BP 60 EP 73 DI 10.1002/jmor.10367 PG 14 WC Anatomy & Morphology SC Anatomy & Morphology GA 969RV UT WOS:000232253300005 PM 16121402 ER PT J AU Britz, R Johnson, GD AF Britz, R Johnson, GD TI Occipito-vertebral fusion in ocean sunfishes (Teleostei : Tetraodontiformes : Molidae) and its phylogenetic implications SO JOURNAL OF MORPHOLOGY LA English DT Article DE basioccipital; first vertebra; phylogeny; ontogeny; homology; Molidae; Ostraciidae ID FISHES AB We describe the ontogeny of the occipital skull and anterior vertebrae of the molids Ranzania laevis and Masturus lanceolatus and compare it with that of the ostraciid Lactophrys sp. The first vertebra fuses to the basioccipital in early ontogeny in the two molids and previous authors thus confused that vertebra with the back of the basioccipital, so that all previous counts of their vertebral numbers are incorrect by one vertebra. As evidenced by Lactophrys sp., ostraciids are the only other tetraodontiforms with similar occipito-vertebral fusion. In contrast to the molids, additional anterior vertebrae fuse with this complex in ostraciids. We conclude that the shared occipitovertebral fusion in molids and ostraciids and its otherwise extremely rare occurrence among teleosts provide support for a sister-group relationship of the two families. C1 Nat Hist Museum, Dept Zool, London SW7 5BD, England. Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. RP Britz, R (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. EM r.britz@nhm.ac.uk NR 23 TC 18 Z9 19 U1 1 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD OCT PY 2005 VL 266 IS 1 BP 74 EP 79 DI 10.1002/jmor.10366 PG 6 WC Anatomy & Morphology SC Anatomy & Morphology GA 969RV UT WOS:000232253300006 PM 16124009 ER PT J AU Ospina, CA Rodriguez, AD Sanchez, JA Ortega-Barria, E Capson, TL Mayer, AMS AF Ospina, CA Rodriguez, AD Sanchez, JA Ortega-Barria, E Capson, TL Mayer, AMS TI Caucanolides A-F, unusual antiplasmodial constituents from a Colombian collection of the gorgonian coral Pseudopterogorgia bipinnata SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID CHRONIC HEPATITIS-B; NATURAL-PRODUCTS; DITERPENES; CHEMISTRY; LACTONES; CEMBRANE; ALPHA AB Six new diterpenoids, caucanolides A-F (1-6), have been isolated from extracts of the gorgonian octocoral Pseudopterogorgia bipinnata collected near the Colombian Southwestern Caribbean Sea. The structures of 1-6 were elucidated by comprehensive analysis of spectroscopic data. The caucanolides showed in vitro antiplasmodial activity against the malaria parasite, Plasmodium. falciparum. In addition to possessing structures based on novel carbon skeletons, one of these metabolites, caucanolide B (2), constitutes the only example from nature of a secondary metabolite possessing the N-1,N-1-dimethyl-N-2-acylformamidine functionality. C1 Univ Puerto Rico, Dept Chem, UPR Stn, Rio Piedras, PR 00931 USA. Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia. Ctr Estudios Biomed, Inst Invest Cient Avanzadas, Panama City, Panama. Ctr Estudios Biomed, Serv Alta Tecnol, Panama City, Panama. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Midwestern Univ, Chicago Coll Osteopath Med, Dept Pharmacol, Downers Grove, IL 60515 USA. RP Rodriguez, AD (reprint author), Univ Puerto Rico, Dept Chem, UPR Stn, POB 23346, Rio Piedras, PR 00931 USA. EM arodrig@cnnet.upr.edu RI Johnson, Selena/K-3541-2013; OI Mayer, Alejandro /0000-0002-8358-4528 FU NIEHS NIH HHS [1 R15 ES12654-01]; NIGMS NIH HHS [S06GM08102]; NINDS NIH HHS [NS39408M] NR 35 TC 17 Z9 18 U1 2 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 OCT PY 2005 VL 68 IS 10 BP 1519 EP 1526 DI 10.1021/np0502239z PG 8 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 983DR UT WOS:000233211800013 PM 16252918 ER PT J AU Brown, M Lappin, MR Brown, JL Munkhtsog, B Swanson, WF AF Brown, M Lappin, MR Brown, JL Munkhtsog, B Swanson, WF TI Exploring the ecologic basis for extreme susceptibility of Pallas' cats (Otocolobus manul) to fatal toxoplasmosis SO JOURNAL OF WILDLIFE DISEASES LA English DT Article DE blood chemistry; captive; free-ranging; hematology; Mongolia; Pallas' cats; serology; Toxoplasma gondii ID FELINE IMMUNODEFICIENCY VIRUS; ADRENOCORTICAL FUNCTION; GONDII INFECTION; SEROPREVALENCE; ANTIBODIES; SEASONALITY; METABOLISM; MAMMALS AB Recent efforts by North American zoos to establish a genetically viable captive population of Pallas' cats (Otocolobus manul) have been compromised by high newborn mortality (similar to 60%), primarily because of toxoplasmosis. The basis for this extreme susceptibility to toxoplasmosis is unknown. In the present study, the general health status of wild Pallas' cats in Mongolia was evaluated, including assessment of basal hematologic parameters and fecal corticoid metabolite concentrations. The prevalence of exposure to Toxoplasma gondii in Mongolian Pallas' cats, local domestic cats, and prey species also was determined based on serology and/or polymerase chain reaction analysis. Biologic samples (blood, feces, and/or brain tissue) were obtained from 15 wild Pallas' cats, 15 domestic cats, and 45 prey animals (rodents and pikas) captured in Mongolia during the summers of 2000 and 2001. Comparative data were obtained from nine captive Pallas' cats maintained in North American zoos. Based on physical examinations, complete blood counts, and blood chemistry analyses, only minor differences were, observed in the general health status of wild and captive Pallas', cats. decal cortisol metabolite concentrations did not differ (P > 0.05) between populations, indicating that Pallas' cats in captivity and in the wild have similar basal adrenocortical activtity. A pronounced difference (P < 0.01) in seroprevalence to T gondii was observed between populations. Whereas all captive Pallas' cats exhibited elevated immuneglobulin titers (IgG > 2,048) to T gondii, only two of 15 (13%) wild Pallas' cats were seropositive, with both cats having lower IgG titers (< 1,024). Furthermore, no evidence of exposure to this parasite was found in any of the Mongolian domestic cats or prey species. These findings suggest that wild Pallas' cats have minimal opportunity for exposure to T. gondii in their natural habitat and, typically, do not become infected with this parasite until being brought into captivity. Accordingly, maintenance of a viable captive population may require implementing effective strategies to prevent exposure of immunologically naive Pallas' cats to T. gondii and to reduce parasite transmission between seropositive females and their highly susceptible offspring. C1 Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, Cincinnati, OH 45220 USA. Colorado State Univ, Coll Vet Med & Biomed Sci, Ft Collins, CO 80523 USA. Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Mongolian Acad Sci, Ulaanbaatar, Mongol Peo Rep. Michigan State Univ, Dept Fisheries & Wildlife, E Lansing, MI 48824 USA. RP Brown, M (reprint author), Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, Cincinnati, OH 45220 USA. EM brownmer@ncifcrf.gov NR 37 TC 13 Z9 14 U1 0 U2 17 PU WILDLIFE DISEASE ASSN, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD OCT PY 2005 VL 41 IS 4 BP 691 EP 700 PG 10 WC Veterinary Sciences SC Veterinary Sciences GA 013AB UT WOS:000235380900003 PM 16456157 ER PT J AU Vessot, RFC AF Vessot, RFC TI The atomic hydrogen maser oscillator (vol 42, pg S80, 2005) SO METROLOGIA LA English DT Correction AB This paper outlines the evolution of the hydrogen maser oscillator and describes the basic operational requirements and the present technology. Design features of a high stability maser oscillator for use in space, maser operation at 0.5 K and the present uses of H-masers are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vessot, RFC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 5 Z9 5 U1 0 U2 0 PU BUREAU INT POIDS MESURES PI SEVRES CEDEX PA B1 PM PAVILLION DE BRETUEIL, F-92312 SEVRES CEDEX, FRANCE SN 0026-1394 J9 METROLOGIA JI Metrologia PD OCT PY 2005 VL 42 IS 5 BP 468 EP 470 DI 10.1088/0026-1394/42/5/C01 PG 3 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 986MO UT WOS:000233453900022 ER PT J AU Weigt, LA Crawford, AJ Rand, AS Ryan, MJ AF Weigt, LA Crawford, AJ Rand, AS Ryan, MJ TI Biogeography of the tungara frog, Physalaemus pustulosus: a molecular perspective SO MOLECULAR ECOLOGY LA English DT Article DE allozymes; biogeography; intergradation; mtDNA ID CENTRAL AMERICAN HERPETOFAUNA; FRESH-WATER FISHES; EVOLUTIONARY TREES; MITOCHONDRIAL-DNA; PHYLOGENETIC INFERENCE; LEPTODACTYLID FROGS; ANDEAN TECTONICS; DIVERGENCE TIME; METABOLIC-RATE; SOUTH-AMERICA AB Physalaemus pustulosus, a small leptodactylid frog with South American affinities, ranges across northern South America through Middle America to southern Mexico. To investigate its geographic variation and evolutionary origins, we analysed the presumptive gene products of 14 allozyme loci and sequenced a portion of the mitochondrial COI gene from individuals sampled throughout the distribution. Generally, allozyme dissimilarities and sequence divergences are correlated with each other and with geographic proximity. The greatest discontinuity in genetic variation was found between populations in Middle America vs. South America + Panama. Based on two Bayesian MCMC (Markov chain Monte Carlo) divergence time estimates involving two independent temporal constraints, the timing of the separation of northern and southern tungara frog lineages is significantly older than the time since completion of the current Panama land bridge. P. pustulosus first invaded Middle America from South America about 6-10 million years ago giving rise to the northern lineage. The southern lineage then invaded Panama independently after land bridge completion. Despite millions of years of independent evolution, the multilocus allozyme data revealed that western Panama populations represent a contact zone containing individuals with alleles from both groups present. C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20250 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. RP Weigt, LA (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20250 USA. EM weigtl@si.edu OI Crawford, Andrew J./0000-0003-3153-6898 NR 89 TC 52 Z9 52 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD OCT PY 2005 VL 14 IS 12 BP 3857 EP 3876 DI 10.1111/j.1365-294X.2005.02707.x PG 19 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 968ED UT WOS:000232143800017 PM 16202101 ER PT J AU Churazov, E Sazonov, S Sunyaev, R Forman, W Jones, C Bohringer, H AF Churazov, E. Sazonov, S. Sunyaev, R. Forman, W. Jones, C. Boehringer, H. TI Supermassive black holes in elliptical galaxies: switching from very bright to very dim SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: jets; galaxies: nuclei ID X-RAY BINARIES; COOLING FLOWS; INTRACLUSTER MEDIUM; CHANDRA OBSERVATION; RADIO LOBES; HYDRA-A; QUASARS; FEEDBACK; CLUSTER; ACCRETION AB Relativistic outflows (mainly observed in the radio) are a characteristic feature of both Galactic stellar-mass black holes and supermassive black holes (SMBHs). Simultaneous radio and X-ray observations of Galactic sources have shown that the outflow is strong at low accretion rates, but it weakens dramatically or disappears completely at high accretion rates, manifesting structural changes in the accretion flow. It is reasonable to assume that SMBHs follow the same trend. For low-luminosity SMBHs in nearby elliptical galaxies and clusters, recent observations strongly suggest that the outflows play the central role in keeping the gas hot (mechanical feedback). If the outflow is quenched in SMBHs at high accretion rates similarly to the behaviour of Galactic sources, then the straightforward consequence is a relatively weak feedback of rapidly accreting SMBHs. We argue that elliptical galaxies and their central engines should then evolve through two stages. Early on, the central SMBH rapidly grows by accreting cooling gas at a near Eddington rate with high radiative efficiency but with weak feedback on the infalling gas. This stage terminates when the black hole has grown to a sufficiently large mass that its feedback (radiative and/or mechanical), despite the low gas heating efficiency, is able to suppress gas cooling. After that the system switches to a stable state corresponding to passively evolving ellipticals, when the accretion rate and radiative efficiency are very low, but the gas heating efficiency is high and energy input from the relativistic outflow keeps the gas hot. C1 [Churazov, E.; Sazonov, S.; Sunyaev, R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.; Sazonov, S.; Sunyaev, R.] Space Res Inst IKI, Moscow 117810, Russia. [Forman, W.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boehringer, H.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Churazov, E (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM churazov@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 FU Smithsonian Institute; Chandra X-ray Center FX We are grateful to the referee for important comments. WF and CJ acknowledge support from the Smithsonian Institute and the Chandra X-ray Center. NR 41 TC 116 Z9 117 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 OCT PY 2005 VL 363 IS 1 BP L91 EP L95 DI 10.1111/j.1745-3933.2005.00093.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V16ZA UT WOS:000207906300019 ER PT J AU Diego, JM Sandvik, HB Protopapas, P Tegmark, M Benitez, N Broadhurst, T AF Diego, JM Sandvik, HB Protopapas, P Tegmark, M Benitez, N Broadhurst, T TI Non-parametric mass reconstruction of A1689 from strong lensing data with the Strong Lensing Analysis Package SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : clusters : general ID X-RAY; DARK-MATTER; ABELL 1689; CLUSTERS; GALAXIES; PROFILE; WEAK; MAGNIFICATION; DISCREPANCY; INVERSION AB We present the mass distribution in the central area of the cluster A1689 by fitting over 100 multiply lensed images with the non-parametric Strong Lensing Analysis Package. The surface mass distribution is obtained in a robust way, finding a total mass of 0.25 x 10(15) h(-1) M circle dot within a 70-arcsec circle radius from the central peak. Our reconstructed density profile fits well a Navarro-Frenk-White (NFW) profile with small perturbations due to substructure, and is compatible with the more model-dependent analysis of Broadhurst et al. based on the same data. Our estimated mass does not rely on any prior information about the distribution of dark matter in the cluster. The peak of the mass distribution falls very close to the central dominant (cD) galaxy and there is substructure near the centre suggesting that the cluster is not fully relaxed. We also examine the effect on the recovered mass when we include the uncertainties in the redshift of the sources and in the original shape of the sources. Using simulations designed to mimic the data, we identify some biases in our reconstructed mass distribution. We find that the recovered mass is biased toward lower masses beyond 1 arcmin (150 kpc) from the cD galaxy and that in the very centre we may be affected by degeneracy problems. On the other hand, we confirm that the reconstructed mass between 25 and 70 arcsec is a robust, unbiased estimate of the true mass distribution and is compatible with an NFW profile. C1 MIT, Ctr Space Res, Cambridge, MA 02138 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Max Planck Inst Astrophys, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. CSIC, Inst Astrofis Andalucia, Granada, Spain. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RP Diego, JM (reprint author), MIT, Ctr Space Res, Cambridge, MA 02138 USA. EM jdiego@space.mit.edu OI Benitez, Narciso/0000-0002-0403-7455 NR 35 TC 47 Z9 47 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 OCT 1 PY 2005 VL 362 IS 4 BP 1247 EP 1258 DI 10.1111/j.1365-2966.2005.09372.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 964TP UT WOS:000231903800013 ER PT J AU Van Bael, SA Brawn, JD AF Van Bael, SA Brawn, JD TI The direct and indirect effects of insectivory by birds in two contrasting Neotropical forests (vol 143, pg 106, 2005) SO OECOLOGIA LA English DT Correction DE arthropods; canopy; herbivory; multitrophic interactions; predation ID FOOD-WEB COMPLEXITY; TROPHIC CASCADES; POPULATION CONTROL; PRIMARY PRODUCTIVITY; HERBIVOROUS INSECTS; COMMUNITY STRUCTURE; RELATIVE ROLES; LEAF DAMAGE; BOTTOM-UP; WHITE OAK AB A goal among community ecologists is to predict when and where trophic cascades occur. For example, several studies have shown that forest birds can limit arthropod abundances on trees, but indirect effects of bird predation (i.e. decreased arthropod damage to trees) are not always observed and their context is not well understood. Because productivity is one factor that is expected to influence trophic cascades, we compared the extent to which birds indirectly limit herbivore damage to trees in two lowland Neotropical forests that differed in seasonality of leaf production and rainfall. We compared the effects of bird predation on local arthropod densities and on damage to foliage through a controlled experiment using bird exclosures in the canopy and understory of two forests. We found that birds decreased local arthropod densities and leaf damage in the canopy of the drier site during periods of high leaf production, but not in the wetter forest where leaf production was low and sporadic throughout the year. Birds had no effect on arthropod abundances and leaf damage in the understory where leaf production and turnover rates were low. In support of these experimental interpretations, although we observed that arthropod densities were similar at the two sites, bird densities and the rate at which birds captured arthropods were greater at the drier, seasonally productive site. The influence of top-down predation by birds in limiting herbivorous insects appears to be conditional and most important when the production and turnover of leaves are comparatively high. C1 Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. Univ Illinois, Dept Nat Resources & Environm Sci, Urbana, IL 61801 USA. RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Ancon, Panama. EM vanbaels@si.edu NR 67 TC 16 Z9 17 U1 1 U2 19 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD OCT PY 2005 VL 145 IS 4 BP 658 EP 668 DI 10.1007/s00442-005-0134-0 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 973ZA UT WOS:000232559900016 PM 16315345 ER PT J AU Gastaldo, RA Adendorff, R Bamford, M Labandeira, CC Neveling, J Sims, H AF Gastaldo, RA Adendorff, R Bamford, M Labandeira, CC Neveling, J Sims, H TI Taphonomic trends of macrofloral assemblages across the Permian-Triassic boundary, Karoo Basin, South Africa SO PALAIOS LA English DT Article ID EXTINCTION; CRISIS; EVENT; LAND; ECOSYSTEMS; SUPERGROUP; PATTERNS; COLLAPSE; SYSTEMS; PLANTS AB The terrestrial crisis that reportedly parallels the P/Tr marine mass extinction is based mainly on Northern Hemisphere microfloral assemblages and Southern Hemisphere Goadwanan macrofloral collections. It is well established that taphonomic filters control the ultimate collectable fossil assemblage in any depositional regime. Recognition and comparison of isotaphonomic assemblages are critical before conclusions can be drawn about evolutionary trends over time. Such an approach has been taken in the investigation of pre-boundary, trans-boundary, and post-boundary plant-fossil assemblages in the Karoo Basin, South Africa. Fourteen stratigraphic sections were evaluated in the Balfour and Normandien formations (Lower Beaufort Group), Katberg Formation, and overlying Burgersdorp Formation (Upper Beaufort Group). These include previously published (e.g, Bulwer, Bethulie, Carlton Heights, Wapadsberg, Commando Drift) as well as newly discovered (e.g, Clouston Farm) localities, and span the Late Permian to Middle Triassic. Fossiliferous intervals were characterized with respect to their sedimentology and plant taphonomy, and bulk collections were made at several stratigraphic levels for future evaluation of floristic and plant-insect associational trends. The depositional regimes and plant taphonomic character of assemblages change through time. Much of the Lower Beaufort Group is characterized by parautochthonous assemblages within oxbow-lake channel fills. Below the P/Tr boundary, these are replaced by allochthonous assemblages, poorly preserved in lateral-accretion deposits and barforms of relatively shallow fluvial nature. Allochthonous assemblages within the same fluvial context continue across the boundary into the earliest Triassic (Palingkloof Member and Katberg Formation, and typify the Middle Triassic where scour-and-fill structures preserve plant debris. Based on the literature, parautochthonous assemblages reappear in the Upper Triassic Molteno Formation. Hence, the change in taphonomic regime to poorly preserved allochthonous assemblages (dispersed, fragmentary adpressions) at the critical interval on either side of the P/Tr extinction event, but not coincident with, requires extreme caution when interpreting global patterns from these data. Additionally, the presence of plant fossils in the Early Triassic provides evidence for a vegetated landscape during a time when sedimentation patterns are interpreted to be the result of a land-plant die-off. C1 Colby Coll, Dept Geol, Waterville, ME 04901 USA. Univ Witwatersrand, Bernard Price Inst Palaeontol, ZA-2050 Wits, South Africa. NMNH, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Council Geosci, Pretoria, South Africa. Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. RP Gastaldo, RA (reprint author), Colby Coll, Dept Geol, Waterville, ME 04901 USA. EM ragastal@colby.edu NR 83 TC 39 Z9 40 U1 1 U2 13 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD OCT PY 2005 VL 20 IS 5 BP 479 EP 497 DI 10.2110/palo.2004.P04-62 PG 19 WC Geology; Paleontology SC Geology; Paleontology GA 970LT UT WOS:000232312400007 ER PT J AU Li, RX Squyres, SW Arvidson, RE Archinal, BA Bell, J Cheng, Y Crumpler, L Marais, DJD Di, K Ely, TA Golombek, M Graat, E Grant, J Guinn, J Johnson, A Greeley, R Kirk, RL Maimone, M Matthies, LH Malin, M Parker, T Sims, M Soderblom, LA Thompson, S Wang, J Whelley, P Xu, FL AF Li, RX Squyres, SW Arvidson, RE Archinal, BA Bell, J Cheng, Y Crumpler, L Marais, DJD Di, K Ely, TA Golombek, M Graat, E Grant, J Guinn, J Johnson, A Greeley, R Kirk, RL Maimone, M Matthies, LH Malin, M Parker, T Sims, M Soderblom, LA Thompson, S Wang, J Whelley, P Xu, FL TI Initial results of rover localization and topographic mapping for the 2003 mars exploration rover mission SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID GUSEV CRATER; ORBITER CAMERA; LANDING SITES; SPIRIT ROVER AB This paper presents the initial results of lander and rover localization and topographic mapping of the MER 2003 mission (by Sol 225 for Spirit and Sol 206 for Opportunity). The Spirit rover has traversed a distance of 3.2 km (actual distance traveled instead of odometry) and Opportunity ut 1.2 km. We localized the landers in the Gusev Crater and on the Meridiani Planum using two-way Doppler radio positioning technology and cartographic triangulations through landmarks visible in both orbital and ground images. Additional high-resolution orbital images were taken to verify the determined lander positions. Visual odometry and bundle-adjustment technologies were applied to overcome wheel slippages, azimuthal angle drift and other navigation errors (as large as 21 percent). We generated timely topographic products including 68 orthophoto mops and 3D Digital Terrain Models, eight horizontal rover traverse maps, vertical traverse profiles up to Sol 214 for Spirit and Sol 62 for Opportunity, and five 3D crater models. A web-based landing-site Geographic Information System (GIS) has been set up at The Ohio State University to update and disseminate the daily localization and topographic information to support tactical and strategic operations of the mission. Also described in this paper are applications of the data for science operations planning, geological traverse survey, survey of wind-related features, and other science applications. The majority of the instruments onboard both rovers are healthy at this moment, and they will continue to explore the two landing sites on the Martian surface. We expect to report further localization and topographic mapping results to be achieved in the rest of the mission period and in post-mission data processing. C1 Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. Cornell Univ, Ithaca, NY USA. Washington Univ, St Louis, MO USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. New Mexico Museum Atural Hist & Sci, Albuquerque, NM USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Smithsonian Inst, Washington, DC 20560 USA. Arizona State Univ, Tempe, AZ USA. US Geol Survey, Flagstaff, AZ 86001 USA. Malin Space Sci Syst, San Diego, CA USA. RP Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. EM li282@osu.edu RI Wang, Jue/C-9215-2009; Whelley, Patrick/B-9560-2012 OI Wang, Jue/0000-0002-9901-9996; Whelley, Patrick/0000-0003-3266-9772 NR 34 TC 33 Z9 41 U1 3 U2 8 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 EI 2374-8079 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD OCT PY 2005 VL 71 IS 10 BP 1129 EP 1142 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 972TL UT WOS:000232476000004 ER PT J AU Wang, T Yelin, SF AF Wang, T Yelin, SF TI Theory for Raman superradiance in atomic gases SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATE; RECOIL-INDUCED RESONANCES; MATTER-WAVE AMPLIFICATION; LIGHT-SCATTERING; SUPER-RADIANCE; LASER; SUPERFLUORESCENCE; FERMIONS; SYSTEMS; VAPORS AB A mean field theory for Raman superradiance (SR) with recoil is presented, where the typical SR signatures are recovered, such as quadratic dependence of the intensity on the number of atoms and inverse proportionality of the time scale to the number of atoms. A comparison with recent experiments and theories on Rayleigh SR and collective atomic recoil lasing (CARL) are included. The role of recoil is shown to be in the decay of atomic coherence and breaking of the symmetry of the SR end-fire modes. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Wang, T (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. NR 40 TC 8 Z9 8 U1 2 U2 5 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 OCT PY 2005 VL 72 IS 4 AR 043804 DI 10.1103/PhysRevA.72.043804 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 979HA UT WOS:000232931800137 ER PT J AU Kohri, K Yamaguchi, M Yokoyama, J AF Kohri, K Yamaguchi, M Yokoyama, J TI Neutralino dark matter from heavy gravitino decay SO PHYSICAL REVIEW D LA English DT Article ID BIG-BANG NUCLEOSYNTHESIS; SUPERSYMMETRY BREAKING; LIGHT-ELEMENTS; PRIMORDIAL NUCLEOSYNTHESIS; COSMOLOGICAL IMPLICATIONS; INFLATIONARY UNIVERSE; PARTICLES; CONSTRAINTS; SUPERGRAVITY; MODELS AB We propose a new scenario of nonthermal production of neutralino cold dark matter, in which the overproduction problem of lightest supersymmetric particles (LSPs) in the standard thermal history is naturally solved. The mechanism requires a heavy modulus field which decays mainly to ordinary particles releasing large entropy to dilute gravitinos produced just after inflation and thermal relics of LSPs. Significant amount of gravitinos are also pair-produced at the decay, which subsequently decay into the neutralinos. We identify the regions of the parameter space in which the requisite abundance of the neutralino dark matter is obtained without spoiling the big-bang nucleosynthesis by injection of hadronic showers from gravitino decay. The neutralino abundance obtained in this mechanism is insensitive to the details of the superparticle mass spectrum, unlike the standard thermal abundance. We also briefly mention the testability of the scenario in future experiments. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. Tohoku Univ, Dept Phys, Sendai, Miyagi 9808578, Japan. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 73 TC 36 Z9 36 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 OCT PY 2005 VL 72 IS 8 AR 083510 DI 10.1103/PhysRevD.72.083510 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 979IX UT WOS:000232936700019 ER PT J AU Burns, JM Janzen, DH AF Burns, JM Janzen, DH TI What's in a name? Lepidoptera : Hesperiidae : Pyrginae : Telemiades Hubner 1819 [Pyrdalus Mabille 1903]: New combinations Telemiades corbulo (Stoll) and Telemiades oiclus (Mabille)-and more SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE nomenclature; genitalia (male and female); secondary sex character; facies; mimicry; pupa; caterpillar; foodplants; Fabaceae; Dioclea; Machaerium; Inga; Area de Conservacion Guanacaste; Costa Rica AB Both the Central American skipper butterfly Achlyodes oiclus Mabille and the South American Pyrdalus corbulo (Stoll) belong in Telemiades. Pyrdalus becomes a junior synonym of Telemiades. Pyrdalus corbulo cora Evans, which is really a species (not a subspecies), is a new synonym of Telemiades oiclus, new combination. Though differing sharply in wingshape and color pattern, T. oiclus and Telemiades corbulo, new combination, share a distinctive male secondary sex character and are, in both sexes, genitalically similar to each other and to T. nicomedes (Moschler). Grown caterpillars of T. oiclus and T. nicomedes resemble each other (and suggest slugs). DNA barcoding further supports the relationship of these species. With its brown-forewing/brown-and-yellow-hindwing adult color pattern, T. oiclus superficially resembles 13 other species of skippers reared in the Area de Conservacion Guanacaste (ACG) of northwestern Costa Rica. Of these presumably mimetic species, one is raised from reduction to subspecific rank, and two arc raised from synonymy, to gain reinstated status: T. gallius (Mabille), T. chrysorrhoea (Godman and Salvin), and Eracon lachesis (Dyar). The pupa of T. oiclus shares distinctive features with the pupae of other species of Telemiades. All eight species of Telemiades reared in the ACG feed only on leaves of plants in the family Fabaceae. Six eat various species of Inga and, in a relatively few cases, species in three other mimosoid genera, whereas T. oiclus and T. nicomedes each use two species in one papilionoid genus-Dioclea and Machaerium, respectively. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Entomol, Washington, DC 20013 USA. Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. RP Burns, JM (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Entomol, POB 37012,MRC 127,Room E-515, Washington, DC 20013 USA. EM burnsj@si.edu; djanzen@sas.upenn.edu NR 15 TC 3 Z9 6 U1 2 U2 5 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 OCT PY 2005 VL 107 IS 4 BP 770 EP 781 PG 12 WC Entomology SC Entomology GA 972BM UT WOS:000232428800004 ER PT J AU Mawdsley, JR AF Mawdsley, JR TI Additional historic records of Cicindela dorsalis Say and Cicindela puritana Horn (Coleoptera : Carabidae : Cicindelini) from the Chesapeake Bay region, USA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cicindela dorsalis; Cicindela puritana; tiger beetle; conservation distribution; endangered species ID TIGER BEETLE AB Previously unpublished historic records are presented for two tiger beetle taxa of conservation concern from the Chesapeake Bay region, Cicindela dorsalis Say and C. puritana Horn. Cicindela dorsalis dorsalis was encountered regularly at Chesapeake Bay sites by collectors during the 1940s and 1950s, when other populations of this subspecies were experiencing a severe decline. The historic presence of C. dorsalis media LeConte in the southern Chesapeake Bay is documented by specimens collected in 1882. Cicindela puritana has been collected regularly at sites in Calvert County, Maryland, since 1911, sometimes in large numbers. Both C. d. dorsalis and C puritana are currently listed as "Threatened" under the U.S. Endangered Species Act. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Mawdsley, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 187, Washington, DC 20013 USA. EM mawdsley@nfwf.org NR 14 TC 1 Z9 1 U1 2 U2 6 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 OCT PY 2005 VL 107 IS 4 BP 808 EP 811 PG 4 WC Entomology SC Entomology GA 972BM UT WOS:000232428800007 ER PT J AU Smith, DR AF Smith, DR TI Review of the Aulacidae (Hymenoptera) of Chile and adjacent Argentina SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE parasitoids; new species; key; Cerambycidae; South America; Juan Fernandez Islands AB Five species of Aulacidae occur in Chile: Aulacus braconiformis (Kieffer). A. krahmeri Elgueta and Lanfranco, A. brevis, n. sp., Pristaulacus capitalis (Schletterer), and P. rubriventer (Philippi). Two of these, A, krahmeri and A. brevis, occur in adjacent Argentina. Aulacus brevis also is recorded from the Juan Fernandez Islands. A key to species is presented and diagnoses and new distribution records are given. Hosts are wood-boring beetles of the family Cerambycidae. C1 Smithsonian Inst, USDA, ARS, PSI,Systemat Entomol Lab,Natl Museum Nat Hist, Washington, DC 20013 USA. RP Smith, DR (reprint author), Smithsonian Inst, USDA, ARS, PSI,Systemat Entomol Lab,Natl Museum Nat Hist, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov NR 10 TC 13 Z9 16 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 OCT PY 2005 VL 107 IS 4 BP 820 EP 834 PG 15 WC Entomology SC Entomology GA 972BM UT WOS:000232428800009 ER PT J AU Smith, DR Schiff, NM AF Smith, DR Schiff, NM TI A new Western Nearctic species of Calameuta Konow (Hymenoptera : Cephidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cephinae; grasses; California; Oregon AB Calameuta middlekauffi, n. sp., is described from southern Oregon and California. It is the second species of Calameuta in North America and is differentiated from C. clavata (Norton) by head shape and coloration. Illustrations, descriptions, and a key are given to separate the two species. The food plant is unknown, but Palearctic species of Calameuta are known to feed in grass stems. C1 Smithsonian Inst, Systemat Entomol Lab, PSI, ARS,USDA,Natl Museum Nat Hist, Washington, DC 20013 USA. USDA ARS, So Res Stn, Ctr Bottomland Hardwood Res, Stoneville, MS 38776 USA. RP Smith, DR (reprint author), Smithsonian Inst, Systemat Entomol Lab, PSI, ARS,USDA,Natl Museum Nat Hist, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov; nschiff@fs.fed.us NR 5 TC 3 Z9 4 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2005 VL 107 IS 4 BP 864 EP 868 PG 5 WC Entomology SC Entomology GA 972BM UT WOS:000232428800014 ER PT J AU Razowski, J Brown, JW AF Razowski, J Brown, JW TI Review of Oregocerata Razowski (Lepidoptera : Tortricidae : Euliini) with descriptions of four new species SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE Tortricinae; systematics; Andes; Colombia; Ecuador; Bolivia; Venezuela AB Oregocerata is a poorly known genus restricted to the Andes and its associated ranges in northwestern South America (i.e., Colombia, Venezuela, Ecuador, Bolivia) usually above 2000 m. Specimens are exceedingly rare in collections; most species are known only from the holotype mate. We describe and illustrate four new species: O. triangulana (TL: Colombia), O. caucana (TL: Colombia), O. quadrifurcata (TL: Colombia), and O. submontana (TL: Venezuela); and we propose a new combination, Oregocerata chrysodetis (Meyrick). As currently defined the genus includes 9 species. It is assigned to Euliini on the basis of the possession of a characteristic hairpencil on the prothoracic leg. C1 Polish Acad Sci, Inst Systemat Zool, Krakow, Poland. Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, PSI,USDA ARS, Washington, DC 20013 USA. RP Razowski, J (reprint author), Polish Acad Sci, Inst Systemat Zool, Slawkowska 17, Krakow, Poland. EM brown@sel.barc.usda.gov NR 8 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 OCT PY 2005 VL 107 IS 4 BP 903 EP 913 PG 11 WC Entomology SC Entomology GA 972BM UT WOS:000232428800019 ER PT J AU Hall, JPW Willmott, KR AF Hall, JPW Willmott, KR TI A new species of Paiwarria (Lepidoptera : Lycaenidae : Eumaeini) from Western Ecuador SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Andes; Colombia; Ecuador; Fasslantonius; Paiwarria; P. episcopalis AB A new eumaeine lycaenid species, Paiwarria chuchuvia, n. sp., is described,and illustrated from wet premontane forest in the western Ecuadorian Andes. Its sister species, Paiwarria episcopalis (Fassl), appears to be distributed allopatrically in the central and eastern Andes. The generic placement of both species is discussed. C1 Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. Univ Florida, Florida Museum Nat Hist, McGuire Ctr Lepidoptera & Biodivers, Gainesville, FL 32611 USA. RP Hall, JPW (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. EM hallja@si.edu; kwillmott@flmnh.ufl.edu NR 23 TC 2 Z9 5 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 OCT PY 2005 VL 107 IS 4 BP 960 EP 967 PG 8 WC Entomology SC Entomology GA 972BM UT WOS:000232428800024 ER PT J AU Sozzetti, A AF Sozzetti, A TI Astrometric methods and instrumentation to identify and characterize extrasolar planets: A review SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Review ID PALOMAR TESTBED INTERFEROMETER; GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; III STELLAR INTERFEROMETER; NARROW-ANGLE ASTROMETRY; RELATIVISTIC SATELLITE ASTROMETRY; BASE-LINE INTERFEROMETRY; DETECTING OUTER PLANETS; MAIN-SEQUENCE STARS; GAS GIANT PLANETS AB I present a review of astrometric techniques and instrumentation used to search for, detect, and characterize extrasolar planets. First, I briefly summarize the properties of the current sample of extrasolar planets, in connection with predictions from theoretical models of planet formation and evolution. Next, the generic approach to planet detection with astrometry is described, with significant discussion of a variety of technical, statistical, and astrophysical issues to be faced by future ground-based and space-borne efforts in order to achieve the required degree of measurement precision. After a brief summary of past and present efforts to detect planets via milliarcsecond astrometry, I then discuss the planet-finding capabilities of future astrometric observatories aiming at microarcsecond precision. Finally, I outline a number of experiments that can be conducted by means of high-precision astrometry during the next decade, to illustrate its potential for important contributions to planetary science, compared to other indirect and direct methods for the detection and characterization of planetary systems. C1 Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. EM asozzetti@cfa.harvard.edu OI Sozzetti, Alessandro/0000-0002-7504-365X NR 275 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT PY 2005 VL 117 IS 836 BP 1021 EP 1048 DI 10.1086/444487 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 968QC UT WOS:000232176100001 ER PT J AU Krings, M Klavins, SD DiMichele, WA Kerp, H Taylor, TN AF Krings, M Klavins, SD DiMichele, WA Kerp, H Taylor, TN TI Epidermal anatomy of Glenopteris splendens Sellards nov emend., an enigmatic seed plant from the Lower Permian of Kansas (USA) SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article DE adaptation; aridity; Artinskian; cuticular analysis; ecology; Glenopteris; Peltaspermales; salinity; succulence; Wellington Formation ID NORTH-CENTRAL TEXAS; PTERIDOSPERM CUTICLES; ADAPTIVE SIGNIFICANCE; TRICHOMES; LEAVES; WATER; PUBESCENCE; DEFENSE; FLORA AB Frond morphology and epidermal anatomy of the enigmatic late Early Permian seed plant Glenopteris splendens Sellards are described based on material from east central Kansas (Wellington Formation, Sumner Group; Artinskian ICS Stage). The specific diagnosis for G. splendens Sellards, 1900 is emended. Frond morphology suggests that G. splendens is a member of the seed plant order Peltaspermales. Macroscopical and epidermal features of G. splendens are consistent with those extant plants adapted to (seasonal) moisture limitation and elevated soil and ground water salinity. For example, the pachymorphous (succulent) pinnules may help mitigate water stress, because succulent foliage delivers large quantities of storage water, but could also be an adaptation to elevated salinity since storage of large quantities of water increases the salt accumulation capacity of the fronds. Wart- and peg-like cuticular projections may represent an adaptation to (seasonal) moisture limitation because extant xeromorpbic plants have similar heavily cutinized anticlinal cell walls. Glenopteris splendens fronds are entirely glabrous, which suggests that epidermal outgrowths were not necessary as protective elements against deleterious environmental influences. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Munich, Bayer Staatssammlung Palaontol & Geol & GeoBio Ct, D-80333 Munich, Germany. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Univ Kansas, Museum Nat Hist, Lawrence, KS 66045 USA. Univ Kansas, Biodivers Res Ctr, Lawrence, KS 66045 USA. Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. Univ Munster, Forsch Stelle Palaobot Geol, Palaontol Inst, D-48143 Munster, Germany. RP Krings, M (reprint author), Univ Munich, Bayer Staatssammlung Palaontol & Geol & GeoBio Ct, Richard Wagner Str 10, D-80333 Munich, Germany. EM m.krings@lrz.uni-muenchen.de RI DiMichele, William/K-4301-2012 NR 81 TC 17 Z9 17 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD OCT PY 2005 VL 136 IS 3-4 BP 159 EP 180 DI 10.1016/j.revpalbo.2005.07.002 PG 22 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 974JJ UT WOS:000232587300003 ER PT J AU Sallum, MAM Peyton, EL Harrison, BA Wilkerson, RC AF Sallum, MAM Peyton, EL Harrison, BA Wilkerson, RC TI Revision of the Leucosphyrus group of Anopheles (Cellia) (Diptera, Culicidae) SO REVISTA BRASILEIRA DE ENTOMOLOGIA LA English DT Review DE Anophelinae; Cellia; distribution; morphology; revision; taxonomy ID BALABACENSIS-BALABACENSIS MOSQUITOES; POLYMERASE-CHAIN-REACTION; DIRUS COMPLEX; SOUTHEAST-ASIA; SIMIAN-MALARIA; SPECIES-B; PLASMODIUM-KNOWLESI; FOREST MALARIA; MONKEY MALARIA; COMPARATIVE SUSCEPTIBILITY AB Revision of the Leucosphyrus Group of Anopheles (Cellia) (Diptera, Culicidae). This is a comprehensive revision of 20 species of the Leucosphyrus Group of the Neomyzomyia Series of Anopheles (Cellia). Morphological description of the adults, male and female, male genitalia, pupa and fourth-instar larva are provided for each taxon in addition to bionomics, distribution data and systematic discussion for each species, including diagnostic characters. Identification keys for females and fourth-instar larvae are provided. When possible medical importance of each species is included. Illustrations of of the adults, fourth-instar larvae and pupae are provided. Distribution maps for each species are mainly based on the material examined; however, when possible published data were also used. Tables on adult character variations, fourth-instar larval and pupal setal branching are included as appendices. A neotype for An. takasagoensis Morishita and Aii. sulawesi Koesoemawinangoen, and a lectotype for An. balabacensis Baisas, are designated. The authorship of Aii. snlowesi previously cited as Waktoedi is corrected to Koesoemawinangoen. C1 Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Dept Entomol, Suitland, MD 20746 USA. Univ Sao Paulo, Fac Saude Publ, BR-01246904 Sao Paulo, Brazil. NC DENR Publ Hlth Pest Management, Winston Salem, NC 27107 USA. RP Sallum, MAM (reprint author), Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Dept Entomol, 4210 Silver Hill Rd, Suitland, MD 20746 USA. RI Sallum, Maria/B-8537-2012 NR 440 TC 34 Z9 35 U1 1 U2 5 PU SOC BRASILEIRA ENTOMOLOGIA PI CURITIBA PA CAIXA POSTAL 19030, CURITIBA, PR 81531-980, BRAZIL SN 0085-5626 EI 1806-9665 J9 REV BRAS ENTOMOL JI Rev. Bras. Entomol. PD OCT-DEC PY 2005 VL 49 SU 1 BP 1 EP 152 DI 10.1590/S0085-56262005000500001 PG 152 WC Entomology SC Entomology GA 999XP UT WOS:000234425200001 ER PT J AU Goldberg, A Alden, HA AF Goldberg, A Alden, HA TI Taxonomy of Haptanthus Goldberg & C. Nelson SO SYSTEMATIC BOTANY LA English DT Article AB Haptanthus is known from only a single collection despite several attempts to recollect it. Because of its unique inflorescence and flowers, and the specimen's lack of fruit, the original authors were unable to assign it to an existing family. After 12 years Nelson described it as the type of a new family, Haptanthaceae. The original authors mainly described and illustrated the gross morphology, pistil anatomy, and pollen of Haptanthus. In attempting to assign it to a family, eight familial placements were considered and reasons were given for their rejection. In the present paper additional characters of the leaf, stem, and pistil, mainly anatomical, are described and illustrated. Most of the wood characters are archaic (primitive). Haptanthus has a suite of characters indicating that it is probably wind-pollinated. Consideration of all the characters studied to date, and examination of additional literature and herbarium specimens of several families, enable us to suggest Flacourtiaceae and Euphorbiaceae as the closest relatives of Haptanthaceae. Recently, Flacourtiaceae has been suggested by another author. Key characters of the three families are compared in a table. C1 Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. Smithsonian Ctr Mat Res & Educ, Museum Support Ctr, Suitland, MD 20746 USA. RP Goldberg, A (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC-166,POB 37012, Washington, DC 20013 USA. NR 6 TC 5 Z9 6 U1 0 U2 0 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2005 VL 30 IS 4 BP 773 EP 778 DI 10.1600/036364405775097815 PG 6 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 994JC UT WOS:000234026700008 ER PT J AU Terrell, EE Robinson, HE Wagner, WL Lorence, DH AF Terrell, EE Robinson, HE Wagner, WL Lorence, DH TI Resurrection of genus Kadua for Hawaiian Hedyotidinae (Rubiaceae), with emphasis on seed and fruit characters and notes on South Pacific species SO SYSTEMATIC BOTANY LA English DT Article AB We examined shapes and surface features of seeds of 19 species of Hawaiian Hedyotideae using scanning electron microscopy. The study concentrates on the Hedyotideae previously recognized in the genus Hedyotis and here recognized as the genus Kadua, lacking diplophragmous capsules, and having salverform, fleshy corollas with appendaged lobes. The seeds fell into four main morphological groups: (1) hat- or fan-shaped, laterally cuneate, compressed seeds (Kadua subg. Kadua and atypical species of Gouldiopsis and Wiegmannia); (2) ovoid or elliptic seeds with conspicuous bubble-shaped bodies included in the areoles (cells) (most of sect. Wiegmannia); (3) flat broadly winged seeds with a lateral hilum attached at wing margin (Kadua centranthoides, type species of sect. Gouldiopsis); (4) brick-like or blocky seeds with a centric ventral hilum (Kadua subg. Gouldia). The results of the seed study correlate with the taxonomic arrangement in the current Hawaiian flora. An appendix lists the Kadua names including necessary new combinations and their Hedyotis synonyms for the Hawaiian taxa and seven additional South Pacific taxa having the same corolla characters. The following new names are published: Kadua subg. Gouldia (A. Gray) W. L. Wagner & Lorence, Kadua sect. Gouldia (A. Gray) W. L. Wagner & Lorence, Kadua fosbergii (W. L. Wagner & a R. Herbst) W. L. Wagner & Lorence, Kadua axillaris (Wawra) W L. Wagner & Lorence, Kadua sect. Phyllozygia (W. L. Wagner & Herbst) W. L. Wagner & Lorence, Kadua tryblium (D. R. Herbst & W. L. Wagner) W. L. Wagner & Lorence, Kadua sect. Oceanica (Fasberg) W. L. Wagner & Lorence, Kadua sect. Austrogouldia (Fosberg) W. L. Wagner & Lorence, Kadua lucei (Lorence & J. Florence) W. L. Wagner & Lorence, Kadua nukuhivensis (J. Florence & Lorence) W L. Wagner & Lorence, Kadua tahuatensis (Lorence & J. Florence) W. L. Wagner & Lorence, Kadua grantii (Fosberg) W. L. Wagner & Lorence, Kadua sect. Protokadua (Fosberg) W L. Wagner & Lorence, Kadua coriacea (J. E. Smith) W. L. Wagner & Lorence, Kadua sect. Gouldiopsis (Fosberg) W. L. Wagner & Lorence, Kadua foggiaria (Fosberg) W L. Wagner & Lorence, Kadua sect. Wiegmannia (Meyen) W. L. Wagner & Lorence, Kadua cordata Cham & Schltdl. subsp. remyi (Hillebr.) W L. Wagner & Lorence, Kadua cordata Cham & Schltdl. subsp. waimeae (Wawra) W. L. Wagner & Lorence, Kadua degeneri (Fosberg) W. L. Wagner & Lorence, Kadua degeneri (Fosberg) W L. Wagner & Lorence subsp. coprosmifolia (Fosberg) W. L. Wagner & Lorence, Kadua elatior (H. Mann) W. L. Wagner & Lorence, Kadua flynnii (W. L. Wagner & Lorence) W. L. Wagner & Lorence, and Kadua st-johnii (B. C. Stone & Lane) W. L. Wagner & Lorence. C1 Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Natl Trop Bot Garden, Kauai, HI 96741 USA. RP Terrell, EE (reprint author), 14001 Wildwood Dr, Silver Spring, MD 20905 USA. EM terr60@msn.com NR 20 TC 10 Z9 15 U1 0 U2 3 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2005 VL 30 IS 4 BP 818 EP 833 DI 10.1600/036364405775097716 PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 994JC UT WOS:000234026700013 ER PT J AU Mitchell, A Wen, J AF Mitchell, A Wen, J TI Phylogeny of Brassaiopsis (Araliaceae) in Asia based on nuclear ITS and 5S-NTS DNA sequences SO SYSTEMATIC BOTANY LA English DT Article ID CHAIN MONTE-CARLO; RIBOSOMAL DNA; MOLECULAR SEQUENCES; INFERENCE; BIOGEOGRAPHY; EVOLUTION; GENUS; CALLISTEMON; MELALEUCA; APIACEAE AB The phylogeny of Brassaiopsis (Araliaceae), a morphologically diverse and widely distributed genus in Asia, was estimated based on sequences of the internal transcribed spacer regions (ITS) and 5S nontranscribed spacer (5S-NTS) of the nuclear ribosomal DNA. Two main paralogous copies of 5S-NTS were found for Brassaiopsis but both were not recovered for all species. All but one species of Brassaiopsis was represented by 5S-NTS (copy 1). Separate parsimony analyses of ITS and 5S-NTS (copy 1) generated largely congruent topologies, but several paralogous 5S-NTS sequences precluded data combination. A sister relationship of Brassaiopsis with Trevesia was strongly inferred. The divergence of Brassaiopsis from Trevesia was estimated to have occurred ca. 20 million years ago (MYA) during a period of mountain building and climatic change in SE Asia. Our analysis suggests a rapid evolutionary radiation of Brassaiopsis in the Sino-Himalayan region and Indochina at ca. 8 MYA. Several clades within the genus were circumscribed based on ITS and 5S-NTS analyses: 1) B. aculeata, B. glomerulata, and B. hainla; 2) B. gigantea, B. grushvitzkyi, B. moumingensis, and B. stellata; 3) B. ciliata and B. hispida; 4) B. fatsioides and B. palmipes; and 5) B. gracilis and B. phanerophlebia. Brassaiopsis producta is morphologically unique in possessing a 3-5-locular ovary, and its phylogenetic position was not well resolved in either analysis. Morphological characters previously considered important for defining species and subgeneric groups were shown to have had multiple origins (e.g., leaf architecture and locule number in the ovary). The Brassaiopsis phylogeny supports strong biogeographic connections between S China and Indochina, S China and SW China, and SW China and the eastern Himalayas. C1 Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. Chinese Acad Sci, Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. Chinese Acad Sci, Herbarium, Inst Bot, Beijing 100093, Peoples R China. RP Mitchell, A (reprint author), Smithsonian Inst, Dept Bot, MRC-166,POB 37012, Washington, DC 20013 USA. EM anthony@inet.net.nz; wenj@NMNH.si.org NR 81 TC 11 Z9 14 U1 1 U2 9 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2005 VL 30 IS 4 BP 872 EP 886 DI 10.1600/036364405775097761 PG 15 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 994JC UT WOS:000234026700016 ER PT J AU Agnarsson, I Kuntner, M AF Agnarsson, I Kuntner, M TI Madagascar: an unexpected hotspot of social Anelosimus spider diversity (Araneae : Theridiidae) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID STUDIOSUS ARANEAE; SUBSOCIAL SPIDER; NATAL DISPERSAL; SEX-RATIO; EVOLUTION; GENUS; KLEPTOPARASITISM; PHYLOGENY; BENEFITS; BEHAVIOR AB The spider genus Anelosimus Simon, 1891 (Theridiidae) currently contains over forty described species, found worldwide in tropical to warm temperate areas. American Anelosimus are all social, a rare trait among spiders, but social behaviour has not been reported for Anelosimus species elsewhere. Old World Anelosimus are poorly known, both behaviourally and taxonomically, and no Anelosimus species have yet been described from sub-Saharan Africa or Madagascar. Based on a preliminary phylogenetic analysis we predicted sociality in an undescribed Madagascar species because it grouped among social New World species. An expedition to Madagascar then found no less than five undescribed periodic-social (subsocial) Anelosimus species in Perinet reserve. A sixth species from the same locality is known from museum specimens and the Anelosimus diversity of Perinet is comparable with the most diverse single locality in the Americas. Subsocial species play a key role in understanding the evolution of permanent sociality (quasisociality). This increased pool of available subsocial study species demonstrates the utility of phylogenies as predictors of traits in species thus far unstudied. Here, A. andasibesp.n., A. may Agnarsson sp.n., A. nazarianisp.n., A. salleesp.n., A. salutsp.n. and A. vondronasp.n. are described. Anelosimus locketi Roberts, 1977 from Aldabra Atoll is a junior synonym of A. decaryi (Fage, 1930) comb.n. from Madagascar. Preliminary data on the behaviour of the new species are given, indicating a level of sociality similar to the American A.'arizona'(1). The phylogenetic analysis supports the monophyly of the Madagascar group and places it as sister to a clade containing the eximius lineage from the Americas, and a pair of undescribed Tanzanian species. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Agnarsson, I (reprint author), Smithsonian Inst, Dept Entomol, NHB 105,POB 37012, Washington, DC 20013 USA. EM ingi@zoology.ubc.ca NR 37 TC 30 Z9 33 U1 1 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD OCT PY 2005 VL 30 IS 4 BP 575 EP 592 DI 10.1111/j.1365-3113.2005.00289.x PG 18 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 972ZF UT WOS:000232491700005 ER PT J AU Brady, SG Ward, PS AF Brady, SG Ward, PS TI Morphological phylogeny of army ants and other dorylomorphs (Hymenoptera : Formicidae) SO SYSTEMATIC ENTOMOLOGY LA English DT Review ID GENUS LEPTANILLA HYMENOPTERA; ANCESTRAL CHARACTER STATES; HIGHER-LEVEL TAXA; MISSING DATA; MADAGASCAR HYMENOPTERA; CHELIOMYRMEX-MOROSUS; REPRODUCTIVE-SYSTEM; METATIBIAL GLAND; INCOMPLETE TAXA; PRIMITIVE ANTS AB The dorylomorph group of ants comprises the three subfamilies of army ants (Aenictinae, Dorylinae, Ecitoninae) together with the subfamilies Aenictogitoninae, Cerapachyinae, and Leptanilloidinae. We describe new morphological characters and synthesize data from the literature in order to present the first hypothesis of phylogenetic relationships among all dorylomorph genera. These data include the first available character information from the newly discovered male caste of Leptanilloidinae. We used ant taxa from Leptanillinae, Myrmeciinae, and the poneromorph (Ponerinae sensu lato) subfamilies Amblyoponinae, Ectatomminae, and Paraponerinae as outgroups. We scored a total of 126 characters from twenty-two terminal taxa and used these data to conduct maximum parsimony and bootstrap analyses. The single most-parsimonious tree and bootstrap results support a single origin of army ants. The Old World army ant genus Dorylus forms a monophyletic group with the enigmatic genus Aenictogiton, which is currently known only from males; the second Old World army ant genus Aenictus is sister to this clade. This result generates the prediction that females of Aenictogiton, when discovered, will be observed to possess the army ant syndrome of behavioural and reproductive traits. The monophyly of the New World army ants (Ecitoninae) is supported very strongly, and within this group the genera Eciton, Nomamyrmex, and Labidus form a robust clade. The monophyly of Leptanilloidinae is also upheld. The subfamily Cerapachyinae appears paraphyletic, although this conclusion is not supported by strong bootstrap results. Relationships among genera of Cerapachyinae similarly are not resolved robustly, although parsimony results suggest clades consisting of (Acanthostichus + Cylindromyrmex) and (Cerapachys + Sphinctomyrmex). We tested for the effect of incompletely known taxa by conducting a secondary analysis in which the two genera containing similar to 50% missing character data (Aenictogiton and Asphinctanilloides) were removed. The strict consensus of the seventeen most-parsimonious trees from this secondary analysis is poorly resolved outside the army ants and contains no clades conflicting with the primary analysis. The position of Leptanilla shifts from forming the sister group to Leptanilloidinae (without high bootstrap support) in the primary analysis, to falling within a polytomy at the base of the root of the dorylomorphs when incompletely known taxa are removed. This instability suggests that the placement of Leptanilla within the dorylomorphs in our primary analysis may be spurious. C1 Smithsonian Inst, Labs Analyt Biol, Dept Entomol, Natl Museum Nat Hist, Suitland, MD 20746 USA. Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA. RP Brady, SG (reprint author), Smithsonian Inst, Labs Analyt Biol, Dept Entomol, Natl Museum Nat Hist, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM sbrady@lab.si.edu NR 160 TC 28 Z9 30 U1 1 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD OCT PY 2005 VL 30 IS 4 BP 593 EP 618 DI 10.1111/j.1365-3113.2005.00290.x PG 26 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 972ZF UT WOS:000232491700006 ER PT J AU Molella, AP AF Molella, AP TI The longue duree of Abbott Payson Usher - A. P. Usher, A History of Mechanical Inventions SO TECHNOLOGY AND CULTURE LA English DT Article C1 Natl Museum Amer Hist, Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. RP Molella, AP (reprint author), Natl Museum Amer Hist, Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. NR 24 TC 3 Z9 3 U1 1 U2 2 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2005 VL 46 IS 4 BP 779 EP 796 DI 10.1353/tech.2006.0027 PG 18 WC History & Philosophy Of Science SC History & Philosophy of Science GA 997ZW UT WOS:000234288600005 ER PT J AU Hacker, BC AF Hacker, BC TI Gunpowder and firearms: Warfare in medieval India. 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 OCT PY 2005 VL 46 IS 4 BP 880 EP 881 DI 10.1353/tech.2006.0013 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 997ZW UT WOS:000234288600048 ER PT J AU Hacker, BC AF Hacker, BC TI Warfare and weaponry in South Asia: 1000-1800. 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 OCT PY 2005 VL 46 IS 4 BP 880 EP 881 DI 10.1353/tech.2006.0013 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 997ZW UT WOS:000234288600049 ER PT J AU Wright, SJ AF Wright, SJ TI Tropical forests in a changing environment SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID LONG-TERM PLOTS; RAIN-FOREST; TREE GROWTH; BRAZILIAN AMAZONIA; SOLAR-RADIATION; LOWLAND FOREST; CLIMATE-CHANGE; ELEVATED CO2; DEFORESTATION; BIODIVERSITY AB Understanding and mitigating the impact of an ever-increasing population and global economic activity on tropical forests is one of the great challenges currently facing biologists, conservationists and policy makers. Tropical forests currently face obvious regional changes, both negative and positive, and uncertain global changes. Although deforestation rates have increased to unprecedented levels, natural secondary succession has reclaimed approximately 15% of the area deforested during the 1990s. Governments have also protected 18% of the remaining tropical moist forest; however, unsustainable hunting continues to threaten many keystone mammal and bird species. The structure and dynamics of old-growth forests appear to be rapidly changing, suggesting that there is a pantropical response to global anthropogenic forcing, although the evidence comes almost exclusively from censuses of tree plots and is controversial. Here, I address ongoing anthropogenic change in tropical forests and suggest how these forests might respond to increasing anthropogenic pressure. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 74 TC 333 Z9 346 U1 30 U2 223 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 OCT PY 2005 VL 20 IS 10 BP 553 EP 560 DI 10.1016/j.tree.2005.07.009 PG 8 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 974QQ UT WOS:000232606900007 PM 16701434 ER PT J AU Scharler, UM Baird, D AF Scharler, UM Baird, D TI The filtering capacity of selected Eastern Cape estuaries, South Africa SO WATER SA LA English DT Article DE filtering capacity of estuaries; nutrient loading; phosphate; nitrate; nitrite; ammonia; South Africa ID GAMTOOS ESTUARY; COASTAL WATERS; NUTRIENTS; NITROGEN; EUTROPHICATION; MANAGEMENT; TRANSPORT; RESPONSES; SALINITY; BIOMASS AB Four Eastern Cape estuaries, the Kromme, Gamtoos, Swartkops and Sundays Estuaries have a permanent connection to the adjacent ocean, but differ in the amount of freshwater inflows as well as in the land-use patterns in their respective catchment areas. The nutrient loading to the four estuaries in terms of phosphate, nitrate, nitrite and ammonia therefore varies. The aim of the study was to show how the nutrient loads received by the estuaries differ, and how they act as filters for nutrients. Discriminant analysis revealed such contrasts: The lower reaches of the four estuaries are similar in their inorganic nutrient concentrations, but concentrations diverge in their upper reaches and in the inflowing river water. C1 Nelson Mandela Metropolitan Univ, Dept Zool, ZA-6031 Port Elizabeth, South Africa. Univ Maryland, Ctr Environm Studies, Chesapeake Biol Lab, Solomons, MD 20688 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Baird, D (reprint author), Nelson Mandela Metropolitan Univ, Dept Zool, POB 77000, ZA-6031 Port Elizabeth, South Africa. EM dan.baird@nmmu.ac.za RI Scharler, Ursula/F-3598-2010 NR 49 TC 3 Z9 3 U1 0 U2 4 PU WATER RESEARCH COMMISSION PI PRETORIA PA PO BOX 824, PRETORIA 0001, SOUTH AFRICA SN 0378-4738 J9 WATER SA JI Water SA PD OCT PY 2005 VL 31 IS 4 BP 483 EP 490 PG 8 WC Water Resources SC Water Resources GA 990JX UT WOS:000233740200008 ER PT J AU Konstantinov, AS AF Konstantinov, AS TI New species of Middle Asian Longitarsus Latreille with discussion of their subgeneric placement (Coleoptera : Chrysomelidae) SO ZOOTAXA LA English DT Article DE Chrysomelidae; flea beetle; Longitarsus; Testergus; Truncatus AB The subgenus Testergus Weise of Longitarsus Latreille is redefined based on the characters of male genitalia and four new species are described and illustrated: L. borisi sp. nov. (Tadzhikistan), L. danilevskyi sp. nov. (Kazakhstan), L. igori sp. nov. (Tadzhikistan), and L. nadiae sp. nov. (Kirgizstan). The lectotypes for L. fuscoaeneus Redtenbacher, L. tmetopterus Jacobson and L. nurataicus Palij are designated. A key to the known Testergus species from Greece, Caucasus and Middle Asia is provided. C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20013 USA. RP Konstantinov, AS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM akonstan@sel.barc.usda.gov 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 SEP 30 PY 2005 IS 1056 BP 19 EP 42 PG 24 WC Zoology SC Zoology GA 968ZY UT WOS:000232204400002 ER PT J AU Falco, EE AF Falco, EE TI A most useful manifestation of relativity: gravitational lenses SO NEW JOURNAL OF PHYSICS LA English DT Article ID TIME-DELAY; ELLIPTIC GALAXIES; DARK-MATTER; BOSON STARS; QUASAR; IMAGE; SUBSTRUCTURE; PARAMETERS; Q0957+561; EVOLUTION AB Gravitational lenses are scarce but extraordinary phenomena that yield a very high rate of return on observational investment. Given their scarcity, it is very impressive that since their discovery in the extragalactic realm in 1979, they have had such an enormous impact on our knowledge of the universe. Gravitational lensing is a manifestation of general relativity that has contributed to a great variety of astrophysical and cosmological studies. In the weak-field limit, lensing studies are based on well-established physics and thus offer a direct approach to study many of the currently pressing problems of astrophysics. Examples of these are the significance of dark matter and the age and size of the universe. I present a brief history of gravitational lensing and describe recent developments in fields such as searches for dark matter and studies of galaxy evolution and cosmology. The approach is non-specialized and emphasizes observational results, to reach the widest possible audience. C1 Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. RP Falco, EE (reprint author), Smithsonian Inst, FL Whipple Observ, POB 97, Amado, AZ 85645 USA. EM falco@cfa.harvard.edu NR 71 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD SEP 29 PY 2005 VL 7 AR 200 DI 10.1088/1367-2630/7/1/200 PG 25 WC Physics, Multidisciplinary SC Physics GA 971FR UT WOS:000232370100003 ER PT J AU Narayan, R AF Narayan, R TI Black holes in astrophysics SO NEW JOURNAL OF PHYSICS LA English DT Review ID ADVECTION-DOMINATED ACCRETION; X-RAY-BURSTS; SAGITTARIUS-A-ASTERISK; MICROQUASAR GRO J1655-40; EVENT-HORIZON; NEUTRON-STAR; XMM-NEWTON; GALACTIC NUCLEI; MAGNETICALLY DRIVEN; RELATIVISTIC JETS AB This paper reviews the current status of black hole (BH) astrophysics, focusing on topics of interest to a physics audience. Astronomers have discovered dozens of compact objects with masses greater than 3M(.), the likely maximum mass of a neutron star. These objects are identified as BH candidates. Some of the candidates have masses similar to 5M(.)- 20M(.) and are found in x-ray binaries, while the rest have masses similar to 10(6)M(.) - 10(9.5)M(.) and are found in galactic nuclei. A variety of methods are being tried to estimate the spin parameters of the candidate BHs. There is strong circumstantial evidence that many of the objects have event horizons, so there is good reason to believe that the candidates are true BHs. Recent MHD simulations of magnetized plasma accreting on rotating BHs seem to hint that relativistic jets may be produced by a magnetic analogue of the Penrose process. C1 Harvard Smithsonian Ctr Astrophys, Harvard Coll Observ, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, Harvard Coll Observ, 60 Garden St, Cambridge, MA 02138 USA. EM rnarayan@cfa.harvard.edu NR 109 TC 95 Z9 95 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD SEP 29 PY 2005 VL 7 AR 199 DI 10.1088/1367-2630/7/1/199 PG 20 WC Physics, Multidisciplinary SC Physics GA 971FR UT WOS:000232370100002 ER PT J AU Nichols, SA Barnes, PAG AF Nichols, SA Barnes, PAG TI A molecular phylogeny and historical biogeography of the marine sponge genus Placospongia (Phylum Porifera) indicate low dispersal capabilities and widespread crypsis SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE biogeography; cosmopolitanism; crypsis; dispersal; phylogeny; porifera ID CRYPTIC SPECIATION; INTRAGENOMIC VARIATION; LARVAL BEHAVIOR; PANAMA; DEMOSPONGIAE; ISTHMUS; DNA; RECRUITMENT; POPULATIONS; SYSTEMATICS AB Very little is known about the dispersal of marine sponges but hypotheses based upon observations of larval life suggest limited dispersal ability. Until recently, the diversity of dispersal mechanisms employed by different species, coupled with the putative cosmopolitan distribution of some species, suggested that short larval life may not limit sponge dispersal. However, recent studies have found that "cosmopolitan species" frequently represent morphologically cryptic species complexes. Here, the historical biogeography of the circum-tropical marine sponge genus Placospongia is investigated using sequence data from the internal transcribed spacer region (ITS). ITS is the predominant marker used for fine-scale investigations in sponges (and many other taxa), but problems with paralogy (divergent copies within individual genomes) have brought the utility of this marker into question. Ninety-eight ITS subclones were sequenced from twenty-eight individuals of Placospongia sampled from twelve localities worldwide. Divergent ITS paralogs were detected but the data still reflected geographic (and presumably phylogenetic) structure. Placospongia populations sampled were found to harbor at least 9 unique evolutionary lineages, several of which are sympatrically distributed but morphologically indistinguishable, Most of the relationships reconstructed are consistent with the hypothesis that marine sponges do not disperse very far (by any means). Nevertheless, phylogenetic divergences between lineages were not clearly consistent with modem, or historical, geological or oceanographic processes. No component of the phylogeny presented clearly reflected the geological event of the rising of this Isthmus of Panama and populations from marine lakes in Indonesia were found to be indistinguishable from populations in the Seychelles. These biogeographically anomalous results highlight that ITS is useful as a tool to identify interesting preliminary patterns in widespread groups, but that these patterns should be tested using multiple independent loci. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94123 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Nichols, SA (reprint author), Univ Calif Berkeley, Dept Integrat Biol, 3060 Valley Life Sci Bldg, Berkeley, CA 94123 USA. EM nichols1@socrates.berkeley.edu; bamesp@mala.bc.ca RI Nichols, Scott/B-9422-2008 NR 46 TC 37 Z9 39 U1 4 U2 13 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 SEP 28 PY 2005 VL 323 IS 1 BP 1 EP 15 DI 10.1016/j.jembe.2005.02.012 PG 15 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 969TH UT WOS:000232257200001 ER PT J AU Leonard, JA Rohland, N Glaberman, S Fleischer, RC Caccone, A Hofreiter, M AF Leonard, JA Rohland, N Glaberman, S Fleischer, RC Caccone, A Hofreiter, M TI A rapid loss of stripes: the evolutionary history of the extinct quagga SO BIOLOGY LETTERS LA English DT Article DE ancient DNA; phylogeography; Africa; vicariance; Pleistocene; refugia ID MITOCHONDRIAL-DNA; GENUS EQUUS AB Twenty years ago, the field of ancient DNA was launched with the publication of two short mitochondrial (mt) DNA sequences from a single quagga (Equus quagga) museum skin, an extinct South African equid (Higuchi et al. 1984 Nature 312, 282-284). This was the first extinct species from which genetic information was retrieved. The DNA sequences of the quagga showed that it was more closely related to zebras than to horses. However, quagga evolutionary history is far from clear. We have isolated DNA from eight quaggas and a plains zebra (subspecies or phenotype Equus burchelli burchelli). We show that the quagga displayed little genetic diversity and very recently diverged from the plains zebra, probably during the penultimate glacial maximum. This emphasizes the importance of Pleistocene climate changes for phylo-geographic patterns in African as well as Holarctic fauna. C1 Max Planck Inst Evolutionary Anthrop, D-04103 Leipzig, Germany. Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. Yale Univ, YIBS, MSCG Lab, New Haven, CT 06520 USA. Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. RP Leonard, JA (reprint author), Uppsala Univ, Dept Evolutionary Biol, Norbyvagen 18D, S-75236 Uppsala, Sweden. EM jennifer.leonard@ebc.uu.se RI Leonard, Jennifer/A-7894-2010; Hofreiter, Michael/A-3996-2017 OI Leonard, Jennifer/0000-0003-0291-7819; Hofreiter, Michael/0000-0003-0441-4705 NR 21 TC 38 Z9 41 U1 2 U2 26 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETT-UK JI Biol. Lett. PD SEP 22 PY 2005 VL 1 IS 3 BP 291 EP 295 DI 10.1098/rsbl.2005.0323 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 968NX UT WOS:000232170300011 PM 17148190 ER PT J AU Drew, JE Greimel, R Irwin, MJ Aungwerojwit, A Barlow, MJ Corradi, RLM Drake, JJ Gansicke, BT Groot, P Hales, A Hopewell, EC Irwin, J Knigge, C Leisy, P Lennon, DJ Mampaso, A Masheder, MRW Matsuura, M Morales-Rueda, L Morris, RAH Parker, QA Phillipps, S Rodriguez-Gil, P Roelofs, G Skillen, I Sokoloski, JL Steeghs, D Unruh, YC Viironen, K Vink, JS Walton, NA Witham, A Wright, N Zijlstra, AA Zurita, A AF Drew, JE Greimel, R Irwin, MJ Aungwerojwit, A Barlow, MJ Corradi, RLM Drake, JJ Gansicke, BT Groot, P Hales, A Hopewell, EC Irwin, J Knigge, C Leisy, P Lennon, DJ Mampaso, A Masheder, MRW Matsuura, M Morales-Rueda, L Morris, RAH Parker, QA Phillipps, S Rodriguez-Gil, P Roelofs, G Skillen, I Sokoloski, JL Steeghs, D Unruh, YC Viironen, K Vink, JS Walton, NA Witham, A Wright, N Zijlstra, AA Zurita, A TI The INT photometric H alpha Survey of the Northern Galactic Plane (IPHAS) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; stars : emission-line, Be; stars : general; galaxy : disc; galaxy : stellar content ID RAYET CENTRAL STARS; DIGITAL SKY SURVEY; CARBON STARS; DATA RELEASE; MILKY-WAY; EMISSION; AAO/UKST; CATALOG; NEBULAE; OBJECTS AB The Isaac Newton Telescope (INT) Photometric H alpha Survey of the Northern Galactic Plane (IPHAS) is a 1800-deg(2) CCD survey of the northern Milky Way spanning the latitude range -5 degrees < b < +5 degrees and reaching down to r' similar or equal to 20 (10 sigma). Representative observations and an assessment of point-source data from IPHAS, now underway, are presented. The data obtained are Wide Field Camera images in the H alpha narrow-band, and Sloan r' and i' broad-band filters. We simulate IPHAS (r' - H alpha, r' - i') point-source colours using a spectrophotometric library of stellar spectra and available filter transmission profiles: this defines the expected colour properties of (i) solar metallicity stars, without H alpha emission, and (ii) emission-line stars. Comparisons with observations of fields in Aquila show that the simulations of normal star colours reproduce the observations well for all spectral types earlier than M. A further comparison between colours synthesized from long-slit flux-calibrated spectra and IPHAS photometry for six objects in a Taurus field confirms the reliability of the pipeline calibration. Spectroscopic follow-up of a field in Cepheus shows that sources lying above the main stellar locus in the (r' H alpha, r' - i') plane are confirmed to be emission-line objects with very few failures. In this same field, examples of H alpha deficit objects (a white dwarf and a carbon star) are shown to be readily distinguished by their IPHAS colours. The role IPHAS can play in studies of spatially resolved northern Galactic nebulae is discussed briefly and illustrated by a continuum-subtracted mosaic image of Shajn 147 (a supernova remnant, 3 degrees in diameter). The final catalogue of IPHAS point sources will contain photometry on about 80 million objects. Used on its own, or in combination with near-infrared photometric catalogues, IPHAS is a major resource for the study of stellar populations making up the disc of the Milky Way. The eventual yield of new northern emission-line objects from IPHAS is likely to be an order of magnitude increase on the number already known. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. UCL, Dept Phys & Astron, London WC1E 6BT, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Radboud Univ Nijmegen, Afd St4errenkunde, NL-6500 GL Nijmegen, Netherlands. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. Univ Bristol, Dept Phys, Astrophys Grp, Bristol BS8 1TL, Avon, England. Univ Manchester, Sch Phys & Astron, Manchester M60 1QD, Lancs, England. Macquarie Univ, Dept Phys, N Ryde, NSW 2109, Australia. Anglo Australian Observ, Epping, NSW 1710, Australia. Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. Univ Granada, Fac Ciencias, E-18071 Granada, Spain. RP Drew, JE (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Exhibit Rd, London SW7 2AZ, England. EM j.drew@imperial.ac.uk RI Gaensicke, Boris/A-9421-2012; Barlow, Michael/A-5638-2009; Steeghs, Danny/C-5468-2009; Zurita, Almudena/A-2218-2015; Groot, Paul/K-4391-2016; Rodriguez-Gil, Pablo/H-7709-2015; OI Gaensicke, Boris/0000-0002-2761-3005; Drew, Janet/0000-0003-1192-7082; Barlow, Michael/0000-0002-3875-1171; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X; Rodriguez-Gil, Pablo/0000-0002-4717-5102; Unruh, Yvonne/0000-0001-8217-6998; Lennon, Daniel/0000-0003-3063-4867; Phillipps, Steven/0000-0001-5991-3486 NR 42 TC 231 Z9 233 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2005 VL 362 IS 3 BP 753 EP 776 DI 10.1111/j.1365-2966.2005.09330.x PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 968JH UT WOS:000232158300001 ER PT J AU Heyl, JS Hernquist, L AF Heyl, JS Hernquist, L TI A quantum electrodynamics model for non-thermal emission from soft gamma repeaters and anomalous X-ray pulsars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE MHD; radiation mechanisms, non-thermal; pulsars, general ID MAGNETIZED NEUTRON-STARS; SPECTRUM AB Previously, we showed that, owing to effects arising from quantum electrodynamics (QED), magnetohydrodynamic fast modes of sufficient strength will break down to form electron-positron pairs while traversing the magnetospheres of strongly magnetized neutron stars. The bulk of the energy of the fast mode fuels the development of an electron-positron fireball. However, a small, but potentially observable, fraction of the energy (similar to 10(33) erg) can generate a non-thermal distribution of electrons and positrons far from the star. In this paper, we examine the cooling and radiative output of these particles. We also investigate the properties of non-thermal emission in the absence of a fireball to understand the breakdown of fast modes that do not yield an optically thick pair plasma. This quiescent, non-thermal radiation associated with fast-mode breakdown may account for the recently observed non-thermal emission from several anomalous X-ray pulsars and soft gamma repeaters. C1 Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyl, JS (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM heyl@physics.ubc.ca NR 30 TC 34 Z9 34 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2005 VL 362 IS 3 BP 777 EP 783 DI 10.1111/j.1365-2966.2005.09338.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 968JH UT WOS:000232158300002 ER PT J AU Pounds, KA Wilkes, BJ Page, KL AF Pounds, KA Wilkes, BJ Page, KL TI X-ray absorption and re-emission from an ionized outflow in the Type I quasi-stellar object 2MASS 234449+1221 observed by XMM-Newton SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : general; galaxies : individual : 2MASS 234449+1221; quasars : general; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; GALAXIES; CHANDRA; SPECTROSCOPY; VARIABILITY; REFLECTION; SPECTRUM; NGC-1068; MATTER; GAS AB We report on the analysis of a short XMM-Newton observation of the reddened Type 1 quasistellar object (QSO) 2MASS 234449+1221 first identified in the Two-Micron All-Sky Survey (2MASS). The underlying X-ray continuum is found to be typical of a broad-line active galaxy, with photon index Gamma similar to 1.9. Low-energy absorption can be modelled by a column N-H similar to 10(22) cm(-2) of moderately ionized gas or a smaller column of cold gas. Addition of a soft X-ray emission component significantly improves the fit in both cases. With the assumption that the soft X-ray flux represents emission from gas photoionized by the incident X-ray continuum, a comparison of the absorbed and emitted luminosities indicates a covering factor of similar to 8 - 17 per cent. The unusual opportunity simultaneously to observe and quantify ionized absorption and emission in 2MASS 234449+1221 is due to the relatively large opacity - for a Type 1 active galactic nucleus (AGN) - of the absorbing gas, which depresses the normally strong continuum below similar to 1 keV. A comparison of the soft X-ray emission of 2MASS 234449+1221 with that of other Type 1 and Type 2 AGNs suggests the existence of an inner turbulent extension to ionized outflows, not detected in current high-resolution X-ray spectra. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pounds, KA (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM kap@leicester.ac.uk OI Wilkes, Belinda/0000-0003-1809-2364 NR 25 TC 7 Z9 7 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 SEP 21 PY 2005 VL 362 IS 3 BP 784 EP 788 DI 10.1111/j.1365-2966.2005.09365.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 968JH UT WOS:000232158300003 ER PT J AU Stern, D Eisenhardt, P Gorjian, V Kochanek, CS Caldwell, N Eisenstein, D Brodwin, M Brown, MJI Cool, R Dey, A Green, P Jannuzi, BT Murray, SS Pahre, MA Willner, SP AF Stern, D Eisenhardt, P Gorjian, V Kochanek, CS Caldwell, N Eisenstein, D Brodwin, M Brown, MJI Cool, R Dey, A Green, P Jannuzi, BT Murray, SS Pahre, MA Willner, SP TI Mid-infrared selection of active galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : formation ID SPITZER-SPACE-TELESCOPE; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; ARRAY CAMERA IRAC; X-RAY; GALACTIC NUCLEI; REDSHIFT SURVEY; QUASARS; CHANDRA; POPULATION AB Mid-infrared photometry provides a robust technique for identifying active galaxies. While the ultraviolet to mid-infrared (lambda less than or similar to 5 mu m) continuum of stellar populations is dominated by the composite blackbody curve and peaks at approximately 1.6 mu m, the ultraviolet to mid-infrared continuum of active galactic nuclei (AGNs) is dominated by a power law. Consequently, with a sufficient wavelength baseline, one can easily distinguish AGNs from stellar populations. Mirroring the tendency of AGNs to be bluer than galaxies in the ultraviolet, where galaxies (and stars) sample the blue, rising portion of stellar spectra, AGNs tend to be redder than galaxies in the mid-infrared, where galaxies sample the red, falling portion of the stellar spectra. We report on Spitzer Space Telescope mid-infrared colors, derived from the IRAC Shallow Survey, of nearly 10,000 spectroscopically identified sources from the AGN and Galaxy Evolution Survey. On the basis of this spectroscopic sample, we find that simple mid-infrared color criteria provide remarkably robust separation of active galaxies from normal galaxies and Galactic stars, with over 80% completeness and less than 20% contamination. Considering only broad-lined AGNs, these mid-infrared color criteria identify over 90% of spectroscopically identified quasars and Seyfert 1 galaxies. Applying these color criteria to the full imaging data set, we discuss the implied surface density of AGNs and find evidence for a large population of optically obscured active galaxies. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Stern, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM stern@zwolfkinder.jpl.nasa.gov RI Brown, Michael/B-1181-2015; Barmby, Pauline/I-7194-2016 OI Brown, Michael/0000-0002-1207-9137; Barmby, Pauline/0000-0003-2767-0090 NR 36 TC 539 Z9 539 U1 2 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 SEP 20 PY 2005 VL 631 IS 1 BP 163 EP 168 DI 10.1086/432523 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100010 ER PT J AU Bottcher, M Harvey, J Joshi, M Villata, M Raiteri, CM Bramel, D Mukherjee, R Savolainen, T Cui, W Fossati, G Smith, IA Able, D Aller, HD Aller, MF Arkharov, AA Augusteijn, T Baliyan, K Barnaby, D Berdyugin, A Benitez, E Boltwood, P Carini, M Carosati, D Ciprini, S Coloma, JM Crapanzano, S de Diego, JA Di Paola, A Dolci, M Fan, J Frasca, A Hagen-Thorn, V Horan, D Ibrahimov, M Kimeridze, GN Kovalev, YA Kovalev, YY Kurtanidze, O Lahteenmaki, A Lanteri, L Larionov, VM Larionova, EG Lindfors, E Marilli, E Mirabal, N Nikolashvili, M Nilsson, K Ohlert, JM Ohnishi, T Oksanen, A Ostorero, L Oyer, G Papadakis, I Pasanen, M Poteet, C Pursimo, T Sadakane, K Sigua, LA Takalo, L Tartar, JB Terasranta, H Tosti, G Walters, R Wiik, K Wilking, BA Wills, W Xilouris, E Fletcher, AB Gu, M Lee, CU Pak, S Yim, HS AF Bottcher, M Harvey, J Joshi, M Villata, M Raiteri, CM Bramel, D Mukherjee, R Savolainen, T Cui, W Fossati, G Smith, IA Able, D Aller, HD Aller, MF Arkharov, AA Augusteijn, T Baliyan, K Barnaby, D Berdyugin, A Benitez, E Boltwood, P Carini, M Carosati, D Ciprini, S Coloma, JM Crapanzano, S de Diego, JA Di Paola, A Dolci, M Fan, J Frasca, A Hagen-Thorn, V Horan, D Ibrahimov, M Kimeridze, GN Kovalev, YA Kovalev, YY Kurtanidze, O Lahteenmaki, A Lanteri, L Larionov, VM Larionova, EG Lindfors, E Marilli, E Mirabal, N Nikolashvili, M Nilsson, K Ohlert, JM Ohnishi, T Oksanen, A Ostorero, L Oyer, G Papadakis, I Pasanen, M Poteet, C Pursimo, T Sadakane, K Sigua, LA Takalo, L Tartar, JB Terasranta, H Tosti, G Walters, R Wiik, K Wilking, BA Wills, W Xilouris, E Fletcher, AB Gu, M Lee, CU Pak, S Yim, HS TI Coordinated multiwavelength observation of 3C 66A during the WEBT campaign of 2003-2004 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (3C 66A); galaxies : active; gamma rays : theory; radiation mechanisms : nonthermal ID BL-LACERTAE OBJECTS; EXTRAGALACTIC RADIO-SOURCES; TEV GAMMA-RAYS; XMM-NEWTON OBSERVATIONS; LIGHT CURVES; LAC OBJECTS; X-RAY; BACKGROUND-RADIATION; BRIGHT BLAZARS; VARIABILITY AB The BL Lac object 3C 66A was the target of an extensive multiwavelength monitoring campaign from 2003 July through 2004 April (with a core campaign from 2003 September to 2003 December) involving observations throughout the electromagnetic spectrum. Radio, infrared, and optical observations were carried out by the WEBT-ENIGMA collaboration. At higher energies, 3C 66Awas observed in X-rays (RXTE), and at very high energy (VHE) in gamma-rays (STACEE, VERITAS). In addition, the source has been observed with the VLBA at nine epochs throughout the period 2003 September to 2004 December, including three epochs contemporaneous with the core campaign. A gradual brightening of the source over the course of the campaign was observed at all optical frequencies, culminating in a very bright maximum around 2004 February 18. The WEBT campaign revealed microvariability with flux changes of similar to 5% on timescales as short as similar to 2 hr. The source was in a relatively bright state, with several bright flares on timescales of several days. The spectral energy distribution (SED) indicates a v F v peak in the optical regime. A weak trend of optical spectral hysteresis with a trend of spectral softening throughout both the rising and decaying phases has been found. On longer timescales, there appears to be a weak indication of a positive hardness-intensity correlation for low optical fluxes, which does not persist at higher flux levels. The 3-10 keV X-ray flux of 3C 66A during the core campaign was historically high and its spectrum very soft, indicating that the low-frequency component of the broadband SED extends beyond similar to 10 keV. No significant X-ray flux and/or spectral variability was detected. STACEE and Whipple observations provided upper flux limits at > 150 and > 390 GeV, respectively. The 22 and 43 GHz data from the three VLBA epochs made between 2003 September and 2004 January indicate a rather smooth jet with only very moderate internal structure. Evidence for superluminal motion (8.5 +/- 5.6 h(-1) c) was found in only one of six components, while the apparent velocities of all other components are consistent with 0. The radial radio brightness profile suggests a magnetic field decay proportional to r(-1) and, thus, a predominantly perpendicular magnetic field orientation. C1 Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA. Osserv Astron Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy. Columbia Univ Barnard Coll, New York, NY 10027 USA. Turku Univ, Tuorla Observ, Piikkio, Finland. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Pulkovo Observ, St Petersburg 196140, Russia. Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Santa Cruz De T, Spain. Phys Res Lab, Ahmedabad 3800009, Gujarat, India. Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42104 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Boltwood Observ, Stittsville, ON K2S 1N6, Canada. Osservatorio Armenzano, Assisi, Italy. Univ Perugia, Osservatorio Astron, I-06126 Perugia, Italy. Agrupacion Astron Sabadell, Sabadell 08200, Spain. Osserv Astron Roma, Ist Nazl Astrofis, I-00136 Rome, Italy. Osservatorio Astron Teramo, INAF, Teramo, Italy. Guangzhou Univ, Ctr Astrophys, Guangzhou 510400, Peoples R China. Osserv Astrofis Catania, I-95125 Catania, Italy. St Petersburg State Univ, Inst Astron, St Petersburg 198504, Russia. Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg 198504, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Uzbek Acad Sci, Ulugh Beg Astron Inst, Tashkent 700052, Uzbekistan. Abastumani Observ, GE-383762 Abastumani, Rep of Georgia. Ctr Astro Space, Moscow 117997, Russia. Natl Radio Astron Observ, Green Bank, WV 24944 USA. Helsinki Univ Technol, Metsahovi Radio Observ, Kylmala 02540, Finland. Columbia Univ, Dept Phys & Astron, New York, NY 10027 USA. Michael Adrian Observ, Astron Stiftung Trebur, D-65468 Trebur, Germany. Osaka Kyoiku Univ, Inst Astron, Kashiwara, Osaka 5828582, Japan. Nyrola Observ, Jyvaskylan Sirius Ry, Jyvaskyla 40950, Finland. Landessternwarte Heidelberg Konigstuhl, D-69117 Heidelberg, Germany. Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Crete, Greece. Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. NOA, Inst Astron & Astrophys, Athens, Greece. Korea Astron & Space Sci Inst, Taejon 305348, South Korea. Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Bottcher, M (reprint author), Ohio Univ, Inst Astrophys, Dept Phys & Astron, Clippinger 339, Athens, OH 45701 USA. EM villata@to.astro.it RI Fossati, Giovanni/A-5841-2009; de Diego, Jose/B-4093-2009; Papadakis, Iossif/C-3235-2011; Pak, Soojong/E-2360-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Larionova, Elena/H-7287-2013; Xilouris, Emmanuel/K-9459-2013; Kovalev, Yuri/J-5671-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Kovalev, Yuri/N-1053-2015 OI Jose A., de Diego/0000-0001-7040-069X; Ostorero, Luisa/0000-0003-3983-5980; Dolci, Mauro/0000-0001-8000-5642; Savolainen, Tuomas/0000-0001-6214-1085; Di Paola, Andrea/0000-0002-2189-8644; Cui, Wei/0000-0002-6324-5772; Villata, Massimo/0000-0003-1743-6946; Frasca, Antonio/0000-0002-0474-0896; Raiteri, Claudia Maria/0000-0003-1784-2784; Pak, Soojong/0000-0002-2548-238X; /0000-0003-0180-8231; Larionov, Valeri/0000-0002-4640-4356; Larionova, Elena/0000-0002-2471-6500; Kovalev, Yuri/0000-0001-9303-3263; NR 71 TC 32 Z9 33 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 SEP 20 PY 2005 VL 631 IS 1 BP 169 EP 186 DI 10.1086/432609 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100011 ER PT J AU Sollins, PK Zhang, QH Keto, E Ho, PTP AF Sollins, PK Zhang, QH Keto, E Ho, PTP TI An infalling torus of molecular gas around the ultracompact HII region G28.20-0.05 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; HII regions; ISM : individual (G28.20-0.05); ISM : molecules; stars : formation ID MASS YOUNG STAR; H-II REGIONS; ACCRETION FLOW; ROTATING-DISK; G10.6-0.4; COLLAPSE; CLOUDS; EVOLUTION; CORES AB We present new observations of the ultracompact H II region G28.20-0.05 in the 23 GHz continuum and the NH3(1,1), NH3(2,2), and NH3(3,3) lines. To explain the complicated kinematics of the molecular gas, we propose a model consisting of two components. One component is an infalling, equatorial torus of molecular gas, whose dense central region has been ionized to form the ultracompact H II region. The second component is a larger expanding molecular shell driven by some type of wide-angle outflow or wind. We estimate that the infall component includes more than 18 M-circle dot of molecular gas. We calculate the central mass to be 79 M-circle dot, probably comprising more than one star. The arrangement of the molecular material suggests a connection to the other disklike structures seen around massive young stars. The central star in this case is more massive, and the whole region may be more evolved than other similar objects such as IRAS 20126+4104, IRAS 18089-1732, G192.16-3.84, and AFGL 5142. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sollins, PK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM psollins@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 30 TC 15 Z9 15 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 SEP 20 PY 2005 VL 631 IS 1 BP 399 EP 410 DI 10.1086/432503 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100028 ER PT J AU Pepper, J Gaudi, BS AF Pepper, J Gaudi, BS TI Searching for transiting planets in stellar systems SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; surveys; techniques : photometric ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EXTRASOLAR GIANT PLANETS; OPEN CLUSTER NGC-6791; GALACTIC DISK; 2001 CAMPAIGN; HOT JUPITERS; STAR; FIELD; CANDIDATES AB We analyze the properties of searches devoted to finding planetary transits by observing simple stellar systems, such as globular clusters, open clusters, and the Galactic bulge. We develop the analytic tools necessary to predict the number of planets that a survey will detect as a function of the parameters of the system ( age, extinction, distance, richness, mass function), the observational setup ( nights observed, bandpass, exposure time, telescope diameter, detector characteristics), site properties ( seeing, sky background), and the planet properties ( frequency, period, and radius). We find that for typical parameters, the detection probability is maximized for I-band observations. At fixed planet period and radius, the signal-to-noise ratio of a planetary transit in the I band is weakly dependent on the mass of the primary for sources with flux above the sky background and falls very sharply for sources below sky. Therefore, for typical targets, the number of detectable planets is roughly proportional to the number of stars with transiting planets with fluxes above sky ( and not necessarily the number of sources with photometric error less than a given threshold). Furthermore, for rising mass functions, the majority of the planets will be detected around sources with fluxes near sky. In order to maximize the number of detections, experiments should therefore be tailored such that sources near sky are above the required detection threshold. Once this requirement is met, the number of detected planets is relatively weakly dependent on the detection threshold, diameter of the telescope, exposure time, seeing, age of the system, and planet radius, for typical ranges of these parameters encountered in current transit searches in stellar systems. The number of detected planets is a strongly decreasing function of the distance to the system, implying that the nearest, richest clusters may prove to be optimal targets. C1 Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pepper, J (reprint author), Ohio State Univ, Dept Astron, McPherson Lab 4055, 140 W 18th Ave, Columbus, OH 43210 USA. EM pepper@astronomy.ohio-state.edu; sgaudi@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012; OI Pepper, Joshua/0000-0002-3827-8417 NR 58 TC 27 Z9 27 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP 581 EP 596 DI 10.1086/432532 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OD UT WOS:000231959100045 ER PT J AU Jorgensen, JK Lahuis, F Schoier, FL van Dishoeck, EF Blake, GA Boogert, ACA Dullemond, CP Evans, NJ Kessler-Silacci, JE Pontoppidan, KM AF Jorgensen, JK Lahuis, F Schoier, FL van Dishoeck, EF Blake, GA Boogert, ACA Dullemond, CP Evans, NJ Kessler-Silacci, JE Pontoppidan, KM TI Protostellar holes: Spitzer Space Telescope observations of the protostellar binary IRAS 16293+2422 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : formation; stars : individual (IRAS 16293+2422) ID SUBMILLIMETER CONTINUUM OBSERVATIONS; 2-DIMENSIONAL RADIATIVE-TRANSFER; LOW-MASS PROTOSTARS; IRAS 16293-2422; STAR-FORMATION; CLOUD CORES; ENVELOPES; ABUNDANCE; DISKS; ENVIRONMENT AB Mid-infrared (23-35 mu m) emission from the deeply embedded Class 0 protostar IRAS 16293-2422 is detected with the Spitzer Space Telescope infrared spectrograph. A detailed radiative transfer model reproducing the full spectral energy distribution (SED) from 23 mu m to 1.3 mm requires a large inner cavity of radius 600 AU in the envelope to avoid quenching the emission from the central sources. This is consistent with a previous suggestion based on high angular resolution millimeter interferometric data. An alternative interpretation using a two-dimensional model of the envelope with an outflow cavity can reproduce the SED but not the interferometer visibilities. The cavity size is comparable to the centrifugal radius of the envelope and therefore appears to be a natural consequence of the rotation of the protostellar core, which has also caused the fragmentation leading to the central protostellar binary. With a large cavity such as required by the data, the average temperature at a given radius does not increase above 60-80 K, and although hot spots with higher temperatures may be present close to each protostar, these constitute a small fraction of the material in the inner envelope. The proposed cavity will also have consequences for the interpretation of molecular line data, especially of complex species probing high temperatures in the inner regions of the envelope. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. SRON, Natl Inst Space Res, NL-9700 AV Groningen, Netherlands. Stockholm Observ, AlbaNova, S-10691 Stockholm, Sweden. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Jorgensen, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM jjorgensen@cfa.harvard.edu; freddy@sron.rug.nl; fredrik@astro.su.se; ewine@strw.leidenuniv.nl; gab@gps.caltech.edu; acab@astro.caltech.edu; dullemon@mpia.de; nje@as.utexas.edu; jes@as.utexas.edu; pontoppi@strw.leidenuniv.nl OI Dullemond, Cornelis/0000-0002-7078-5910 NR 22 TC 32 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP L77 EP L80 DI 10.1086/497003 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OG UT WOS:000231959400020 ER PT J AU Khan, SA Shafer, RA Benford, DJ Staguhn, JG Chanial, P Le Floc'h, E Babbedge, TSR Farrah, D Moseley, SH Dwek, E Clements, DL Sumner, TJ Ashby, MLN Brand, K Brodwin, M Eisenhardt, PR Elston, R Gonzalez, AH McKenzie, E Murray, SS AF Khan, SA Shafer, RA Benford, DJ Staguhn, JG Chanial, P Le Floc'h, E Babbedge, TSR Farrah, D Moseley, SH Dwek, E Clements, DL Sumner, TJ Ashby, MLN Brand, K Brodwin, M Eisenhardt, PR Elston, R Gonzalez, AH McKenzie, E Murray, SS TI On the discovery of the first galaxy selected at 350 microns SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : high-redshift; galaxies : starburst; infrared : galaxies; submillimeter ID DEEP SUBMILLIMETER SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; HIGH-REDSHIFT GALAXIES; EXTREMELY RED OBJECTS; STELLAR MASS DENSITY; LUMINOSITY DENSITY; INFRARED GALAXIES; SHARC-II; FIELD AB We report the detection of a 3.6 sigma source selected at 350 mm in the Bootes Deep Field. The source, the first short-wavelength submillimeter-selected galaxy (SSG1), was discovered as part of a blank-field extragalactic survey using the 350 mu m-optimized Submillimeter High Angular Resolution Camera (SHARC II) at the Caltech Submillimeter Observatory. With multiwavelength photometry from the NOAO Deep Wide-Field Survey (R and I band), FLAMEX (J and K-s), Spitzer (IRAC and MIPS), and the Westerbork 1.4 GHz deep survey (radio upper limit), we are able to constrain the photometric redshift using different methods, all of which suggest a redshift of similar to 1. In the absence of long-wavelength submillimeter data, we use SED templates to infer that this source is an ultraluminous infrared galaxy with a dust temperature of 30 +/- 5 K, occupying a region of luminosity-temperature space shared by moderate-redshift ISO-selected ULIRGs (rather than high-redshift SCUBA-selected submillimeter galaxies). SHARC II can thus select galaxies with moderately "warm" dust that might be missed in submillimeter surveys at longer wavelengths. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Khan, SA (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 49 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP L9 EP L12 DI 10.1086/497111 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OG UT WOS:000231959400003 ER PT J AU Luhman, KL Lada, CJ Hartmann, L Muench, AA Megeath, ST Allen, LE Myers, PC Muzerolle, J Young, E Fazio, GG AF Luhman, KL Lada, CJ Hartmann, L Muench, AA Megeath, ST Allen, LE Myers, PC Muzerolle, J Young, E Fazio, GG TI The disk fractions of brown dwarfs in IC 348 and Chamaeleon I 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 INITIAL MASS FUNCTION; STAR-FORMING REGION; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; YOUNG CLUSTER IC-348; CIRCUMSTELLAR DISKS; EVOLUTIONARY MODELS; TRAPEZIUM CLUSTER; CENSUS; TAURUS AB Using the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope, we have obtained mid-infrared photometry for 25 and 18 low-mass members of the IC 348 and Chamaeleon I star-forming clusters, respectively (> M6, M less than or similar to 0.08 M-circle dot). We find that 42% +/- 13% and 50% +/- 17% of the two samples exhibit excess emission indicative of circumstellar disks. In comparison, the disk fractions for stellar members of these clusters are 33% +/- 4% and 45% +/- 7% (M0-M6, 0.7 M-circle dot greater than or similar to M greater than or similar to 0.1 M-circle dot). The similarity in the disk fractions of stars and brown dwarfs is consistent with a common formation mechanism and indicates that the raw materials for planet formation are available around brown dwarfs as often as around stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Luhman, KL (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM kluhman@cfa.harvard.edu; clada@cfa.harvard.edu; lhartmann@cfa.harvard.edu; gmuench@cfa.harvard.edu; tmegeath@cfa.harvard.edu; leallen@cfa.harvard.edu; pmyers@cfa.harvard.edu; jamesm@as.arizona.edu; eyoung@as.arizona.edu; gfazio@cfa.harvard.edu OI Muench, August/0000-0003-0666-6367 NR 36 TC 51 Z9 51 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP L69 EP L72 DI 10.1086/497031 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OG UT WOS:000231959400018 ER PT J AU Sridharan, TK Williams, SJ Fuller, GA AF Sridharan, TK Williams, SJ Fuller, GA TI The direct detection of a (proto) binary/disk system in IRAS 20126+4104 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; circumstellar matter; infrared : ISM; ISM : individual (IRAS 20126+4104); stars : early-type; stars : formation ID MASS PROTOSTELLAR CANDIDATES; IRAS 20126+4104; CIRCUMSTELLAR ENVIRONMENTS; MOLECULAR OUTFLOWS; DUST CONTINUUM; ACCRETION DISK; ROTATING-DISK; YOUNG STAR; SAMPLE; JET AB We report the direct detection of a binary/disk system toward the high-mass (proto) stellar object IRAS 20126 + 4104 at infrared wavelengths. The presence of a multiple system had been indicated by the precession of the outflow and the double-jet system detected earlier at centimeter wavelengths. Our new K-, L'-, and M'-band infrared images, obtained with the UKIRT under exceptional seeing conditions on Mauna Kea, are able to resolve the central source for the first time, and we identify two objects separated by similar to 0".5 (850 AU). The K and L' images also uncover features characteristic of a nearly edge-on disk, similar to many low-mass protostars with disks: two emission regions oriented along an outflow axis and separated by a dark lane. The peaks of the L'- and M'-band and millimeter-wavelength emission are on the dark lane, presumably locating the primary young star. The thickness of the disk is measured to be similar to 850 AU for radii less than or similar to 1000 AU. Approximate limits on the NIR magnitudes of the two young stars indicate a high-mass system, although with much uncertainty. These results are a demonstration of the high-mass nature of the system, and of the similarities of the star formation process in the low-mass and high-mass regimes, viz., the presence of a disk-accretion stage. The companion is located along the dark lane, consistent with it being in the equatorial/disk plane, indicating a disk-accretion setting for massive, multiple, star formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. UMIST, Dept Phys, Manchester M60 1QD, Lancs, England. RP Sridharan, TK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM tksridha@cfa.harvard.edu; stewart.williams@manchester.ac.uk; gary.fuller@manchester.ac.uk NR 29 TC 33 Z9 33 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP L73 EP L76 DI 10.1086/497093 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OG UT WOS:000231959400019 ER PT J AU Zhou, JL Aarseth, SJ Lin, DNC Nagasawa, M AF Zhou, JL Aarseth, SJ Lin, DNC Nagasawa, M TI Origin and ubiquity of short-period earth-like planets: Evidence for the sequential accretion theory of planet formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; planetary systems : protoplanetary disks; planets and satellites : formation; solar system : formation; stars : individual (GJ 876) ID PROTOSTELLAR DISKS; TERRESTRIAL PLANETS; GIANT PLANETS; SOLAR NEBULA; GRAVITATIONAL-INSTABILITY; DETERMINISTIC MODEL; EXTRASOLAR PLANETS; ORBITAL MIGRATION; RAPID FORMATION; SYSTEMS AB The formation of gas giant planets is assumed to be preceded by the emergence of solid cores in the conventional sequential accretion paradigm. This hypothesis implies that the presence of Earth-like planets can be inferred from the detection of gas giants. A similar prediction cannot be made with the gravitational instability model, which assumes that gas giants formed from the collapse of gas fragments analogous to their host stars. We propose an observational test for the determination of the dominant planetary formation channel. Based on the sequential accretion model, we identify several potential avenues that may lead to the prolific formation of a population of close-in Earth-mass (M-circle plus) planets around stars with (1) short-period or (2) solitary eccentric giants and (3) systems that contain intermediate-period resonant giants. In contrast, these close-in Earths are not expected to form in systems where giants originated rapidly through gravitational instability. As a specific example, we suggest that sequential accretion processes led to the formation of the 7.5 M-circle plus planet around GJ 876 and predict that it may have an atmosphere and envelope rich in O-2 and liquid water. Assessments of the ubiquity of these planets will lead to (1) the detection of the first habitable terrestrial planets, (2) verification of the dominant mode of planet formation, (3) an estimate of the fraction of stars harboring Earth-like planets, and (4) modification of biomarker signatures. C1 Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA. Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. Univ Cambridge, Astron Inst, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. RP Zhou, JL (reprint author), Univ Calif Santa Cruz, UCO, Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA. EM zhoujl@nju.edu.cn; sverre@ast.cam.ac.uk; lin@ucolick.org; nagaswmk@cc.nao.ac.jp NR 44 TC 58 Z9 62 U1 2 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2005 VL 631 IS 1 BP L85 EP L88 DI 10.1086/497094 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 965OG UT WOS:000231959400022 ER PT J AU Pawson, DL Vance, DJ AF Pawson, DL Vance, DJ TI Rynkatorpa felderi, new species, from a bathyal hydrocarbon seep in the northern Gulf of Mexico (Echinodermata : Holothuroidea : Apodida) SO ZOOTAXA LA English DT Article DE Rynkatorpa felderi; cold seeps; Gulf of Mexico; Holothuroidea; Apodida ID COMMENSAL SEA CUCUMBER; COMMUNITIES AB Rynkatorpa felderi new species was collected at a cold hydrocarbon seep at bathyal depths in the northern Gulf of Mexico. This is the first record of a synaptid holothurian from a chemosynthetic site, and the first record of the genus Rynkatorpa in the Atlantic; all other congeners are known from the Indo-Pacific. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20013 USA. RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Mail Stop MRC163, Washington, DC 20013 USA. EM pawsond@si.edu NR 16 TC 1 Z9 1 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 SEP 16 PY 2005 IS 1050 BP 15 EP 20 PG 6 WC Zoology SC Zoology GA 964ME UT WOS:000231884400002 ER PT J AU Mukhopadhyay, B AF Mukhopadhyay, B TI Neutrino asymmetry around black holes: Neutrinos interact with gravity SO MODERN PHYSICS LETTERS A LA English DT Article DE neutrino asymmetry; rotating black hole; spacetime curvature; CPT violation ID CPT VIOLATION; GRAVITATIONAL-FIELD; GENERAL-RELATIVITY; SPIN-1/2 PARTICLE; EXTENDED BODIES; QUANTUM-GRAVITY; COSMIC-RAYS; BARYOGENESIS; ANNIHILATION; CURVATURE AB Propagation of fermions in curved spacetime generates gravitational interaction due to coupling of its spin with spacetime curvature connection. This gravitational interaction, which is an axial-four-vector multiplied by a four-gravitational vector potential, appears as a CPT violating term in the Lagrangian which generates an opposite sign and thus an asymmetry between the left-handed and the right-handed partners under the CPT transformation. In the case of neutrinos, this property can generate neutrino asymmetry in the Universe. If the background metric is of the rotating black hole, i.e. the Kerr geometry, this interaction for the neutrino is nonzero. Therefore the dispersion energy relation for the neutrino and its anti-neutrino are different which gives rise to the difference in their number densities and neutrino asymmetry in the Universe in addition to the known relic asymmetry. C1 Harvard Smithsonian Ctr Astrophys, Div Theory, Cambridge, MA 02138 USA. RP Mukhopadhyay, B (reprint author), Harvard Smithsonian Ctr Astrophys, Div Theory, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM bmukhopa@cfa.harvard.edu NR 50 TC 22 Z9 22 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 EI 1793-6632 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD SEP 14 PY 2005 VL 20 IS 28 BP 2145 EP 2155 DI 10.1142/S0217732305017640 PG 11 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 965AW UT WOS:000231923100004 ER PT J AU Protopapas, P Jimenez, R Alcock, C AF Protopapas, P Jimenez, R Alcock, C TI Fast identification of transits from light-curves SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques : photometric; binaries : eclipsing; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; PLANETARY TRANSITS; SEARCH; CANDIDATES; PHOTOMETRY; ALGORITHM; PROJECT; STAR; MASS AB We present an algorithm that allows fast and efficient detection of transits, including planetary transits, from light-curves. The method is based on building an ensemble of fiducial models and compressing the data using the MOPED compression algorithm. We describe the method and demonstrate its efficiency by finding planet-like transits in simulated Panoramic Survey Telescope & Rapid Response System (Pan-STARRS) light-curves. We show that our method is independent of the size of the search space of transit parameters. In large sets of light-curves, we achieve speed-up factors of the order of 10(3) times over an optimized adaptive search in the chi(2) space. We discuss how the algorithm can be used in forthcoming large surveys like Pan-STARRS and the Large Synoptic Survey Telescope (LSST), and how it may be optimized for future space missions like Kepler and COROT where most of the processing must be done on board. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Protopapas, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pprotopapas@cfa.harvard.edu OI Jimenez, Raul/0000-0002-3370-3103 NR 22 TC 20 Z9 20 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 SEP 11 PY 2005 VL 362 IS 2 BP 460 EP 468 DI 10.1111/j.1365-2966.2005.09305.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959HX UT WOS:000231509900007 ER PT J AU El-Gharbawy, HA Metwally, SM Sharshar, T Elnimr, T Badran, HM AF El-Gharbawy, HA Metwally, SM Sharshar, T Elnimr, T Badran, HM TI Establishment of HPGe detector efficiency for point source including true coincidence correction SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE HPGe detector efficiency; point source; true coincidence correction; effective solid angle ID MONTE-CARLO CALCULATIONS; DIFFERENT COUNTING GEOMETRIES; ABSOLUTE PEAK EFFICIENCY; EXTENDED SOURCES; CALIBRATION; CURVE; SPECTROMETRY; SIMULATIONS AB Due to the variation of the activity levels of various samples in gamma-ray spectroscopy, the source-to-detector distance is not fixed at a constant value. This means that the measurements of the absolute detector efficiency must be carried out for each geometrical arrangement used in gamma-ray measurements, which is difficult and non-feasible. This work established a method to calibrate an HPGe detector using only one precise efficiency curve obtained experimentally at a reference source-to-detector distance and a simple computer program to extract the resulting efficiency curves at other distances. The validity of the computed efficiencies for various detector geometries was checked against published calculation and simulation results. The disagreements were < 1% for the calculations and < 2.7% in the case of simulation results except for one case with a 9% discrepancy. The results obtained with this method were also checked against efficiency curves measured experimentally at different source-to-detector distances using 10% and 50% p-type HPGe detectors with single and multi gamma-ray emitters. The results of this method are in good agreement with that carried out by single gamma-ray emitters. The disagreement was < 2.2% and 4.7% for the 50% and 10% HPGe, respectively. The experimental results with multi gamma-ray radionuclides were found to disagree with those obtained using the established method at small source-to-detector distances. A computer program was used to estimate the gamma-gamma true coincidence correction factor to eliminate this disagreement. For multi gamma-ray emitters the disagreement after true coincidence correction was found to be < 10% and < 6% at small source-to-detector distances for the 50% and 10% HPGe, respectively. The maximum values were < 3% and < 5% at large distances (>= 11.5 cm) in the case of the 50% and 10% HPGe, respectively. (c) 2005 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. Tanta Univ, Dept Phys, Fac Sci, Tanta 31527, Egypt. Ain Shams Univ, Fac Sci, Dept Phys, Cairo, Egypt. Tanta Univ, Fac Educ, Dept Chem & Phys, Kafr El Shaikh, Egypt. RP Badran, HM (reprint author), Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 97, Amado, AZ 85645 USA. EM badran@egret.sao.arizona.edu NR 24 TC 3 Z9 3 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD SEP 11 PY 2005 VL 550 IS 1-2 BP 201 EP 211 DI 10.1016/j.nima.2005.05.051 PG 11 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 965QE UT WOS:000231964500020 ER PT J AU McQuinn, M Furlanetto, SR Hernquist, L Zahn, O Zaldarriaga, M AF McQuinn, M Furlanetto, SR Hernquist, L Zahn, O Zaldarriaga, M TI The kinetic Sunyaev-Zel'dovich effect from reionization SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : theory; intergalactic medium ID DARK-MATTER HALOES; MICROWAVE BACKGROUND ANISOTROPIES; PROBE WMAP OBSERVATIONS; POPULATION-III STARS; GUNN-PETERSON TROUGH; EXCURSION SET MODEL; LY-ALPHA FOREST; INTERGALACTIC MEDIUM; HIGH REDSHIFTS; MASS FUNCTION AB During the epoch of reionization, local variations in the ionized fraction ( patchiness) imprint arcminute- scale temperature anisotropies in the CMB through the kinetic Sunyaev- Zel'dovich ( kSZ) effect. We employ an improved version of an analytic model of reionization devised by Furlanetto and coworkers to calculate the kSZ anisotropy from patchy reionization. This model uses extended Press- Schechter theory to determine the distribution and evolution of H (II) bubbles and produces qualitatively similar reionization histories to those seen in recent numerical simulations. We find that the angular power spectrum of the kSZ anisotropies depends strongly on the size distribution of the H (II) bubbles and on the duration of reionization. In addition, we show that upcoming measurements of the kSZ effect should be able to distinguish between several popular reionization scenarios. In particular, the amplitude of the patchy power spectrum for reionization scenarios in which the IGM is significantly ionized by Population III stars ( or by miniquasars/ decaying particles) can be larger ( or smaller) by over a factor of 3 than the amplitude in more traditional reionization histories ( with temperature anisotropies that range between 0.5 and 3 mu K at l= 5000). We highlight the differences in the kSZ signal between many possible reionization morphologies and discuss the constraints that future observations of the kSZ will place on this epoch. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. 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. NR 79 TC 86 Z9 86 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 SEP 10 PY 2005 VL 630 IS 2 BP 643 EP 656 DI 10.1086/432049 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400001 ER PT J AU Zahn, O Zaldarriaga, M Hernquist, L McQuinn, M AF Zahn, O Zaldarriaga, M Hernquist, L McQuinn, M TI The influence of nonuniform reionization on the CMB SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : theory; large-scale structure of universe ID MICROWAVE BACKGROUND ANISOTROPIES; PROBE WMAP OBSERVATIONS; PARTICLE HYDRODYNAMICS SIMULATIONS; POPULATION-III STARS; DIGITAL SKY SURVEY; HIGH-REDSHIFT; COSMIC REIONIZATION; STELLAR SOURCES; LY-ALPHA; UNIVERSE AB We investigate the impact of spatial variations in the ionized fraction during reionization on temperature anisotropies in the CMB. We combine simulations of large- scale structure to describe the underlying density field with an analytic model based on extended Press- Schechter theory to track the reionization process. We find that the power spectrum of the induced CMB anisotropies depends sensitively on the character of the reionization epoch. Models that differ in the extent of the `` patchy phase'' could be distinguished by future experiments such as the Atacama Cosmology Telescope ( ACT) and the South Pole Telescope ( SPT). In our models, the patchy signal peaks at l similar or equal to 2000, where it can be 4 times larger than the kinetic Sunyaev- Zel'dovich ( kSZ)/ Ostriker- Vishniac ( OV) signal (Delta T-tot similar or equal to 2: 6 mu K). On scales beyond l similar or equal to 4000 the total Doppler signal is dominated by kSZ/ OV, but the patchy signal can contribute up to 30% to the power spectrum. The effect of patchy reionization is largest on scales on which the primordial CMB anisotropies dominate. Ignoring this contribution could lead to significant biases in the determination of cosmological parameters derived from CMB temperature measurements. Improvements in the theoretical modeling of the reionization epoch will become increasingly important to interpret the results of upcoming experiments. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Jefferson Phys Lab, Cambridge, MA 02138 USA. RP Zahn, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ozahn@cfa.harvard.edu NR 70 TC 80 Z9 80 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2005 VL 630 IS 2 BP 657 EP 666 DI 10.1086/431947 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400002 ER PT J AU Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Martini, P Robertson, B Springel, V AF Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Martini, P Robertson, B Springel, V TI Black holes in galaxy mergers: Evolution of quasars SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; galaxies : active; galaxies : evolution; galaxies : nuclei quasars : general ID DIGITAL SKY SURVEY; PARTICLE HYDRODYNAMICS SIMULATIONS; ULTRALUMINOUS INFRARED GALAXY; LUMINOSITY IRAS GALAXIES; ACTIVE GALACTIC NUCLEUS; DARK-MATTER UNIVERSE; REGION NEARBY SURVEY; LY-ALPHA FOREST; INFALL REGION; MOLECULAR GAS AB Based on numerical simulations of gas- rich galaxy mergers, we discuss amodel in which quasar activity is tied to the self- regulated growth of supermassive black holes in galaxies. The nuclear inflow of gas attending a galaxy collision triggers a starburst and feeds black hole growth, but for most of the duration of the starburst, the black hole is `` buried,'' being heavily obscured by surrounding gas and dust, limiting the visibility of the quasar, especially at optical and ultraviolet wavelengths. As the black hole grows, feedback energy from accretion heats the gas and eventually expels it in a powerful wind, leaving behind a `` dead quasar.'' Between the buried and dead phases, there is a window in time during which the galaxy would be seen as a luminous quasar. Because the black hole mass, radiative output, and distribution of obscuring gas and dust all evolve strongly with time, the duration of this phase of observable quasar activity depends on both the waveband and imposed luminosity threshold. We determine the observed and intrinsic lifetimes as a function of luminosity and frequency, and calculate observable lifetimes similar to 10 Myr for bright quasars in the optical B band, in good agreement with empirical estimates and much smaller than our estimated black hole growth timescales similar to 100 Myr, naturally producing a substantial population of buried quasars. However, the observed and intrinsic energy outputs converge in the IR and hard X- ray bands as attenuation becomes weaker and chances of observation greatly increase. We also obtain the distribution of column densities along sight lines in which the quasar is seen above a given luminosity, and find that our result agrees remarkably well with observed estimates of the column density distribution from the SDSS for the appropriate luminosity thresholds. Our model reproduces a wide range of quasar phenomena, including observed quasar lifetimes, intrinsic lifetimes, column density distributions, and differences between optical and X- ray samples, having properties consistent with observations across more than 5 orders of magnitude in bolometric luminosity from 10(9) to 10(14) L circle dot (- 17 less than or similar to M-B less than or similar to -30). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Gerlingen, Germany. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 123 TC 359 Z9 360 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2005 VL 630 IS 2 BP 705 EP 715 DI 10.1086/432438 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400006 ER PT J AU Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Robertson, B Springel, V AF Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Robertson, B Springel, V TI Luminosity-dependent quasar lifetimes: A new interpretation of the quasar luminosity function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : active; galaxies : evolution; galaxies : nuclei quasars : general ID SUPERMASSIVE BLACK-HOLES; ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEI; QSO REDSHIFT SURVEY; X-RAY BINARIES; COSMOLOGICAL EVOLUTION; SPACE DISTRIBUTION; GALAXIES; GROWTH; ORIGIN AB We propose a new interpretation of the quasar luminosity function ( LF) derived from physically motivated models of quasar lifetimes and light curves. In our picture, quasars evolve rapidly, and their lifetime depends on both their instantaneous and peak luminosities. We study this model using simulations of galaxy mergers that successfully reproduce a wide range of observed quasar phenomena. With lifetimes inferred from the simulations, we deconvolve the observed quasar LF from the distribution of peak luminosities and show that they differ qualitatively, unlike the simple models of quasar lifetimes used previously. We find that the bright end of the LF traces the intrinsic peak quasar activity but that the faint end consists of quasars that are either undergoing exponential growth to much larger masses and higher luminosities, or are in sub- Eddington quiescent states going into or coming out of a period of peak activity. The `` break'' in the LF directly corresponds to the maximum in the intrinsic distribution of peak luminosities, which falls off at both brighter and fainter luminosities. Our interpretation of the quasar LF provides a physical basis for the nature and slope of the faint- end distribution, as well as the location of the break luminosity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 32 TC 107 Z9 107 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 SEP 10 PY 2005 VL 630 IS 2 BP 716 EP 720 DI 10.1086/432463 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400007 ER PT J AU Sollins, PK Ho, PTP AF Sollins, PK Ho, PTP TI The molecular accretion flow in G10.6-0.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; HII regions; ISM : individual (G10.6-0.4); stars : formation ID ULTRACOMPACT HII-REGIONS; MASSIVE STAR-FORMATION; H-II REGIONS; ROTATING-DISK; YOUNG STAR; GALAXY; CORE; CONTINUUM; EVOLUTION; CLOUDS AB We have observed the ultracompact H II region G10.6 - 0.4 with the VLA in the 23 GHz continuum and the NH3 ( 3, 3) inversion line. By analyzing the optical depth of the line as well as the kinematics, we have detected a flattened, rotating molecular accretion flow. We detect the fact that the highest column density gas is more flattened, that is, distributed more narrowly, than the lower column density gas, and that there is some inclination of the rotation axis. The rotation is sub-Keplerian, and the molecular gas is not in a rotationally supported disk. We do not find a single massive ( proto-) star forming in a scaled-up version of low-mass star formation. Instead, our observations suggest a different mode of clustered massive star formation, in which the accretion flow flattens but does not form an accretion disk. Moreover, in this mode of star formation the central object can be a group of massive stars rather than a single massive star. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sollins, PK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM psollins@cfa.harvard.edu NR 29 TC 35 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2005 VL 630 IS 2 BP 987 EP 995 DI 10.1086/432254 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400029 ER PT J AU Bogdanov, S Grindlay, JE van den Berg, M AF Bogdanov, S Grindlay, JE van den Berg, M TI An X-ray variable millisecond pulsar in the globular cluster 47 tucanae: Closing the link to low-mass X-ray binaries SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; pulsars : individual (PSR J0024 7204W); stars : neutron; X-rays : stars ID ACTIVE RADIO PULSAR; SAX J1808.4-3658; NEUTRON-STARS; OPTICAL COUNTERPART; PSR J1740-5340; XMM-NEWTON; COMPANION; NGC-6397; EMISSION; QUIESCENCE AB We report the discovery of peculiar X-ray spectral variability in the binary radio millisecond pulsar PSR J0024 - 7204W in the globular cluster 47 Tuc. The observed emission consists of a dominant nonthermal component, which is eclipsed for a portion of the orbit, and a thermal component, which appears to be persistent. We propose that the nonthermal X-rays originate in a relativistic intrabinary shock, formed due to interaction between the relativistic particle wind from the pulsar and matter from the main-sequence companion star, while the thermal photons are from the heated magnetic polar caps of the millisecond pulsar. At optical wavelengths, the emission exhibits large-amplitude variations at the orbital period, which can be attributed to heating of one side of the tidally locked secondary star by the pulsar wind. The observed X-ray and optical properties of PSR J0024 - 7204W are remarkably similar to those of the low-mass X-ray binary and X-ray millisecond pulsar SAX J1808.4 - 3658 in quiescence. This supports the conjecture that the nonthermal X-ray emission and optical modulations seen in the SAX J1808.4 - 3658 system in a quiescent state are due to interaction between the wind from a reactivated rotation-powered pulsar and matter from the companion star. The striking similarities between the two systems provide support for the long-sought connection between millisecond radio pulsars and accreting neutron star systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bogdanov, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sbogdanov@cfa.harvard.edu; josh@cfa.harvard.edu; mvandenberg@cfa.harvard.edu OI Bogdanov, Slavko/0000-0002-9870-2742 NR 47 TC 57 Z9 58 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 SEP 10 PY 2005 VL 630 IS 2 BP 1029 EP 1036 DI 10.1086/432249 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LR UT WOS:000231664400034 ER PT J AU Calvet, N D'Alessio, P Watson, DM Franco-Hernandez, R Furlan, E Green, J Sutter, PM Forrest, WJ Hartmann, L Uchida, KI Keller, LD Sargent, B Najita, J Herter, TL Barry, DJ Hall, P AF Calvet, N D'Alessio, P Watson, DM Franco-Hernandez, R Furlan, E Green, J Sutter, PM Forrest, WJ Hartmann, L Uchida, KI Keller, LD Sargent, B Najita, J Herter, TL Barry, DJ Hall, P TI Disks in transition in the Taurus population: Spitzer IRS spectra of GM Aurigae and DM Tauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars : formation; stars : pre-main-sequence ID MAIN-SEQUENCE EVOLUTION; TW-HYDRAE ASSOCIATION; ACCRETION DISKS; INFRARED SPECTROGRAPH; CIRCUMSTELLAR DISKS; SPACE-TELESCOPE; YOUNG OBJECTS; STARS; PLANET; DUST AB We present Spitzer Infrared Spectrograph (IRS) observations of two objects of the Taurus population that show unambiguous signs of clearing in their inner disks. In one of the objects, DM Tau, the outer disk is truncated at 3 AU; this object is akin to another recently reported in Taurus, CoKu Tau/4, in that the inner disk region is free of small dust. Unlike CoKu Tau/4, however, this star is still accreting, so optically thin gas should still remain in the inner disk region. The other object, GM Aur, also accreting, has similar to 0.02 lunar masses of small dust in the inner disk region within similar to 5 AU, consistent with previous reports. However, the IRS spectrum clearly shows that the optically thick outer disk has an inner truncation at a much larger radius than previously suggested, similar to 24 AU. These observations provide strong evidence for the presence of gaps in protoplanetary disks. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Calvet, N (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM ncalvet@cfa.harvard.edu OI Furlan, Elise/0000-0001-9800-6248 NR 38 TC 251 Z9 251 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2005 VL 630 IS 2 BP L185 EP L188 DI 10.1086/491652 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LT UT WOS:000231664600021 ER PT J AU Dow-Hygelund, CC Holden, BP Bouwens, RJ van der Wel, A Illingworth, GD Zirm, A Franx, M Rosati, P Ford, H van Dokkum, PG Stanford, SA Eisenhardt, P Fazio, GG AF Dow-Hygelund, CC Holden, BP Bouwens, RJ van der Wel, A Illingworth, GD Zirm, A Franx, M Rosati, P Ford, H van Dokkum, PG Stanford, SA Eisenhardt, P Fazio, GG TI UV continuum spectroscopy of a 6L(*) z=5.5 starburst galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : high-redshift; galaxies : individual (J1252-5224-4599); galaxies : starburst ID LYMAN-BREAK GALAXIES; FRAME ULTRAVIOLET-SPECTRA; ULTRA-DEEP-FIELD; STAR-FORMATION; SPACE-TELESCOPE; ADVANCED CAMERA; Z-APPROXIMATE-TO-6; RDCS-1252.9-2927; Z-SIMILAR-TO-6; DENSITY AB We have obtained a high S/ N ( 22.3 hr integration) UV continuum VLT FORS2 spectrum of an extremely bright (z(850) = 24.3) z = 5.515 +/- 0.003 star- forming galaxy ( BD38) in the field of the z = 1.24 cluster RDCS 1252.9 - 2927. From HST Advanced Camera for Surveys imaging, this object was selected as a potential z similar to 6 Lyman break galaxy ( LBG) based on its red i(775) -z(850) = 1.5 color. This object shows substantial continuum ( 0.41 +/- 0.02 mu Jy at 1300 angstrom) and low- ionization interstellar absorption features typical of LBGs at lower redshift A ( z similar to 3); this is the highest redshift LBG confirmed via metal- absorption spectral features. The equivalent widths of the absorption features are similar to z similar to 3 strong Ly alpha absorbers. No noticeable Ly alpha emission was detected (F <= 1.4 x 10(-18) ergs cm (-2) s (-1), 3 sigma). This object is at most amplified 0.3 mag from gravitational lensing by the foreground cluster. The delensed half- light radius of this object is 1.6 kpc ( 0 ".25), and the star formation rate derived from the rest- frame UV luminosity is SFRUV = 38h(0.7)(-2) M-circle dot yr (-1) corrected for dust extinction). In terms of recent determinations of the z similar to 6 UV luminosity function, this object appears to be 6L(*). The Spitzer IRAC fluxes for this object are 23.3 and 23.2 AB mag ( delensed) in the 3.6 and 4.5 mu m channels, respectively, implying a mass of ( 1 - 6) x 10(10) M-circle dot from population synthesis models. This galaxy is brighter than any confirmed z similar to 6 i- dropout to date in the band, and in the 3.6 and 4.5 mu m channels, and is the most z (850) massive starbursting galaxy known at z > 5. C1 Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 96064 USA. Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 96062 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. European So Observ, D-85748 Garching, Germany. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dow-Hygelund, CC (reprint author), Univ Calif Santa Cruz, Dept Phys, 211 Interdisciplinary Sci Bldg,1156 High St, Santa Cruz, CA 96064 USA. EM cdow@scipp.ucsc.edu; holden@ucolick.org; bouwens@ucolick.org; vdwel@strw.leidenuniv.nl; gdi@ucolick.org; azirm@strw.leidenuniv.nl; franx@strw.leidenuniv.nl; prosati@eso.org; ford@pha.jhu.edu; dokkum@astro.yale.edu RI van der Wel, Arjen/G-8365-2011 NR 30 TC 28 Z9 28 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 SEP 10 PY 2005 VL 630 IS 2 BP L137 EP L140 DI 10.1086/491700 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LT UT WOS:000231664600009 ER PT J AU McClure-Griffiths, NM Gaensler, BM AF McClure-Griffiths, NM Gaensler, BM TI Constraints on the distance to SGR 1806-20 from HI absorption SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (SGR 1806-20); radio lines : ISM; stars : distances; stars : neutron; techniques : radial velocities ID SGR 1806-20; MAGNETAR SGR-1806-20; GIANT FLARE; CO SURVEY; REGIONS; CLOUDS; GALAXY AB The giant flare detected from the magnetar SGR 1806 - 20 on 2004 December 27 had a fluence more than 100 times higher than the only two other soft gamma repeater ( SGR) flares ever recorded. Whereas the fluence is independent of distance, an estimate for the luminosity of the burst depends on the source's distance, which has previously been argued to be similar to 15 kpc. The burst produced a bright radio afterglow, against which Cameron et al. have measured an H I absorption spectrum. This has been used to propose a revised distance to SGR 1806 - 20 of between 6.4 and 9.8 kpc. Here we analyze this absorption spectrum and compare it both to H i emission data from the Southern Galactic Plane Survey and to archival (CO)-C-12 survey data. We confirm similar to 6 kpc as a likely lower limit on the distance to SGR 1806 - 20, but argue that it is difficult to place an upper limit on the distance to SGR 1806 - 20 from the H I data currently available. The previous value of similar to 15 kpc thus remains the best estimate of the distance to the source. C1 CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McClure-Griffiths, NM (reprint author), CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. EM naomi.mcclure-griffiths@csiro.au; bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Gaensler, Bryan/0000-0002-3382-9558 NR 28 TC 34 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2005 VL 630 IS 2 BP L161 EP L163 DI 10.1086/496879 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LT UT WOS:000231664600015 ER PT J AU Risaliti, G Bianchi, S Matt, G Baldi, A Elvis, M Fabbiano, G Zezas, A AF Risaliti, G Bianchi, S Matt, G Baldi, A Elvis, M Fabbiano, G Zezas, A TI Highly ionized iron absorption lines from outflowing gas in the X-ray spectrum of NGC 1365 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual ( NGC 1365); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; NGC-3783; VELOCITY; WINDS AB We present the discovery of four absorption lines in the X- ray spectrum of the Seyfert galaxy NGC 1365, at energies between 6.7 and 8.3 keV. The lines are detected with high statistical confidence ( from > 20 sigma for the strongest to similar to 4 sigma for the weakest) in two XMM- Newton observations 60 ks long. We also detect the same lines, with a lower signal- to- noise ratio ( but still > 2 sigma for each line), in two previous shorter (similar to 10 ks) XMM- Newton observations. The spectral analysis identifies these features as Fe xxv and Fe xxvi K alpha and K beta lines, outflowing with velocities varying between similar to 1000 and similar to 5000 km s (-1) among the observations. These are the highest quality detections of such lines so far. The high equivalent widths [EW(K alpha) similar to 100eV] and the K alpha/ K beta ratios imply that the lines are due to absorption of the AGN continuum by a highly ionized gas with column density N-H similar to 5 x 10(23)cm (-2) at a distance of similar to( 50 - 100) R-S from the continuum source. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAF, Osservatorio Arcetri, I-50125 Florence, Italy. European Space Astron Ctr, XMM Newton Sci Operat Ctr, ESA, E-28080 Madrid, Spain. Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM grisaliti@cfa.harvard.edu RI Bianchi, Stefano/B-4804-2010; Zezas, Andreas/C-7543-2011; OI Bianchi, Stefano/0000-0002-4622-4240; Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X NR 23 TC 76 Z9 76 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 SEP 10 PY 2005 VL 630 IS 2 BP L129 EP L132 DI 10.1086/491646 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961LT UT WOS:000231664600007 ER PT J AU Ruostekoski, J Isella, L AF Ruostekoski, J Isella, L TI Dissipative quantum dynamics of bosonic atoms in a shallow 1D optical lattice SO PHYSICAL REVIEW LETTERS LA English DT Article ID BOSE-EINSTEIN CONDENSATE; ULTRACOLD ATOMS; SUPERFLUID; GAS AB We theoretically study the dipolar motion of bosonic atoms in a very shallow, strongly confined 1D optical lattice using the parameters of the recent experiment [C. D. Fertig , Phys. Rev. Lett. 94, 120403 (2005)]. We find that, due to momentum uncertainty, a small, but non-negligible, atom population occupies the unstable velocity region of the corresponding classical dynamics, resulting in the observed dissipative atom transport. This population is generated even in a static vapor, due to quantum fluctuations which are enhanced by the lattice and the confinement, and is not notably affected by the motion of atoms or finite temperature. C1 Univ Hertfordshire, Dept Phys, Hatfield AL10 9AB, Herts, England. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02135 USA. RP Ruostekoski, J (reprint author), Univ Hertfordshire, Dept Phys, Hatfield AL10 9AB, Herts, England. NR 31 TC 45 Z9 46 U1 0 U2 6 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 SEP 9 PY 2005 VL 95 IS 11 AR 110403 DI 10.1103/PhysRevLett.95.110403 PG 4 WC Physics, Multidisciplinary SC Physics GA 963KA UT WOS:000231802000005 PM 16196983 ER PT J AU Olson, SL Matsuoka, H AF Olson, SL Matsuoka, H TI New specimens of the early Eocene frigatebird Limnofregata (Pelecaniformes : Fregatidae), with the description of a new species SO ZOOTAXA LA English DT Article DE Eocene; fossil birds; Fregata; Fregatidae; frigatebirds; Limnofregata; paleoecology; pelecaniformes; sexual dimorphism; Wyoming AB Four additional specimens from the Green River Formation of Wyoming are referred to the Eocene frigatebird Limnofregata azygosternon Olson, originally described from a nearly complete skeleton and two partial paratypes. Two skulls with mandibles and a partial postcranial skeleton are described as a new species, Limnofregata hasegawai, characterized by much larger size and a proportionately longer bill. One of the referred specimens of L. azygosternon is from Eocene Lake Gosiute, whereas all of the other specimens of Limnofregata are from Fossil Lake. The species of Limnofregata would have taken advantage of frequent periodic dieoffs of fish in the Green River lakes. Geological and climatic factors that may have influenced the paleoecology, distribution, and size variation in frigatebirds in the Cenozoic are reviewed. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. Kyoto Univ, Grad Sch Sci, Dept Geol & Mineral, Kyoto 6068502, Japan. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. EM olsons@si.edu; maca@bs.kueps.kyoto-u.ac.jp NR 20 TC 20 Z9 21 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 SEP 8 PY 2005 IS 1046 BP 1 EP 15 PG 15 WC Zoology SC Zoology GA 962ES UT WOS:000231714400001 ER PT J AU Durden, LA Adams, NE AF Durden, LA Adams, NE TI Primary type specimens of sucking lice (Insecta : Phthiraptera : Anoplura) in the U.S. National Museum of Natural History, Smithsonian Institution SO ZOOTAXA LA English DT Article DE Phthiraptera; Anoplura; sucking lice; primary types; synonymies; nomenclature; U. S. National Museum of Natural History; Smithsonian Institution ID POLYPLACIDAE AB An annotated list is presented of the 110 primary types (holotypes, lectotypes, syntypes, or neotypes) of sucking lice ( Insecta: Phthiraptera: Anoplura) deposited in the U. S. National Museum of Natural History (USNM), Smithsonian Institution, as of May 2005. Annotations for each taxon are listed alphabetically by specific epithet, and are followed by the original generic assignment and ( in parentheses) the current family designation. Next, the author, year of description, and original citation are provided. The primary type held in the USNM ( with USNM type number, slide number and other relevant data, if these were assigned), original collection data, current taxonomic assignment ( if different from the original designation), and additional taxonomic remarks, if relevant, are then given. Brief information on allotypes and paratypes are included if these are mounted on the same microscope slide as the primary type or if they are otherwise relevant. The types include those of the type species of seven genera (Abrocomaphthirus Durden & Webb, Atopophthirus Kim & Emerson, Haematopinoides Osborn, Latagophthirus Kim & Emerson, Pecaroecus Babcock & Ewing, Phthirpediculus Ewing, and Sathrax Johnson) one of which is the type genus of a family (Pecaroecidae). Primary types for five species of Anoplura that have not yet been described, and for another four species that were described in an unpublished dissertation are also deposited in the USNM. Hosts and collection data for these nine specimens are briefly mentioned after the main list; however, species names are excluded because these names currently have no nomenclatural standing. A neotype specimen is designated for Haematopinus montanus Osborn, 1896, a taxon which is currently treated as a junior synonym of Linognathoides laeviusculus ( Grube, 1851). C1 Georgia So Univ, Dept Biol, Statesboro, GA 30460 USA. Georgia So Univ, Inst Arthropodol & Parasitol, Statesboro, GA 30460 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Durden, LA (reprint author), Georgia So Univ, Dept Biol, Statesboro, GA 30460 USA. EM ldurden@georgiasouthern.edu NR 24 TC 5 Z9 8 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 8 PY 2005 IS 1047 BP 21 EP 60 PG 40 WC Zoology SC Zoology GA 962EU UT WOS:000231714600002 ER PT J AU Campbell, BA Hawke, BR AF Campbell, BA Hawke, BR TI Radar mapping of lunar cryptomaria east of Orientale basin SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MOON; WAVELENGTH; HUMORUM AB Lunar cryptomare deposits represent early basaltic volcanic material that has been mantled by or incorporated into highland-rich ejecta from basin- or crater-forming impacts. Mapping these buried basalts is important for understanding regional stratigraphy and the history and extent of lunar volcanism. We use new 70 cm wavelength radar images, collected using Arecibo Observatory and the Green Bank Telescope, and Clementine data to study cryptomaria east of Orientale basin. Earlier multispectral analyses showed that mare material is mixed with the highland terrain along the western margin of Oceanus Procellarum, leading to a detectable increase in the FeO and TiO2 abundance of the regolith surface. The highland margin of western Procellarum is also characterized by low 70 cm radar returns, consistent with an increased regolith loss tangent due to ilmenite in the mare-derived material. The low 70 cm radar echo, however, persists well to the west of the mixed zone evident in multispectral data and includes the region surrounding Cruger crater. It is likely that mare basalt, or a mixed zone of mare and highland material, exists at depth across the region and only reaches the visible surface near the western Procellarum margin. The plausible depth to this mixed zone is dependent upon the loss tangent of the overlying "pure" highland ejecta. If Orientale ejecta is primarily low-loss anorthosite, then the mixed zone could lie at depths of up to several tens of meters. We propose that pre-Orientale mare deposits flooded the region between Cruger, Grimaldi, and Oceanus Procellarum and also patches west and northwest of Humorum basin. The total area of these deposits represents 178 x 10(3) km(2), or an additional similar to 0.5% of the lunar surface, covered by mare basalts. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. EM campbellb@si.edu NR 31 TC 26 Z9 26 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 7 PY 2005 VL 110 IS E9 AR E09002 DI 10.1029/2005JE002425 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 963TL UT WOS:000231828700001 ER PT J AU Behrensmeyer, A Barry, J AF Behrensmeyer, Anna Barry, John TI BIOSTRATIGRAPHIC SURVEYS IN THE SIWALIK SEQUENCE OF PAKISTAN: A METHOD FOR STANDARDIZED SURFACE SAMPLING OF THE VERTEBRATE FOSSIL RECORD SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Behrensmeyer, Anna] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Barry, John] Harvard Univ, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 35A EP 35A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900026 ER PT J AU Bloch, J Cadena, E Herrera, F Wing, S Jaramillo, C AF Bloch, Jonathan Cadena, Edwin Herrera, Fabiany Wing, Scott Jaramillo, Carlos TI PALEOCENE VERTEBRATES FROM THE CERREJON FORMATION, GUAJIRA PENINSULA, NORTHEASTERN COLOMBIA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Bloch, Jonathan] Univ Florida, Gainesville, FL 32611 USA. [Cadena, Edwin] Inst Colombiano Petro, Bucaramanga, Santander, Colombia. [Herrera, Fabiany] Univ Ind Santander, Bucaramanga, Santander, Colombia. [Wing, Scott] Natl Museum Nat Hist, Washington, DC 20560 USA. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. NR 0 TC 3 Z9 3 U1 1 U2 1 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 SEP 7 PY 2005 VL 25 IS 3 BP 37A EP 38A PG 2 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900038 ER PT J AU Brett-Surman, M Jabo, S Kroehler, P Carrano, M Kvale, E AF Brett-Surman, Michael Jabo, Steven Kroehler, Peter Carrano, Matthew Kvale, Erik TI A NEW MICROVERTEBRATE ASSEMBLAGE FROM THE UPPER JURASSIC MORRISON FORMATION, INCLUDING MAMMALS, THEROPODS, AND SPHENODONTIANS SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Brett-Surman, Michael; Jabo, Steven; Kroehler, Peter; Carrano, Matthew] Smithsonian Inst, Washington, DC 20560 USA. [Kvale, Erik] Indiana Geol Survey, Bloomington, IN USA. RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 0 TC 1 Z9 1 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 SU S BP 39A EP 39A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900047 ER PT J AU Carrano, M AF Carrano, Matthew TI THE DINOSAUR FOSSIL RECORD SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Carrano, Matthew] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 0 TC 1 Z9 1 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 42A EP 42A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900065 ER PT J AU Chaney, D AF Chaney, Dan TI A FOSSIL PLANT! NOW WHAT DO I DO? SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Chaney, Dan] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 43A EP 43A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900069 ER PT J AU Clyde, W Hamzi, W Finarelli, J Secord, R Wing, S AF Clyde, William Hamzi, Walid Finarelli, John Secord, Ross Wing, Scott TI A NEW BASIN-WIDE MAGNETOSTRATIGRAPHIC FRAMEWORK FOR THE BIGHORN BASIN, WYOMING SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Clyde, William; Hamzi, Walid] Univ New Hampshire, Durham, NH 03824 USA. [Finarelli, John] Univ Chicago, Chicago, IL 60637 USA. [Secord, Ross; Wing, Scott] Smithsonian, Washington, DC USA. RI Clyde, William/C-9595-2017 OI Clyde, William/0000-0001-8814-3409 NR 0 TC 0 Z9 0 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 46A EP 47A PG 2 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900087 ER PT J AU Head, J AF Head, Jason TI ARCHAEOPHIS PROAVUS AND THE EVOLUTIONARY HISTORY OF PALAEOPHIID SNAKES SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Head, Jason] Queen Mary Univ London, Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 68A EP 68A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900201 ER PT J AU Hilton, E Forey, P AF Hilton, Eric Forey, Peter TI OSTEOLOGY, SYSTEMATICS, AND BIOGEOGRAPHY OF FOSSIL AND LIVING OSTEOGLOSSID FISHES (TELEOSTEI: OSTEOGLOSSOMORPHA), WITH A DESCRIPTION OF NEW FORMS AND A REVIEW OF THE BIOGEOGRAPHIC RELATIONSHIPS OF THE CLADE MEMBERS SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Hilton, Eric] Smithsonian Inst, Div Fish, Washington, DC 20560 USA. [Forey, Peter] Nat Hist Museum, London SW7 5BD, England. NR 0 TC 0 Z9 0 U1 1 U2 1 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 SEP 7 PY 2005 VL 25 IS 3 BP 70A EP 70A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900211 ER PT J AU Jabo, S AF Jabo, Steven TI THE VERTEBRATE PREPARATION LABORATORY AS A MULTI-DISCIPLINARY, MULTI-FUNCTIONAL SPACE (OR, OTHER INTERESTING PROJECTS I'VE WORKED ON) SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Jabo, Steven] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 74A EP 74A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900234 ER PT J AU Kroehler, PA AF Kroehler, Peter A. TI CAMPTOSAURUS BROWNI, GILMORE; THE HOLOTYPE IS NO LONGER MOUNTED SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Kroehler, Peter A.] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 80A EP 80A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900269 ER PT J AU Lansing, S Behrensmeyer, A AF Lansing, Sarah Behrensmeyer, Anna TI ANALYSIS OF FAUNAL REMAINS FROM SPOTTED HYENA (CROCUTA CROCUTA) DENS IN AMBOSELI NATIONAL PARK, KENYA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Lansing, Sarah] Michigan State Univ, Haslett, MI USA. [Behrensmeyer, Anna] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 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 SEP 7 PY 2005 VL 25 IS 3 BP 82A EP 82A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900281 ER PT J AU Miller, J Behrensmeyer, A AF Miller, Joshua Behrensmeyer, Anna TI SKELETAL DISTRIBUTIONS ACROSS TIME; A MULTIVARIATE APPROACH TO THE CHANGING TAPHONOMY OF AMBOSELI PARK, KENYA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Miller, Joshua] Univ Chicago, Chicago, IL 60637 USA. [Behrensmeyer, Anna] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 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 SEP 7 PY 2005 VL 25 IS 3 BP 92A EP 92A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900335 ER PT J AU Purdy, R AF Purdy, Robert TI IS STRIATOLAMIA A JUNIOR SYNONYM OF MITSUKURINA? SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Purdy, Robert] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 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 SEP 7 PY 2005 VL 25 IS 3 BP 102A EP 102A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900386 ER PT J AU Secord, R Wing, S AF Secord, Ross Wing, Scott TI PALEOENVIRONMENTAL INTERPRETATION OF AN EARLY EOCENE FAUNA USING STABLE ISOTOPES FROM MAMMAL TEETH SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Secord, Ross; Wing, Scott] NMNH, Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 SEP 7 PY 2005 VL 25 IS 3 BP 113A EP 113A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900448 ER PT J AU Sues, HD Clark, J AF Sues, Hans-Dieter Clark, James TI THALATTOSAURS (REPTILIA: DIAPSIDA) FROM THE LATE TRIASSIC (CARNIAN) OF NEVADA AND THEIR PALEOBIOGEOGRAPHIC SIGNIFICANCE SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Sues, Hans-Dieter] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Clark, James] George Washington Univ, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 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 SEP 7 PY 2005 VL 25 IS 3 BP 119A EP 119A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900480 ER PT J AU Whatley, R AF Whatley, Robin TI PHYLOGENY OF THE RHYNCHOSAURIA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Whatley, Robin] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 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 SEP 7 PY 2005 VL 25 IS 3 BP 129A EP 129A PG 1 WC Paleontology SC Paleontology GA V05MU UT WOS:000207130900533 ER PT J AU Bettarel, Y Kan, J Wang, K Williamson, KE Cooney, S Ribblett, S Chen, F Wommack, KE Coats, DW AF Bettarel, Y Kan, J Wang, K Williamson, KE Cooney, S Ribblett, S Chen, F Wommack, KE Coats, DW TI Isolation and preliminary characterisation of a small nuclear inclusion virus infecting the diatom Chaetoceros cf. gracilis SO AQUATIC MICROBIAL ECOLOGY LA English DT Article DE virus; diatom; phytoplankton; infectivity; Chesapeake Bay ID HETEROSIGMA-AKASHIWO RAPHIDOPHYCEAE; PHAEOCYSTIS-POUCHETII PRYMNESIOPHYCEAE; MARINE VIRUSES; HETEROCAPSA-CIRCULARISQUAMA; ELECTRON-MICROSCOPE; MICROMONAS-PUSILLA; EMILIANIA-HUXLEYI; ALGAL VIRUS; BLOOM; PHYTOPLANKTON AB A novel virus (Chaetoceros nuclear inclusion virus: CspNIV) causing lysis of a culture of the diatom Chaetoceros cf. gracilis was isolated from the Chesapeake Bay, USA, in April 2003. Transmission electron microscopy Of ultrathin sections of infected C. cf. gracilis revealed that CspNIV proliferates within the nucleus and forms paracrystalline arrays corresponding to the alignment of icosahedral viral particles of about 25 nm diameter. CspNIV shows some strong similarities with Heterosigma akashiwo nuclear inclusion virus (HaNIV) (cf. Lawrence et al. 2001; J Phycol 37: 216-222). The latent period of CspNIV is <24 h. The most widespread occurrence of Chaetoceros viruses in Chesapeake Bay was recorded in April 2003, ca. 1 mo after the winter-spring Chaetoceros bloom. However, results indicate that CspNIV remains infectious in surface water of the bay no longer than 1 mo after the disappearance of its host. Thus, our results reinforce the idea that microalgae are also sensitive to viruses other than those belonging to the family Phycodnaviridae. Furthermore, discovery and initial description of the infection process and ecology of CspNIV expands the breadth of phytoplankton shown to be susceptible to viral attack to include a ubiquitous diatom genera. C1 Ctr Bel Air, Inst Rech Dev, Dakar, Senegal. Univ Maryland, Ctr Marine Biotechnol, Baltimore, MD 21202 USA. Delaware Biotechnol Inst, Newark, DE 19711 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Bettarel, Y (reprint author), Ctr Bel Air, Inst Rech Dev, BP 1386, Dakar, Senegal. EM bettarel@ird.sn RI Kan, Jinjun/C-5252-2011; Chen, Feng/P-3088-2014 NR 45 TC 36 Z9 39 U1 4 U2 16 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0948-3055 J9 AQUAT MICROB ECOL JI Aquat. Microb. Ecol. PD SEP 6 PY 2005 VL 40 IS 2 BP 103 EP 114 DI 10.3354/ame040103 PG 12 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 968QG UT WOS:000232176600001 ER PT J AU Betancur-R, R Acero, A AF Betancur-R, R Acero, A TI Description of Cathorops mapale, a new species of sea catfish (Siluriformes : Ariidae) from the Colombian Caribbean, based on morphological and mitochondrial evidence SO ZOOTAXA LA English DT Article DE Cathorops mapale; Ariidae; sea catfishes; Colombian Caribbean; mitochondrial genes AB A new species of sea catfish ( Ariidae), Cathorops mapale, is described from the central and southwestern Colombian Caribbean coast. The species is distinguished from other Cathorops species from the western Atlantic by the following combination of features: 20 - 24 anterior gill rakers on first gill arch, 18 - 21 anterior gill rakers on second gill arch; maxillary barbels 27.8 - 39.3% standard length; medial head groove long and deep, extending posteriorly almost to supraoccipital keel. This species has been widely misidentified as C. spixii ( Agassiz), a species known from Brazil to the Guianas. Based on mitochondrial evidence ( cytochrome b and ATP synthase 8/ 6), C. mapale is more closely related to the eastern Pacific C. fuerthii ( Steindachner) species group ( 2.2 - 2.8% sequence divergence) than to the C. spixii clade ( 5.9 - 6.2% sequence divergence). C. mapale is distinguished from the C. fuerthii group by having higher anterior gill raker counts on the first ( 14 - 15 in the C. fuerthii group) and second ( 15 - 17 in the C. fuerthii group) gill arches, and by having a smaller mouth ( 8.3 - 10.6% standard length in C. mapale and 11.0 - 11.6% standard length in the C. fuerthii group). C1 Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. Smithsonian Trop Res Inst, Naos Mol Lab, Balboa, Panama. Univ Nacl Colombia, Inst Ciencias Nat, INVEMAR, Santa Marta, Colombia. RP Betancur-R, R (reprint author), Auburn Univ, Dept Biol Sci, 101 Cary Hall, Auburn, AL 36849 USA. EM betanri@auburn.edu; aacero@invemar.org.co RI Betancur-R., Ricardo/A-7276-2009 NR 31 TC 9 Z9 12 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 SEP 5 PY 2005 IS 1045 BP 45 EP 60 PG 16 WC Zoology SC Zoology GA 960VU UT WOS:000231622100004 ER PT J AU Baron-Szabo, RC AF Baron-Szabo, RC TI Remarks on the genus Arctangia Wells, 1937, with the re-description of the type species Thecocyathus nathorsti Lindstrom, 1900 (Anthozoa : Scleractinia) from the Lower Cretaceous of Norway SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The genus Arctangia Wells is a poorly known group that consists of only the type species Thecocyathus nathorsti Lindstrom, 1900. The original description is the only documentation of the species. Including the first description of the genus Arctangia by Wells (1937), all of the later interpretations of the species represent only adaptations of Lindstrom's original report. The present paper gives the re-description of the type species and also provides the first photographic images of this species based on newly discovered material. C1 Natl Museum Nat Hist, Dept Zool, Smithsonian Inst, Washington, DC 20013 USA. Res Inst Senckenberg Palaezool 2, D-60325 Frankfurt, Germany. RP Baron-Szabo, RC (reprint author), Natl Museum Nat Hist, Dept Zool, Smithsonian Inst, MRC-163,POB 37012, Washington, DC 20013 USA. EM rosebaron@comcast.net NR 12 TC 0 Z9 0 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 2 PY 2005 VL 118 IS 3 BP 479 EP 482 DI 10.2988/0006-324X(2005)118[479:ROTGAW]2.0.CO;2 PG 4 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 962RO UT WOS:000231750100001 ER PT J AU Munroe, TA Robertson, DR AF Munroe, TA Robertson, DR TI Symphurus ocellaris, a new shallow-water symphurine tonguefish collected off Pacific Panama (Pleuronectiformes : Cynoglossidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Symphurus ocellaris is described on the basis of a holotype (73.2 mm SL) and paratype (42.3 mm SL) collected in the environs of Coiba Island, Gulf of Chiriqui, Pacific Panama, at 24 m and 7.4 m, respectively. This species is distinguished from congeners by the combination of: a 1-3-4 pattern of interdigitation of dorsal-fin pterygiophores and neural spines (ID pattern), 12 caudal-fin rays, presence of an ocellated spot on the caudal fin in both sexes, 51 total vertebrae, 96-97 dorsal-fin rays, 80-81 anal-fin rays, 85-86 longitudinal scale rows, a pupillary operculum, unpigmented peritoneum, uniformly pigmented blind side, and ocular-side background coloration lacking prominent dark spots or conspicuous crossbands. Symphurus ocellaris is only the second known species in the genus characterized by a 1-3-4 ID pattern. Among eastern Pacific Symphurus, S. callopterus also has a 1-3-4 ID pattern and 12 caudal-fin rays, but lacks the ocellated caudal spot, has a different ocular-side pigmentation, and has higher, non-overlapping meristic features. The only other eastern Pacific tonguefish with an ocellated caudal-fin spot, S. fasciolaris, differs in having 10 caudal-fin rays, a 1-4-3 ID pattern, and ocular-side pigmentation featuring prominent spots and crossbands. C1 NOAA, NMFS, Natl Systemat Lab, Smithsonian Inst, Washington, DC 20013 USA. Smithsonian Trop Res Inst, DRR, Ancona, Italy. RP Munroe, TA (reprint author), NOAA, NMFS, Natl Systemat Lab, Smithsonian Inst, POB 37012,Room WC57,MRC-0153, Washington, DC 20013 USA. EM munroet@si.edu; drr@stri.org NR 5 TC 3 Z9 3 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 2 PY 2005 VL 118 IS 3 BP 576 EP 581 DI 10.2988/0006-324X(2005)118[576:SOANSS]2.0.CO;2 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 962RO UT WOS:000231750100013 ER PT J AU Heyer, WR Crombie, RI AF Heyer, WR Crombie, RI TI Leptodactylus lauramiriamae, a distinctive new species of frog (Amphibia : Anura : Leptodactylidae) from Rondonia, Brazil SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new species of frog is described from Rondonia, Brazil. The new species shares most features with the genus Leptodactylus, although externally it resembles species of Physalaemus as much as. species of Leptodactylus. The new species is provisionally assigned to the genus Leptodactylus, the definition of which must be expanded to include an areolate belly and small osteoderms lying above the vertebral column in order to accommodate the new species. The new species is known: only from a single cerrado enclave in a predominantly Amazonian rainforest landscape. C1 Smithsonian Inst, Washington, DC 20013 USA. Calif Acad Sci, Res Assoc Herpetol, San Francisco, CA 94118 USA. RP Heyer, WR (reprint author), Smithsonian Inst, MRC 162,POB 37012, Washington, DC 20013 USA. EM heyerr@si.edu; rcrombie@calacademy.org NR 8 TC 4 Z9 4 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 2 PY 2005 VL 118 IS 3 BP 590 EP 595 DI 10.2988/0006-324X(2005)118[590:LLADNS]2.0.CO;2 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 962RO UT WOS:000231750100015 ER PT J AU Carleton, MD Stanley, WT AF Carleton, MD Stanley, WT TI Review of the Hylomyscus denniae complex (Rodentia : Muridae) in Tanzania, with a description of a new species SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID MORPHOLOGICAL EVOLUTION; AFRICAN POPULATIONS; MUROID RODENTS; DIFFERENTIATION; ZYGODONTOMYS AB Based on morphological and morphometric comparisons, a new species of Hylomyscus, H. arcimontensis (Muridae: Murinae), is identified from Mount Rungwe and the Eastern Arc Mountains of central and eastern Tanzania. The new species is confined to wet montane forests of these mountains and represents another vertebrate endemic to the Tanganyika-Nyasa Montane Forest biotic region (sensu Moreau 1966). It is most closely related to H. anselli, a form described from mountains in northern Zambia as a subspecies of H. denniae and here elevated to species rank. Morphological evidence supports the view that the nominal species H. denniae is a composite of several species whose interrelationships and differentiation patterns indicate two species complexes: the H. denniae group centered in Central East African mountains (Burundi, Kenya, Rwanda, Uganda, Zaire) and the H. anselli group distributed across more southern mountains (Angola, Malawi, Tanzania, Zambia). C1 Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Dept Vertebrate Zool, Washington, DC 20560 USA. Field Museum Nat Hist, Div Mammals, Dept Zool, Chicago, IL 60605 USA. RP Carleton, MD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Dept Vertebrate Zool, Washington, DC 20560 USA. EM Carleton@si.edu; stanley@fieldmuseum.org NR 35 TC 30 Z9 35 U1 1 U2 5 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 SEP 2 PY 2005 VL 118 IS 3 BP 619 EP 646 DI 10.2988/0006-324X(2005)118[619:ROTHDC]2.0.CO;2 PG 28 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 962RO UT WOS:000231750100018 ER PT J AU Berry, PE Hipp, AL Wurdack, KJ Van Ee, B Riina, R AF Berry, PE Hipp, AL Wurdack, KJ Van Ee, B Riina, R TI Molecular phylogenetics of the giant genus Croton and tribe Crotoneae (Euphorbiaceae sensu stricto) using its and trnL-trnF DNA sequence data SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Astraea; Croton; Crotoneae; Euphorbiaceae; giant genus; ITS; molecular; phylogenetics; trnL-F ID NUCLEAR RIBOSOMAL DNA; ASTRAGALUS FABACEAE; CHROMOSOME-NUMBERS; CHLOROPLAST DNA; GENERA; INCONGRUENCE; SENSITIVITY; SYNOPSIS; REGIONS; SPACER AB Parsimony, likelihood, and Bayesian analyses of nuclear ITS and plastid trnL-F DNA sequence data are presented tor the giant genus Croton (Euphorbiaceae S.S.) and related taxa. Sampling comprises 88 taxa, including 78 of the estimated 1223 species and 29 of the 40 sections previously recognized of Croton, It also includes the satellite genus Moacroton and genera formerly placed in tribe Crotoneae. Croton and ail sampled segregate genera form a monophyletic group sister to Brasiliocroton, with (lie exception of Croton sect. Astraea, which is reinstated to the genus Astraea. A small clade including Moacroton, Croton alahamensis, and C, olivaceus is sister to all other Croton species sampled. The remaining Croton species fall into three major clades. One of these is entirely New World, corresponding to sections Cyclostigma. Cascarilla, and Velamea sensu Webster. The second is entirely Old World anti is to a third, also entirely New World clade, which is composed of it least 13 of Webster's sections of Croton. This study establishes a phylogenetic framework for future studies in the hyper-diverse genus Croton. indicates a New World origin for the genus, and will soon be used to evaluate wood anatomical, cytological, and morphological data in the Crotoneac tribe. C1 Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. Morton Arboretum, Lisle, IL 60532 USA. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Smithsonian Inst, Labs Anayt Biol, Washington, DC 20013 USA. NMNH, MRC 166, Washington, DC 20013 USA. RP Berry, PE (reprint author), Univ Wisconsin, Dept Bot, 430 Lincoln Dr, Madison, WI 53706 USA. EM peberry@wisc.edu RI Riina, Ricarda/J-1032-2014 OI Riina, Ricarda/0000-0002-7423-899X NR 56 TC 88 Z9 110 U1 0 U2 6 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 SEP PY 2005 VL 92 IS 9 BP 1520 EP 1534 DI 10.3732/ajb.92.9.1520 PG 15 WC Plant Sciences SC Plant Sciences GA 960JW UT WOS:000231587600014 PM 21646170 ER PT J AU Keita, SOY AF Keita, SOY TI History in the interpretation of the pattern of p49a,f Taql RFLP Y-chromosome variation in Egypt: A consideration of multiple lines of evidence SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Article ID HIGH-RESOLUTION ANALYSIS; MIGRATORY EVENTS; DNA HAPLOTYPES; AFRICA; JEWS; POPULATIONS; MIGRATIONS; ORIGINS; PHYLOGEOGRAPHY; PENINSULA AB The possible factors involved in the generation of p49a,f TaqI Y-chromosome spatial diversity in Egypt were explored. The object was to consider explanations beyond those that emphasize gene flow mediated via military campaigns within the Nile corridor during the dynastic period. Current patterns of the most common variants (V, XI, and IV) have been suggested to be primarily related to Middle Kingdom and New Kingdom political actions in Nubia, including occasional settler colonization, and the conquest of Egypt by Kush (in upper Nubia, northern Sudan), thus initiating the Twenty-Fifth Dynasty. However, a synthesis of evidence from archaeology, historical linguistics, texts, distribution of haplotypes outside Egypt, and some demographic considerations lends greater support to the establishment, before the Middle Kingdom, of the observed distributions of the most prevalent haplotypes V, XI, and IV. It is suggested that the pattern of diversity for these variants in the Egyptian Nile Valley was largely the product of population events that occurred in the late Pleistocene to mid-Holocene through the First Dynasty, and was sustained by continuous smaller-scale bidirectional migrations/interactions. The higher frequency of V in Ethiopia than in Nubia or upper (southern) Egypt has to be taken into account in any discussion of variation in the Nile Valley. C1 Howard Univ, Natl Ctr Human Genome Res, Ctr Canc, Howard Univ Hosp, Washington, DC 20060 USA. Smithsonian Inst, Dept Anthropol, Washington, DC 20060 USA. RP Keita, SOY (reprint author), Howard Univ, Natl Ctr Human Genome Res, Ctr Canc, Howard Univ Hosp, 2041 Georgia Ave NW, Washington, DC 20060 USA. NR 61 TC 5 Z9 5 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 SEP-OCT PY 2005 VL 17 IS 5 BP 559 EP 567 DI 10.1002/ajhb.20428 PG 9 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 961IO UT WOS:000231655700002 PM 16136533 ER PT J AU de Queiroz, K AF de Queiroz, K TI Cracking the code SO AMERICAN SCIENTIST LA English DT Letter C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP de Queiroz, K (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SIGMA XI-SCI RES SOC PI RES TRIANGLE PK PA PO BOX 13975, RES TRIANGLE PK, NC 27709 USA SN 0003-0996 J9 AM SCI JI Am. Scientist PD SEP-OCT PY 2005 VL 93 IS 5 BP 388 EP 388 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 954OY UT WOS:000231165600003 ER PT J AU Rothschild, B Naples, V AF Rothschild, B Naples, V TI Whale of a tale SO ANNALS OF THE RHEUMATIC DISEASES LA English DT Editorial Material ID ARTHRITIS; SPONDYLOARTHROPATHY C1 Arthrit Ctr NE Ohio, Youngstown, OH 44512 USA. NE Ohio Univ, Coll Med, Rootstown, OH 44527 USA. Carnegie Museum Nat Hist, Pittsburgh, PA 15213 USA. Univ Kansas, Museum Nat Hist, Lawrence, KS 66045 USA. Smithsonian Inst, USNM, Div Vertebrate Zool, Washington, DC 20506 USA. No Illinois Univ, Dept Biol Sci, De Kalb, IL 60115 USA. RP Rothschild, B (reprint author), Arthrit Ctr NE Ohio, 5500 Market, Youngstown, OH 44512 USA. EM bmr@neoucom.edu NR 7 TC 1 Z9 1 U1 0 U2 0 PU B M J PUBLISHING GROUP PI LONDON PA BRITISH MED ASSOC HOUSE, TAVISTOCK SQUARE, LONDON WC1H 9JR, ENGLAND SN 0003-4967 J9 ANN RHEUM DIS JI Ann. Rheum. Dis. PD SEP PY 2005 VL 64 IS 9 BP 1385 EP 1386 DI 10.1136/ard.2004.033423 PG 2 WC Rheumatology SC Rheumatology GA 955ER UT WOS:000231208700037 PM 16100354 ER PT J AU Burchett-Anderson, T AF Burchett-Anderson, T TI Birthplace of Country Music Alliance Museum. Bristol, Tennessee-Virginia. SO APPALACHIAN JOURNAL LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP Burchett-Anderson, T (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU APPALACHIAN STATE UNIV, CENTER APPALACHIAN STUDIES PI BOONE PA BELK LIBRARY, BOX 32026, BOONE, NC 28608 USA SN 0090-3779 J9 APPALACHIAN J JI Appalach. J. PD FAL PY 2005 VL 33 IS 1 BP 127 EP 128 PG 2 WC History; Literary Reviews SC History; Literature GA 006NI UT WOS:000234903800036 ER PT J AU Pedretti, E Traub, WA Monnier, JD Millan-Gabet, R Carleton, NP Schloerb, FP Brewer, MK Berger, JP Lacasse, MG Ragland, S AF Pedretti, E Traub, WA Monnier, JD Millan-Gabet, R Carleton, NP Schloerb, FP Brewer, MK Berger, JP Lacasse, MG Ragland, S TI Robust determination of optical path difference: fringe tracking at the Infrared Optical Telescope Array interferometer SO APPLIED OPTICS LA English DT Article ID IOTA INTERFEROMETER; PROTOTYPE; ENVELOPE AB We describe the fringe-packet tracking system used to equalize the optical path lengths at the Infrared Optical Telescope Array interferometer. The measurement of closure phases requires obtaining fringes on three baselines simultaneously. This is accomplished by use of an algorithm based on double Fourier interferometry for obtaining the wavelength-dependent phase of the fringes and a group-delay tracking algorithm for determining the position of the fringe packet. A comparison of data acquired with and without the fringe-packet tracker shows a factor of similar to 3 reduction of the error in the closure-phase measurement. The fringe-packet tracker has been able so far to track fringes with signal-to-noise ratios as low as 1.8 for stars as faint as m(H) = 7.0. (c) 2005 Optical Society of America. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Michigan, Ann Arbor, MI 48109 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Massachusetts, Amherst, MA 01003 USA. Lab Astrophys Grenoble, Grenoble 9, France. RP Pedretti, E (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM epedrett@umich.edu NR 38 TC 18 Z9 18 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 SEP 1 PY 2005 VL 44 IS 25 BP 5173 EP 5179 DI 10.1364/AO.44.005173 PG 7 WC Optics SC Optics GA 960FH UT WOS:000231575100002 PM 16149339 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ Prieto, CA Beers, TC Wilhelm, R AF Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ Prieto, CA Beers, TC Wilhelm, R TI The century survey Galactic halo project. II. Global properties and the luminosity function of field blue horizontal branch stars SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxy : halo; galaxy : stellar content; stars : horizontal-branch ID DIGITAL SKY SURVEY; A-TYPE STARS; METAL-POOR STARS; RR LYRAE STARS; DATA RELEASE; STATISTICAL PARALLAX; SOLAR CIRCLE; LARGE-SAMPLE; MILKY-WAY; HOT STARS AB We discuss a 175 deg(2) spectroscopic survey for blue horizontal branch (BHB) stars in the Galactic halo. We use the Two Micron All Sky Survey (2MASS) and the Sloan Digital Sky Survey (SDSS) to select BHB candidates, and we find that the 2MASS and SDSS color selection is 38% and 50% efficient, respectively, for BHB stars. Our samples include one likely runaway B7 star 6 kpc below the Galactic plane. The global properties of the BHB samples are consistent with membership in the halo population: the median metallicity is [Fe/H] = -1.7, the velocity dispersion is 108 km s(-1), and the mean Galactic rotation of the BHB stars 3 kpc < vertical bar z vertical bar < 15 kpc is -4 +/- 30 km s(-1). We discuss the theoretical basis of the Preston, Shectman, and Beers M-V-color relation for BHB stars and conclude that the intrinsic shape of the BHB MV-color relation results from the physics of stars on the horizontal branch. We calculate the luminosity function for the field BHB star samples using the maximum likelihood method of Efstathiou and coworkers, which is unbiased by density variations. The field BHB luminosity function exhibits a steep rise at bright luminosities, a peak between 0.8 < MV < 1.0, and a tail at faint luminosities. We compare the field BHB luminosity functions with the luminosity functions derived from 16 different globular cluster BHBs. Kolmogorov-Smirnov tests suggest that field BHB stars and BHB stars in globular clusters share a common distribution of luminosities, with the exception of globular clusters with extended BHBs. C1 Harvard Smithsonian Ctr Astrophys, Harvard Smithsonian Observ, Cambridge, MA 02138 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. RP Harvard Smithsonian Ctr Astrophys, Harvard Smithsonian Observ, 60 Garden St, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009; OI Kenyon, Scott/0000-0003-0214-609X; Kurtz, Michael/0000-0002-6949-0090 NR 51 TC 19 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2005 VL 130 IS 3 BP 1097 EP 1110 DI 10.1086/431976 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900015 ER PT J AU Doppmann, GW Greene, TP Covey, KR Lada, CJ AF Doppmann, GW Greene, TP Covey, KR Lada, CJ TI The physical natures of Class I and flat-spectrum protostellar photospheres: A near-infrared spectroscopic study SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : stars; stars : formation; stars : fundamental parameters; stars : late-type; stars : low-mass, brown dwarfs; stars : pre-main-sequence; stars : rotation; techniques : spectroscopic ID YOUNG STELLAR OBJECTS; T-TAURI STARS; AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; MAGNETOSPHERIC ACCRETION MODELS; SCORPIUS OB ASSOCIATION; INITIAL MASS FUNCTION; CO EMISSION; RADIAL-VELOCITIES; IRAS OBSERVATIONS AB We present high-resolution (R similar or equal to 18,000), high signal-to-noise ratio, 2 mu m spectra of 52 IR-selected Class I and flat-spectrum young stellar objects in the Taurus-Auriga, rho Ophiuchi, Serpens, Perseus, and Corona Australis dark clouds. We detect key absorption lines in 41 objects and fit synthetic spectra generated from pre-main-sequence models to deduce the effective temperatures, surface gravities, near-IR veilings, rotation velocities, and radial velocities of each of these 41 sources. We find these objects to span ranges in effective temperature, surface gravity, and stellar luminosity that appear similar to those of late spectral type Class II sources and classical T Tauri stars. However, because of significant but uncertain corrections for scattering and extinction, the derived luminosities for the embedded protostellar objects must be regarded as being highly uncertain. We determine that the mean 2 mu m veiling of Class I and flat-spectrum objects is significantly higher than that of Class II objects in the same region where both types of objects are extensively observed (rho Oph). We find that a significant fraction of our protostellar sample also exhibits emission lines. Twenty-three objects show H-2 emission, which is usually indicative of the presence of energetic outflows. Thirty-four sources show H I Br gamma emission, and a number of these exhibit profile asymmetries consistent with infall. Eight sources show significant Delta(v) = 2 CO emission suggestive of emission from a circumstellar disk. Overall, these observations indicate that Class I and flat-spectrum objects are self-embedded protostars undergoing significant mass accretion, although the objects appear to span a broad range of mass accretion activity. C1 NASA, Ames Res Ctr, Moffett Field, CA USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Assoc Univ Res Astron Inc, Gemini Observ, So Operat Ctr, Casilla 603, La Serena, Chile. EM doppmann@gemini.edu; thomas.p.greene@nasa.gov; covey@.astro.washington.edu; clada@cfa.harvard.edu OI Covey, Kevin/0000-0001-6914-7797 NR 90 TC 69 Z9 69 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2005 VL 130 IS 3 BP 1145 EP 1170 DI 10.1086/431954 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LX UT WOS:000231450900019 ER PT J AU Belloni, T Homan, J Casella, P van der Klis, M Nespoli, E Lewin, WHG Miller, JM Mendez, M AF Belloni, T Homan, J Casella, P van der Klis, M Nespoli, E Lewin, WHG Miller, JM Mendez, M TI The evolution of the timing properties of the black-hole transient GX 339-4 during its 2002/2003 outburst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; black hole physics; stars : oscillations; X-rays : binaries ID QUASI-PERIODIC OSCILLATIONS; MICROQUASAR GRO J1655-40; CANDIDATE XTE J1859+226; LOW-LUMINOSITY STATES; X-RAY VARIABILITY; GX 339-4; HIGH-FREQUENCY; RXTE OBSERVATIONS; LIGHT CURVES; GRS-1915+105 AB We present the results of the timing and color analysis of more than two hundred RXTE/PCA observations of the bright black-hole transient GX 339-4 obtained during its 2002/2003 outburst. The color-intensity evolution of the system, coupled to the properties of its fast time variability, allow the identification of four separate states. Depending on the state, strong noise is detected, together with a variety of quasi-periodic oscillations at frequencies from 0.2 to 8 Hz. We present a characterization of the timing parameters of these states and compare them to what has been observed in other systems. These results, together with those obtained from energy spectra, point towards a common evolution of black-hole transients through their outbursts. C1 INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. MIT, Ctr Space Res, Cambridge, MA 02139 USA. INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. Univ Rome 3, Dipartimento Fis, I-00146 Rome, Italy. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. RP Belloni, T (reprint author), INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy. EM belloni@merate.mi.astro.it RI Mendez, Mariano/C-8011-2012; OI Mendez, Mariano/0000-0003-2187-2708; Casella, Piergiorgio/0000-0002-0752-3301 NR 77 TC 200 Z9 203 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 SEP PY 2005 VL 440 IS 1 BP 207 EP U132 DI 10.1051/0004-6361:20042457 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957GO UT WOS:000231358000027 ER PT J AU Alencar, SHP Basri, G Hartmann, L Calvet, N AF Alencar, SHP Basri, G Hartmann, L Calvet, N TI The extreme T Tauri star RW Aur: accretion and outflow variability SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line : profiles; stars : formation; stars : pre main sequence; stars : winds, outflows; stars : individual : RW Aur ID TELESCOPE IMAGING SPECTROGRAPH; EMISSION-LINE DIAGNOSTICS; HAMILTON ECHELLE SPECTRA; YOUNG STARS; MAGNETOSPHERIC ACCRETION; MASS-LOSS; DISK ACCRETION; WINDS; JETS; AURIGAE AB We present an analysis of the classical T Tauri star RW Aur A, based on 77 echelle spectra obtained at Lick Observatory over a decade of observations. RW Aur, which has a higher than average mass accretion rate among T Tauri stars, exhibits permitted ( H alpha, H beta, Ca II, He I, NaD) and forbidden ([OI] 6300 angstrom) emission lines with strong variability. The permitted lines display multiple periodicities over the years, often with variable accretion (redshifted) and outflow (blueshifted) absorption components, implying that both processes are active and changing in this system. The broad components of the different emission lines exhibit correlated behavior, indicating a common origin for all of them. We compute simple magnetospheric accretion and disk-wind H alpha, H beta and NaD line profiles for RW Aur. The observed Balmer emission lines do not have magnetospheric accretion line profiles. Our modeling indicates that the wind contribution to these line profiles is very important and must be taken into account. Our results indicate that the H alpha, H beta and NaD observed line profiles of RW Aur are better reproduced by collimated disk-winds starting from a small region near the disk inner radius. Calculations were performed in a region extending out to 100 R-*. Within this volume, extended winds originating over many stellar radii along the disk are not able to reproduce the three lines simultaneously. Strongly open-angled winds also generate profiles that do not look like the observed ones. We also see evidence that the outflow process is highly dynamic - the low- and high- velocity components of the [OI]( 6300 angstrom) line vary independently on timescales of days. The apparent disappearance from December 1999 to December 2000 of the [OI]( 6300 angstrom) low velocity component, which is thought to come from the disk-wind, shows that the the slow wind can exhibit dramatic variability on timescales of months ( placing limits on how extended it can be). There is no comprehensive explanation yet for the behavior of RW Aur, which may in part be due to complications that would be introduced if it is actually a close binary. C1 UFMG, ICEx, Dept Fis, BR-30123970 Belo Horizonte, MG, Brazil. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Alencar, SHP (reprint author), UFMG, ICEx, Dept Fis, CP 702, BR-30123970 Belo Horizonte, MG, Brazil. EM silvia@fisica.ufmg.br; basri@astro.berkeley.edu; hartmann@cfa.harvard.edu; ncalvet@cfa.harvard.edu RI Alencar, Silvia/C-2803-2013 NR 50 TC 49 Z9 49 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 SEP PY 2005 VL 440 IS 2 BP 595 EP 608 DI 10.1051/0004-6361:20053315 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959VM UT WOS:000231547400026 ER PT J AU Ramsay, G Hakala, P Marsh, T Nelemans, G Steeghs, D Cropper, M AF Ramsay, G Hakala, P Marsh, T Nelemans, G Steeghs, D Cropper, M TI XMM-Newton observations of AM CVn binaries SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars : binaries : general; stars : novae : cataclysmic variables; X-rays : binaries; stars : individual : AM CVn, HP lib, CR boo, GP com ID NONMAGNETIC CATACLYSMIC VARIABLES; X-RAY; CANUM-VENATICORUM; ACCRETION DISK; GP COMAE; QUIESCENCE; SPECTRUM; NITROGEN; STARS AB We present the results of XMM-Newton observations of four AM CVn systems - AM CVn, CR Boo, HP Lib and GP Com. Their light curves show very different characteristics. The X-ray light curves show no coherent pulsations, suggesting the accreting white dwarfs have relatively low magnetic field strengths. Their spectra were best modelled using a multi-temperature emission model and a strong UV component. We find that CR Boo and HP Lib have X-ray spectra with abundances consistent with relatively low temperature CNO processed material, while AM CVn and GP Com show an enhancement of nitrogen. A large fraction of the accretion luminosity is emitted in the UV. We determine accretion luminosities of similar to 1.6 x 10(33) erg s(-1) and 1.7 x 10(31) erg s(-1) for AM CVn and GP Com respectively. Comparing the implied mass transfer rates with that derived using model fits to optical and UV spectra, we find evidence that in the case of AM CVn, we do not detect a significant proportion of the accretion energy. This missing component could be lost in the form of a wind. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Helsinki, FIN-00014 Helsinki, Finland. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Radboud Univ Nijmegen, Dept Astrophys, NL-6500 Nijmegen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ramsay, G (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM gtbr@mssl.ucl.ac.uk RI Cropper, Mark/C-1574-2008; Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746 NR 31 TC 14 Z9 14 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 SEP PY 2005 VL 440 IS 2 BP 675 EP 681 DI 10.1051/0004-6361:20052950 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959VM UT WOS:000231547400034 ER PT J AU Rodriguez-Gil, P Gansicke, BT Hagen, HJ Nogami, D Torres, MAP Lehto, H Aungwerojwit, A Littlefair, S Araujo-Betancor, S Engels, D AF Rodriguez-Gil, P Gansicke, BT Hagen, HJ Nogami, D Torres, MAP Lehto, H Aungwerojwit, A Littlefair, S Araujo-Betancor, S Engels, D TI HS0943+1404, a true intermediate polar SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disc; stars : binaries : close; stars : novae, cataclysmic variables ID CATACLYSMIC VARIABLES; ORBITAL PERIOD; EX-HYDRAE; LINE SPECTRUM; DWARF NOVA; LOW STATES; SPECTROSCOPY; PHOTOMETRY; GAP; EXTRACTION AB We have identified a new intermediate polar, HS 0943+ 1404, as part of our ongoing search for cataclysmic variables in the Hamburg Quasar Survey. The orbital and white dwarf spin periods determined from time-resolved photometry and spectroscopy are P-orb similar or equal to 250 min and P-spin = 69.171 +/- 0.001 min, respectively. The combination of a large ratio P-spin/P-orb similar or equal to 0.3 and a long orbital period is very unusual compared to the other known intermediate polars. The magnetic moment of the white dwarf is estimated to be mu(1) similar to 10(34) Gcm(3), which is in the typical range of polars. Our extensive photometry shows that HS 0943+ 1404 enters into deep (similar to 3mag) low states, which are also a characteristic feature of polars. We therefore suggest that the system is a true "intermediate" polar that will eventually synchronise, that is, a transitional object between intermediate polars and polars. The optical spectrum of HS 0943+1404 also exhibits a number of unusual emission lines, most noticeably NII lambda 5680, which is likely to reflect enhanced nitrogen abundances in the envelope of the secondary. C1 Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Inst Astrofis Canarias, Santa Cruz de Tenerife 38205, Spain. Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. Kyoto Univ, Hida Observ, Gifu 5061314, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Turku Univ, Tuorla Observ, Piikkio 21500, Finland. Turku Univ, Dept Phys, Turku 20014, Finland. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Rodriguez-Gil, P (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM prguez@iac.es RI Gaensicke, Boris/A-9421-2012; Rodriguez-Gil, Pablo/H-7709-2015 OI Gaensicke, Boris/0000-0002-2761-3005; Rodriguez-Gil, Pablo/0000-0002-4717-5102 NR 44 TC 14 Z9 14 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 SEP PY 2005 VL 440 IS 2 BP 701 EP 709 DI 10.1051/0004-6361:20053141 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959VM UT WOS:000231547400037 ER PT J AU Henkel, C Jethava, N Kraus, A Menten, KM Carilli, CL Grasshoff, M Lubowich, D Reid, AJ AF Henkel, C Jethava, N Kraus, A Menten, KM Carilli, CL Grasshoff, M Lubowich, D Reid, AJ TI The kinetic temperature of a molecular cloud at redshift 0.7: ammonia in the gravitational lens B0218+357 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : abundances; galaxies : ISM; quasars : individual : B0218+357; quasars : absorption lines; radio lines : galaxies ID EINSTEIN RING B0218+357; STAR-FORMING REGIONS; NEARBY GALAXIES; DENSE GAS; SYSTEM B0218+357; HOT AMMONIA; (CO)-O-18/(CO)-O-17 RATIO; INTERSTELLAR AMMONIA; VLBI OBSERVATIONS; ABUNDANCE RATIO AB Using the Effelsberg 100-m telescope, absorption in the (J, K) = ( 1, 1), ( 2, 2) and ( 3, 3) inversion lines of ammonia (NH3) was detected at a redshift of z = 0.6847 toward the gravitational lens system B0218 + 357. The lambda similar to 2 cm absorption peaks at 0.5 - 1.0% of the continuum level and appears to cover a smaller fraction of the radio continuum background than lines at millimeter wavelengths. Measured intensities are consistent with a rotation temperature of similar to 35K, corresponding to a kinetic temperature of similar to 55 K. The column density toward the core of image A then becomes N(NH3) similar to 1 x 10(14) cm(-2) and fractional abundance and gas density are of order X(NH3) similar to 10(-8) and n(H-2) similar to 5 x 10(3) cm(-3), respectively. Upper limits are reported for the ( 2, 1) and ( 4, 4) lines of NH3 and for transitions of the SO, DCN, OCS, SiO, C3N, H2CO, SiC2, HC3N, HC5N, and CH3OH molecules. These limits and the kinetic temperature indicate that the absorption lines are not arising from a cold dark cloud but from a warm, diffuse, predominantly molecular medium. The physical parameters of the absorbing molecular complex, seen at a projected distance of similar to 2 kpc to the center of the lensing galaxy, are quite peculiar when compared with the properties of clouds in the Galaxy or in nearby extragalactic systems. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Henkel, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM chenkel@mpifr-bonn.mpg.de NR 61 TC 44 Z9 44 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2005 VL 440 IS 3 BP 893 EP 899 DI 10.1051/0004-6361:20052816 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961VG UT WOS:000231689300011 ER PT J AU Strassmeier, KG Rice, JB Ritter, A Kuker, M Hussain, GAJ Hubrig, S Shobbrook, R AF Strassmeier, KG Rice, JB Ritter, A Kuker, M Hussain, GAJ Hubrig, S Shobbrook, R TI Spatially resolving the accretion shocks on the rapidly-rotating M0 T-Tauri star MN Lupi SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : activity; starspots; stars : imaging; stars : individual : MN Lup; stars : individual : T Tauri; stars : pre-main sequence ID T-TAURI STARS; STELLAR SURFACE-STRUCTURE; COLOR-MAGNITUDE DIAGRAMS; MAGNETIC NEUTRON STARS; MAIN-SEQUENCE STARS; LINE-DATA-BASE; DISK ACCRETION; YOUNG STARS; BOLOMETRIC CORRECTIONS; ECHELLE SPECTROGRAPH AB We obtained high-resolution, high-quality VLT/UVES spectra to reconstruct the two-dimensional surface structure of the rapidly-rotating classical T-Tauri star MN Lupi on two separate nights. Both surface maps show a structured warm (5000 K) band centered around the pole at a latitude of approximate to 65 degrees. Located within the band are two hot spots with temperatures of approximately or possibly even in excess of 5800 K, i.e. 2000 K above the effective photospheric temperature. Both maps appear with an adjacent equatorial band of temperature 3400 K, some 400-500 K below the effective photospheric temperature. While we interpret the two hot spots and the warm high-latitude band to be the heating points from two accretion impacts at the time of our observations and their redistributed energy trailed due to the fast stellar rotation, respectively, the cool equatorial band may not be cool after all but due to obscuration of the stellar surface by the innermost region of the disk. The fact that the hot spots appear at high stellar latitude is in agreement with the magnetospheric accretion model that proposes material funnelling onto the star along a predominantly dipolar magnetic field at roughly 50 degrees latitude. The evidence of ongoing disk accretion, together with the very fast rotation of MN Lupi of just 3-4 times below its break-up velocity, suggests that the accretion mechanism is the cause of its rapid surface rotation. We present a model of magnetic star-disk coupling for MN Lupi that predicts a polar surface magnetic field of approximate to 3 kG. C1 Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Brandon Univ, Dept Phys, Brandon, MB R7A 6A9, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, Santiago 19001, Chile. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Strassmeier, KG (reprint author), Astrophys Inst Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. EM KStrassmeier@aip.de; ARitter@aip.de; MKueker@aip.de NR 63 TC 18 Z9 18 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 SEP PY 2005 VL 440 IS 3 BP 1105 EP 1118 DI 10.1051/0004-6361:20052901 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 961VG UT WOS:000231689300029 ER PT J AU Leipski, C Haas, M Meusinger, H Siebenmorgen, R Chini, R Scheyda, CM Albrecht, M Wilkes, BJ Huchra, JP Ott, S Cesarsky, C Cutri, R AF Leipski, C Haas, M Meusinger, H Siebenmorgen, R Chini, R Scheyda, CM Albrecht, M Wilkes, BJ Huchra, JP Ott, S Cesarsky, C Cutri, R TI The ISO-2MASS AGN survey: on the type-1 sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : fundamental parameters; galaxies : photometry; quasars : general; infrared : galaxies ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; ISOCAM PARALLEL MODE; SKY SURVEY; QUASARS; SELECTION; CATALOG; SAMPLE AB We combined the ISOCAM Parallel Mode Survey at 6.7 mu m (LW2 filter) with the 2 Two Micron All Sky Survey in order to obtain a powerful tool to search for AGN independent of dust extinction. Using moderate colour criteria H - K > 0.5 and K-LW2 > 2.7 we have selected a sample of 77 AGN candidates in an effective area of similar to 10 square degrees. By means of optical spectroscopy we find 24 (similar to 30%) type-1 QSOs at redshifts 0 0.1 < z < 2.3; nine of them have z > 0.8. About one third of the ISO-2MASS QSOs show so red optical colours, that they are missed in optical and UV AGN surveys like SDSS, 2DF, or HES. With a surface density of about 2 deg(-2) down to R < 18 mag the ISO-2MASS QSOs outnumber the 1.35 deg-2 of the SDSS quasar survey by 50%; we find a combined optical-IR QSO surface density of 2.7 deg(-2). Since only two of the ISO-2MASS. QSOs have also J - K > 2, the inclusion of the ISO mid-infrared photometry significantly extends the capabilities of the pure 2MASS red AGN survey. We suggest that the newly found red AGN resemble young members of the quasar population, and that quasars spend much of their lifetime in a dust enshrouded phase. C1 AIRUB, D-44780 Bochum, Germany. TLS, D-07778 Tautenburg, Germany. ESO, D-85748 Garching, Germany. Univ Catolica Norte, Inst Astron, Antofagasta, Chile. CFA, 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), AIRUB, Univ Str 150, D-44780 Bochum, Germany. EM leipski@astro.rub.de OI Wilkes, Belinda/0000-0003-1809-2364 NR 25 TC 15 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2005 VL 440 IS 1 BP L5 EP U11 DI 10.1051/0004-6361:200500152 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 957GO UT WOS:000231358000002 ER PT J AU Craspi, A DeVries, CH Huard, TL Lee, JE Myers, PC Ridge, NA Bourke, TL Evans, NJ Jorgensen, JK Kauffmann, J Lee, CW Shirley, YL Young, CH AF Craspi, A DeVries, CH Huard, TL Lee, JE Myers, PC Ridge, NA Bourke, TL Evans, NJ Jorgensen, JK Kauffmann, J Lee, CW Shirley, YL Young, CH TI Dynamical and chemical properties of the "starless" core L1014 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : clouds; ISM : evolution; ISM : individual objects : L1014; ISM : molecules; ISM : jets and outflows; stars : formation ID YOUNG STELLAR OBJECTS; INFALL MOTIONS; PROTOSTELLAR COLLAPSE; MOLECULAR OUTFLOWS; DUST EXTINCTION; SCUBA SURVEY; DARK CLOUDS; DENSE CORES; CS 2-1; PROTOSTARS AB Spitzer Space Telescope observations of a point-like source, L1014-IRS, close to the dust peak of the low-mass dense core L1014, have raised questions about its starless nature. These show the presence of an object with colors expected for an embedded protostar with the implication that L1014-IRS would be the lowest luminosity isolated protostar known, and an ideal target with which to test star formation theories at the low mass end. In order to study its molecular content and to search for the presence of a molecular outflow, we mapped L1014 in at least one transition of (12)CO, N(2)H(+), HCO(+), CS, and of their isotopologues (13)CO, C(18)O, C(17)O, N(2)D(+), and H(13)CO(+), using the Five College Radio Astronomy Observatory (FCRAO), the IRAM 30 m antenna, and the Caltech Submillimeter Observatory (CSO). The data show physical and chemical properties in L1014 typical of moderately evolved dense cores: i.e. H(2) central density of a few 10(5) molecules cm(-3), estimated mass of similar to 2 M(circle dot), CO integrated depletion factor less than 10, N(N(2)H(+)) similar or equal to 6 x 10(12) cm(-2), N(N(2)D(+))/N(N(2)H(+)) equal to 10%, and relatively broad N(2)H(+) and N(2)D(+) lines (0.35 km s(-1)). Infall signatures and significant velocity shifts between optically thick and optically thin tracers are not observed in the line profiles. No classical signatures of molecular outflow are found in the (12)CO and (13)CO FCRAO observations. In particular, no high velocity wings are found, and no well-defined blue-red lobes of (12)CO emission are seen in the channel maps. Sensitive, higher resolution observations will clarify the presence of a molecular outflow on a smaller scale than that probed by our observations. C1 Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Univ Texas, Austin, TX 78712 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. Max Planck Inst Radioastron, Bonn, Germany. Korea Astron & Space Sci Inst, Taejon 305348, South Korea. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Craspi, A (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM craspsi@arcetri.astro.it RI Lee , Jeong-Eun/E-2387-2013; Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 NR 41 TC 37 Z9 37 U1 0 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 SEP PY 2005 VL 439 IS 3 BP 1023 EP 1032 DI 10.1051/004-6361:20042411 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 955EA UT WOS:000231206900021 ER PT J AU Perez-Gonzalez, PG Rieke, GH Egami, E Alonso-Herrero, A Dole, H Papovich, C Blaylock, M Jones, J Rieke, M Rigby, J Barmby, P Fazio, GG Huang, J Martin, C AF Perez-Gonzalez, PG Rieke, GH Egami, E Alonso-Herrero, A Dole, H Papovich, C Blaylock, M Jones, J Rieke, M Rigby, J Barmby, P Fazio, GG Huang, J Martin, C TI Spitzer view on the evolution of star-forming galaxies from z=0 to z similar to 3 SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : evolution; galaxies : high-redshift; galaxies : photometry; galaxies : starburst; infrared : galaxies ID HUBBLE-DEEP-FIELD; ULTRAVIOLET LUMINOSITY DENSITY; FRANCE REDSHIFT SURVEY; DIGITAL SKY SURVEY; X-RAY SOURCES; ESTIMATING PHOTOMETRIC REDSHIFTS; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; ARTIFICIAL NEURAL-NETWORKS AB We use a 24 mu m - selected sample containing more than 8000 sources to study the evolution of star- forming galaxies in the redshift range from z = 0 to z similar to 3. We obtain photometric redshifts for most of the sources in our survey using a method based on empirically built templates spanning from ultraviolet to mid- infrared wavelengths. The accuracy of these redshifts is better than 10% for 80% of the sample. The derived redshift distribution of the sources detected by our survey peaks at around z 0: 6 1: 0 ( the location of the peak being affected by cosmic variance) and decays monotonically from z similar to 1 to z similar to 3. We have fitted infrared luminosity functions in several redshift bins in the range 0 < z less than or similar to 3. Our results constrain the density and/ or luminosity evolution of infrared- bright star- forming galaxies. The typical infrared luminosity ( L*) decreases by an order of magnitude from z similar to 2 to the present. The cosmic star formation rate ( SFR) density goes as ( 1+ z) (4. 0 +/- 0. 2) from z= 0 to 0.8. From z= 0. 8 z similar to 1. 2, the SFR density continues rising with a smaller slope. At 1: 2 < z <= 3, the cosmic SFR density remains roughly constant. The SFR density is dominated at low redshift ( z less than or similar to 0: 5) by galaxies that are not very luminous in the infrared ( L-TIR < 10(11) L-circle dot, where L-TIR is the total infrared luminosity, integrated from 8 to 1000 mu m). The contribution from luminous and ultraluminous infrared galaxies ( L-TIR > 10(11) L-circle dot) to the total SFR density increases steadily from z similar to 0 up to z similar to 2.5, forming at least half of the newly born stars by z similar to 1. 5. Ultraluminous infrared galaxies ( L-TIR > 10(12) L-circle dot) play a rapidly increasing role for z greater than or similar to 1.3. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CSIC, Inst Estructura Mat, E-28006 Madrid, Spain. Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Rigby, Jane/D-4588-2012; Alonso-Herrero, Almudena/H-1426-2015; OI Rigby, Jane/0000-0002-7627-6551; Alonso-Herrero, Almudena/0000-0001-6794-2519; Barmby, Pauline/0000-0003-2767-0090 NR 169 TC 379 Z9 379 U1 0 U2 9 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 SEP 1 PY 2005 VL 630 IS 1 BP 82 EP 107 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700007 ER PT J AU Greene, JE Ho, LC AF Greene, JE Ho, LC TI Estimating black hole masses in active galaxies using the H alpha emission line SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : jets; galaxies : nuclei; galaxies : Seyfert; quasars : general ID DIGITAL SKY SURVEY; QUASI-STELLAR OBJECTS; RADIO-LOUD QUASARS; GALACTIC NUCLEI; SEYFERT-GALAXIES; VELOCITY DISPERSION; ASTRONOMICAL DATA; REGION SIZES; LUMINOSITY; CONTINUUM AB It has been established that virial masses for black holes in low-redshift active galaxies can be estimated from measurements of the optical continuum strength and the width of the broad H beta line. Under various circumstances, however, both of these quantities can be challenging to measure or can be subject to large systematic uncertainties. To mitigate these difficulties, we present a new method for estimating black hole masses. From analysis of a new sample of broad-line active galactic nuclei, we find that H alpha luminosity scales almost linearly with optical continuum luminosity and that a strong correlation exists between H alpha and H beta line widths. These two empirical correlations allow us to translate the standard virial mass system to a new one based solely on observations of the broad H alpha emission line. 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 58 TC 282 Z9 285 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 SEP 1 PY 2005 VL 630 IS 1 BP 122 EP 129 DI 10.1086/431897 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700010 ER PT J AU Blazejowski, MB Blaylock, G Bond, IH Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Cogan, P Cui, W Daniel, M Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gammell, S Gibbs, K Gillanders, GG Grube, J Gutierrez, K Hall, J Hanna, D Holder, J Horan, D Humensky, B Kenny, G Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, M LeBohec, S Linton, E Evans, JL Maier, G Mendoza, D Milovanovic, A Moriarty, P Nagai, TN Ong, RA Mooney, BP Quinn, J Quinn, M Ragan, K Reynolds, PT Rebillot, P Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Valcarel, L Vassiliev, VV Wakely, SP Walker, G Weekes, TC White, R Zweerink, J Mochejska, B Smith, B Aller, M Aller, H Terasranta, H Boltwood, P Sadun, A Stanek, K Adams, E Foster, J Hartman, J Lai, K Bottcher, M Reimer, A Jung, I AF Blazejowski, MB Blaylock, G Bond, IH Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Cogan, P Cui, W Daniel, M Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gammell, S Gibbs, K Gillanders, GG Grube, J Gutierrez, K Hall, J Hanna, D Holder, J Horan, D Humensky, B Kenny, G Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, M LeBohec, S Linton, E Evans, JL Maier, G Mendoza, D Milovanovic, A Moriarty, P Nagai, TN Ong, RA Mooney, BP Quinn, J Quinn, M Ragan, K Reynolds, PT Rebillot, P Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Valcarel, L Vassiliev, VV Wakely, SP Walker, G Weekes, TC White, R Zweerink, J Mochejska, B Smith, B Aller, M Aller, H Terasranta, H Boltwood, P Sadun, A Stanek, K Adams, E Foster, J Hartman, J Lai, K Bottcher, M Reimer, A Jung, I CA VERITAS Collaboration TI A multiwavelength view of the TeV blazar markarian 421: Correlated variability, flaring, and spectral evolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (Markarian 421); galaxies : active; galaxies : jets; gamma rays : observations; radiation mechanisms : nonthermal; X-rays : galaxies ID ACTIVE GALAXY MARKARIAN-421; EXTRAGALACTIC RADIO-SOURCES; BL-LACERTAE OBJECTS; GAMMA-RAY EMISSION; X-RAY; CHERENKOV TELESCOPES; GALACTIC NUCLEI; LAC OBJECTS; AGN JETS; ENERGY AB We report results from an intensive multiwavelength monitoring campaign on the TeV blazar Mrk 421 over the period of 2003 - 2004. The source was observed simultaneously at TeV energies with the Whipple 10 m telescope and at X-ray energies with the Rossi X-Ray Timing Explorer (RXTE) during each clear night within the Whipple observing windows. Supporting observations were also frequently carried out at optical and radio wavelengths to provide simultaneous or contemporaneous coverages. The large amount of simultaneous data has allowed us to examine the variability of Mrk 421 in detail, including cross-band correlation and broadband spectral variability, over a wide range of flux. The variabilities are generally correlated between the X-ray and gamma-ray bands, although the correlation appears to be fairly loose. The light curves show the presence of flares with varying amplitudes on a wide range of timescales at both X-ray and TeV energies. Of particular interest is the presence of TeV flares that have no coincident counterparts at longer wavelengths, because the phenomenon seems difficult to understand in the context of the proposed emission models for TeV blazars. We have also found that the TeV flux reached its peak days before the X-ray flux did during a giant flare (or outburst) in 2004 (with the peak flux reaching similar to 135mcrab in X-rays, as seen by the RXTE ASM, and similar to 3 crab in gamma rays). Such a difference in the development of the flare presents a further challenge to both the leptonic and hadronic emission models. Mrk 421 varied much less at optical and radio wavelengths. Surprisingly, the normalized variability amplitude in the optical seems to be comparable to that in the radio, perhaps suggesting the presence of different populations of emitting electrons in the jet. The spectral energy distribution of Mrk 421 is seen to vary with flux, with the two characteristic peaks moving toward higher energies at higher fluxes. We have failed to fit the measured spectral energy distributions (SEDs) with a one-zone synchrotron self-Compton model; introducing additional zones greatly improves the fits. We have derived constraints on the physical properties of the X-ray/gamma-ray flaring regions from the observed variability (and SED) of the source. The implications of the results are discussed. C1 Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Natl Univ Ireland Univ Coll Dublin, Dept Phys, Dublin 4, Ireland. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Adler Planetarium & Astron Museum, Chicago, IL 60605 USA. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Oberv, Amado, AZ 85645 USA. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Depauw Univ, Dept Phys, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Sch Phys Sci, Galway, Ireland. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. Boltwood Observ, Stittsville, ON K2S 1N6, Canada. Univ Colorado, Dept Phys, Denver, CO 80217 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio Univ, Dept Astron, Athens, OH USA. Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany. RP Purdue Univ, Dept Phys, 525 Northwestern Ave, W Lafayette, IN 47907 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; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 59 TC 109 Z9 111 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 130 EP 141 DI 10.1086/431925 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700011 ER PT J AU Green, PJ Infante, L Lopez, S Aldcroft, TL Winn, JN AF Green, PJ Infante, L Lopez, S Aldcroft, TL Winn, JN TI Discovery of a galaxy cluster in the foreground of the wide-separation quasar pair UM 425 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (UM 425); X-rays : galaxies : clusters ID GRAVITATIONAL LENS CANDIDATE; ABSORPTION-LINE QUASARS; X-RAY; CHANDRA OBSERVATIONS; STELLAR OBJECTS; BINARY QUASARS; TIME-DELAY; UM 425; REDSHIFT; LAMBDA AB We report the discovery of a cluster of galaxies in the field of UM 425, a pair of quasars separated by 6."5. Based on this finding, we revisit the long-standing question of whether this quasar pair is a binary quasar or a wide-separation lens. Previous work has shown that both quasars are at z = 1.465 and show broad absorption lines. No evidence for a lensing galaxy has been found between the quasars, but there are two hints of a foreground cluster: diffuse X-ray emission observed with Chandra, and an excess of faint galaxies observed with the Hubble Space Telescope. Here we show, via VLT spectroscopy, that there is a spike in the redshift histogram of galaxies at z = 0.77. We estimate the chance of finding a random velocity structure of such significance to be about 5%, and thereby interpret the diffuse X-ray emission as originating from z = 0.77 rather than from the quasar redshift. The mass of the cluster, as estimated from either the velocity dispersion of the z = 0.77 galaxies or the X-ray luminosity of the diffuse emission, would be consistent with the theoretical mass required for gravitational lensing. The positional offset between the X-ray centroid and the expected location of the mass centroid is similar to 40 kpc, which is not too different from offsets observed in lower redshift clusters. However, UM 425 would be an unusual gravitational lens, by virtue of the absence of a bright primary lensing galaxy. Unless the mass-to-light ratio of the galaxy is at least 80 times larger than usual, the lensing hypothesis requires that the galaxy group or cluster plays a uniquely important role in producing the observed deflections. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Univ Chile, Dept Astron, Santiago, Chile. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pgreen@cfa.harvard.edu RI Lopez, Sebastian /I-5657-2016 OI Lopez, Sebastian /0000-0003-0389-0902 NR 51 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 142 EP 151 DI 10.1086/431946 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700012 ER PT J AU Krauss, MI Kilgard, RE Garcia, MR Roberts, TP Prestwich, AH AF Krauss, MI Kilgard, RE Garcia, MR Roberts, TP Prestwich, AH TI M74 X-1 (CXOU J013651.1+154547): An extremely variable ultraluminous X-ray source SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 628, M74); X-rays : individual (CXOU J013651.1+154547) ID MASS BLACK-HOLES; GRS 1915+105; CHANDRA OBSERVATIONS; NEARBY GALAXIES; LUMINOSITY; OSCILLATIONS; BINARIES; VARIABILITY; EMISSION; ANTENNAE AB Ultraluminous X-ray sources (ULXs) have been described variously as the most luminous normal X-ray binaries, hypernovae, and "intermediate-mass'' black holes with masses of hundreds to thousands of solar masses. We present results on M74 X-1 (CXOU J013651.1+ 154547), a ULX in the nearby spiral galaxy M74 ( NGC 628), from observations by Chandra and XMM-Newton. M74 X-1 is a persistent source that exhibits extreme variability and changes in spectral state on timescales of several thousand seconds. Its variability timescales and behavior resemble some Galactic microquasars. This suggests that the emission mechanism may be related to relativistically beamed jets and that M74 X-1 could be an extragalactic "microblazar'' -a microquasar whose jet axis is aligned with our line of sight. We also note that its spectrum is consistent with the presence of a low-temperature disk blackbody component, which, assuming it is due to radiation from an accretion disk, could indicate that M74 X-1 contains an intermediate-mass black hole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02139 USA. Univ Leicester, Leicester LE1 7RH, Leics, England. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 46 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 228 EP 237 DI 10.1086/431784 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700018 ER PT J AU Machacek, ME Nulsen, P Stirbat, L Jones, C Forman, WR AF Machacek, ME Nulsen, P Stirbat, L Jones, C Forman, WR TI XMM-Newton observation of an X-ray trail between the spiral galaxy NGC 6872 and the central elliptical galaxy NGC 6876 in the Pavo group SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : individual (NGC 6876 NGC 6872) intergalactic medium; X-rays : galaxies ID VIRGO-CLUSTER; HOT GAS; INTERGALACTIC MEDIUM; INTRACLUSTER MEDIUM; INTRAGROUP MEDIUM; HRI OBSERVATIONS; FORNAX CLUSTER; RICH CLUSTERS; COLD FRONTS; S0 GALAXIES AB We present XMM-Newton observations of a trail of enhanced X-ray emission extending along the full 8.'7; 40 region between the large spiral galaxy NGC 6872 and the dominant elliptical galaxy NGC 6876 in the Pavo group, the first known X-ray trail associated with a spiral galaxy in a poor galaxy group and, with a projected length of 90 kpc, one of the longest known X-ray trails. The X-ray surface brightness in the trail region is roughly constant beyond similar to 20 kpc of NGC 6876 in the direction of the spiral galaxy. The trail is hotter (similar to 1 keV) than the undisturbed Pavo IGM (similar to 0.5 keV) and has low metal abundances (0.2 Z(circle dot)). The 0.5-2 keV luminosity of the trail, measured using a 67; 90 kpc rectangular region, is 6: 6; 1040 ergs s(-1). We compare the properties of gas in the trail to the spectral properties of gas in the spiral galaxy NGC 6872 and in the elliptical galaxy NGC 6876 to constrain its origin. We suggest that the X-ray trail is either IGM gas gravitationally focused into a Bondi-Hoyle wake, a thermal mixture of similar to 60% Pavo IGM gas with similar to 40% galaxy gas that has been removed from the spiral galaxy NGC 6872 by turbulent viscous stripping, or both, due to the spiral galaxy's supersonic motion at angle xi similar to 40 degrees with respect to the plane of the sky, through the densest region of the Pavo IGM. Assuming xi similar to 40 degrees and a filling factor eta in a cylindrical volume with radius 33 kpc and projected length 90 kpc, the mean electron density and total hot gas mass in the trail are 1; 10(-3) eta(-1/2) cm(-3) and 1: 1; 10(10) eta(1/2) M-circle dot, respectively. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 67, Cambridge, MA 02138 USA. EM mmachacek@cfa.harvard.edu; pnulsen@head-cfa.cfa.harvard.edu; lstirbat@fas.harvard.edu; cjf@head.cfa.harvard.edu; wrf@head-cfa.cfa.harvard.edu OI Stirbat, Liviu/0000-0001-7106-5512; Forman, William/0000-0002-9478-1682 NR 77 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 280 EP 297 DI 10.1086/431944 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700022 ER PT J AU Gonzalez, ME Kaspi, VM Camilo, F Gaensler, BM Pivovaroff, MJ AF Gonzalez, ME Kaspi, VM Camilo, F Gaensler, BM Pivovaroff, MJ TI Unusual pulsed X-ray emission from the young, high magnetic field pulsar PSR J1119-6127 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G292.2-0.5); pulsars : individual (PSR J1119-6127); supernova remnants; X-rays : ISM ID SUPERNOVA REMNANT G292.2-0.5; SOFT GAMMA-REPEATERS; NEUTRON-STARS; RADIO PULSARS; CONSTRAINTS; J1119-6127; MODELS; SPECTROSCOPY; SURFACE; OBJECT AB We present XMM-Newton observations of the radio pulsar PSR J1119-6127, which has an inferred age of 1700 yr and surface dipole magnetic field strength of 4: 1; 1013 G. We report the first detection of pulsed X-ray emission from PSR J1119-6127. In the 0.5-2.0 keV range, the pulse profile shows a narrow peak with a very high pulsed fraction of 74% +/- 14%. In the 2.0-10.0 keV range, the upper limit for the pulsed fraction is 28% (99% confidence). The pulsed emission is well described by a thermal blackbody model with a temperature of T-infinity = 2.4(-0.2)(+0.3) x 10(6) K and emitting radius of 3.4(-0.3)(+1.8) km (at a distance of 8.4 kpc). Atmospheric models result in problematic estimates for the distance/emitting area. PSR J1119-6127 is now the radio pulsar with smallest characteristic age from which thermal X- ray emission has been detected. The combined temporal and spectral characteristics of this emission are unlike those of other radio pulsars detected at X- ray energies and challenge current models of thermal emission from neutron stars. 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 McGill Univ, Dept Phys, Rutherford Phys Bldg, Montreal, PQ H3A 2T8, Canada. 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 40 TC 45 Z9 45 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP 489 EP 494 DI 10.1086/432032 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700037 ER PT J AU Long, KS Froning, CS Knigge, C Blair, WP Kallman, TR Ko, YK AF Long, KS Froning, CS Knigge, C Blair, WP Kallman, TR Ko, YK TI Far-ultraviolet spectroscopy of the dwarf novae SS cygni and WX Hydri in quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; binaries : close; novae, cataclysmic variables; stars : individual ( SS Cygni, WX Hydri); ultraviolet : stars ID HIGH-RESOLUTION SPECTROGRAPH; DISC INSTABILITY MODEL; ROTATING WHITE-DWARF; LONG-TERM BEHAVIOR; U-GEMINORUM; CATACLYSMIC VARIABLES; X-RAY; ACCRETION DISK; VW-HYDRI; OPTICAL OBSERVATIONS AB We present time-resolved FUV spectra of the dwarf novae SS Cyg and WX Hyi in quiescence from observations using the Hopkins Ultraviolet Telescope on the Astro-1 and Astro-2 space shuttle missions and the Goddard High Resolution Spectrograph on the Hubble Space Telescope. Both dwarf novae are characterized by blue continua that extend to the Lyman limit punctuated by broad emission lines including transitions of O VI, N V, Si IV, andC IV. The continuum of WX Hyi can be fitted with a white dwarf model with physically reasonable model parameters, but neither system actually shows unambiguous signatures of white dwarf emission. The shape and flux of the spectrum of SS Cyg cannot be self-consistently reconciled with a white dwarf providing all of the FUV continuum flux. Combination white dwarf/disk or white dwarf/optically thin plasma models improve the fit but still do not give physically reasonable model parameters for a quiescent dwarf nova. Assuming that the UV emission lines arise from the disk, the line shapes indicate that surface fluxes fall roughly as R-2 in both systems. Fits to the double-peaked line profiles in SS Cyg indicate that the FUV line-forming region is concentrated closer to the white dwarf than that of the optical lines and provide no evidence of a hole in the inner disk. Although the flux from SS Cyg was relatively constant during all of our observations, WX Hyi showed significant variability during the GHRS observations. In WX Hyi, the line and continuum fluxes are (with the exception of He II) highly correlated, indicating a link between the formation mechanisms of the line and continuum regions. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM long@stsci.edu; cfroning@casa.colorado.edu; christian@astro.soton.ac.uk; wpb@pha.jhu.edu; tim@xstar.gsfc.nasa.gov; yko@cfa.harvard.edu NR 66 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 SEP 1 PY 2005 VL 630 IS 1 BP 511 EP 527 DI 10.1086/432088 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700040 ER PT J AU Schrijver, CJ van Ballegooijen, AA AF Schrijver, CJ van Ballegooijen, AA TI Is the quiet-sun corona a quasi-steady, force-free environment? SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : corona; sun : magnetic fields ID SOLAR TRANSITION REGION; AB-INITIO APPROACH; ACTIVE-REGION; MAGNETIC-FIELD; ENERGY-BALANCE; LOOPS; MODELS; LINES; DYNAMICS; NETWORK AB We model a coronal volume over a quiet, mixed-polarity solar network as an ensemble of quasi-steady loop atmospheres. These are contained by an assumed potential field, including the associated variations in the loop cross section through the coronal volume and the loop flows induced by such asymmetries. The average temperature and density stratifications are close to those of the quiet-Sun corona for a coronal heating flux density into the corona of F-H = 8 X 10(14)B/L (ergs cm(-2) s(-1)) for loop-base field strengths B ( G) and loop half-lengths L ( cm). Earlier, that heating parameterization was shown to be consistent with the appearance and radiative losses of a solar corona in which active regions dominated the emission. This study thus supports the hypothesis that the same, likely braiding-driven, heating dominates throughout the quiescent corona. The average ratio beta of gas to magnetic pressure lies close to unity throughout the modeled coronal height range of 22 Mm, with beta > 1 in similar to 30% of the volume and beta > 0: 4 in similar to 90% of the volume, perhaps indicating that the quiet-Sun corona is driven to near its maximum heating capacity by the random walk of its footpoints. Our findings that the solar corona has beta close to unity, and that our model corona exhibits insufficient fine structure and no significant spatially averaged Doppler shifts, imply that the quiet-Sun corona is often neither quasi-steady nor force free and thus that dynamic magnetohydrodynamics (MHD) models are essential to furthering our understanding of the quiet solar corona. C1 Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lockheed Martin Adv Technol Ctr, 3251 Hanover St, Palo Alto, CA 94304 USA. EM schryver@lmsal.com; vanballe@cfa.harvard.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 30 TC 36 Z9 36 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 SEP 1 PY 2005 VL 630 IS 1 BP 552 EP 560 DI 10.1086/431754 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JD UT WOS:000231439700044 ER PT J AU Chatterjee, S Vlemmings, WHT Brisken, WF Lazio, TJW Cordes, JM Goss, WM Thorsett, SE Fomalont, EB Lyne, AG Kramer, M AF Chatterjee, S Vlemmings, WHT Brisken, WF Lazio, TJW Cordes, JM Goss, WM Thorsett, SE Fomalont, EB Lyne, AG Kramer, M TI Getting its kicks: A VLBA parallax for the hyperfast pulsar B1508+55 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; pulsars : individual (B1508+55); stars : kinematics; stars : neutron ID NEUTRON-STAR KICKS; RADIO PULSARS; CYGNUS SUPERBUBBLE; SPACE VELOCITIES; ORIGIN; RADIATION; PROGENITORS; COLLAPSE; MOTIONS; SYSTEMS AB The highest velocity neutron stars establish stringent constraints on natal kicks, asymmetries in supernova core collapse, and the evolution of close binary systems. Here we present the first results of a long-term pulsar astrometry program using the VLBA. We measure a proper motion and parallax for the pulsar B1508+55, leading to model-independent estimates of its distance (2.37(-0.20)(+0.23) kpc) and transverse velocity (1083(-90)(+103) km s(-1)), the highest to velocity directly measured for a neutron star. We trace the pulsar back from its present Galactic latitude of 52 degrees.3 to a birth site in the Galactic plane near the Cyg OB associations, and find that it will inevitably escape the Galaxy. Binary disruption alone is insufficient to impart the required birth velocity, and a natal kick is indicated. A composite scenario including a large kick along with binary disruption can plausibly account for the high velocity. C1 Natl Radio Astron Observ, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. USN, Res Lab, Washington, DC 20375 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Chatterjee, S (reprint author), Natl Radio Astron Observ, 60 Garden St, Cambridge, MA 02138 USA. EM schatterjee@cfa.harvard.edu OI /0000-0002-2700-9916 NR 38 TC 79 Z9 79 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 SEP 1 PY 2005 VL 630 IS 1 BP L61 EP L64 DI 10.1086/491701 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JG UT WOS:000231440000016 ER PT J AU McKinney, JC AF McKinney, JC TI Total and jet Blandford-Znajek power in the presence of an accretion disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : jets; gamma rays : bursts; X-rays : bursts ID GAMMA-RAY BURSTS; MAGNETICALLY DRIVEN ACCRETION; ACTIVE GALACTIC NUCLEI; ROTATING SUPERMASSIVE STAR; BLACK-HOLE MAGNETOSPHERES; ELECTROMAGNETIC EXTRACTION; SUPERLUMINAL MOTION; RELATIVISTIC JETS; RADIO JETS; ENERGY AB Rotating black holes probably power ultrarelativistic jets in gamma-ray bursts, relativistic jets from some active galactic nuclei, and jets from some black hole X-ray binaries. Prior estimates of the power output of a black hole have assumed an infinitely thin disk and a magnetic field based upon a slowly rotating black hole and have not self-consistently determined the geometry or magnitude of the magnetic field for a realistic accretion disk. We provide useful formulae for the total and jet Blandford-Znajek (BZ) power and efficiency as determined selfconsistently from general relativistic magnetohydrodynamic numerical models. Of all jet mechanisms, we suggest that only the BZ mechanism is able to produce an ultrarelativistic jet. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP McKinney, JC (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Mail Stop 51,60 Garden St, Cambridge, MA 02138 USA. EM jmckinney@cfa.harvard.edu NR 77 TC 139 Z9 139 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 SEP 1 PY 2005 VL 630 IS 1 BP L5 EP L8 DI 10.1086/468184 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JG UT WOS:000231440000002 ER PT J AU Zapata, LA Rodriguez, LF Ho, PTP Zhang, QZ Qi, CH Kurtz, SE AF Zapata, LA Rodriguez, LF Ho, PTP Zhang, QZ Qi, CH Kurtz, SE TI A highly collimated, young, and fast CO outflow in OMC-1 south SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (M42,Orion,Orion OMC-1S); ISM : jets and outflows; stars : pre-main-sequence ID BIPOLAR MOLECULAR OUTFLOWS; ORION-NEBULA; TRAPEZIUM CLUSTER; IMAGING SURVEY; STARS; OBJECTS; CLOUD; JET; PROTOSTARS; TELESCOPE AB We present high angular resolution (similar to 1(n)), sensitive CO (2-1) line observations of the region OMC-1S in the Orion Nebula made using the Submillimeter Array. We detect the CO (2-1) high-velocity outflow that was first found by Rodriguez- Franco et al. with the IRAM 30 m telescope. Our observations resolve the outflow, whose velocity-integrated emission has a deconvolved width of ( 390 AU) and a projected length of similar to 48(n) 0(n).89 +/- 0(n).89 ( 21,000 AU) with very high redshifted and blueshifted gas with velocities of about +/- 80 km s(-1). This outflow is among the most collimated (similar to 3 degrees) and youngest outflows (600 yr) that have been reported. The data show that this collimated outflow has been blowing in the same direction during the last 600 years. At high velocities, the CO (2-1) outflow traces an extremely collimated jet, while at lower velocities, the CO emission traces an envelope possibly produced by entrainment of ambient gas. Furthermore, we also detect for the first time a millimeter wavelength continuum source associated with a class I protostar that we suggest could be the possible exciting source for this collimated outflow. However, the bolometric luminosity of this source appears to be far too low to account for the powerful molecular outflow. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zapata, LA (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apdo Postal 3-72, Morelia 58089, Michoacan, Mexico. EM lzapata@astrosmo.unam.mx OI Zhang, Qizhou/0000-0003-2384-6589 NR 43 TC 24 Z9 24 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2005 VL 630 IS 1 BP L85 EP L88 DI 10.1086/491470 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958JG UT WOS:000231440000022 ER PT J AU O'Shea, BW Nagamine, K Springel, V Hernquist, L Norman, ML AF O'Shea, BW Nagamine, K Springel, V Hernquist, L Norman, ML TI Comparing AMR and SPH cosmological simulations. I. Dark matter and adiabatic simulations SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : theory; galaxies : formation; methods : numerical ID SMOOTHED PARTICLE HYDRODYNAMICS; N-BODY SIMULATIONS; RADIATION MAGNETOHYDRODYNAMICS CODE; ADAPTIVE MESH REFINEMENT; 2 SPACE DIMENSIONS; NUMERICAL TECHNIQUES; ASTROPHYSICAL FLOWS; GRAVITY SOLVER; TESTS; ALGORITHMS AB We compare two cosmological hydrodynamic simulation codes in the context of hierarchical galaxy formation: the Lagrangian smoothed particle hydrodynamics (SPH) code GADGET, and the Eulerian adaptive mesh refinement (AMR) code Enzo. Both codes represent dark matter with the N-body method but use different gravity solvers and fundamentally different approaches for baryonic hydrodynamics. The SPH method in GADGET uses a recently developed "entropy conserving'' formulation of SPH, while for the mesh-based Enzo two different formulations of Eulerian hydrodynamics are employed: the piecewise parabolic method (PPM) extended with a dual energy formulation for cosmology, and the artificial viscosity-based scheme used in the magnetohydrodynamics code ZEUS. In this paper we focus on a comparison of cosmological simulations that follow either only dark matter, or also a nonradiative ("adiabatic'') hydrodynamic gaseous component. We perform multiple simulations using both codes with varying spatial and mass resolution with identical initial conditions. The dark matter-only runs agree generally quite well provided Enzo is run with a comparatively fine root grid and a low overdensity threshold for mesh refinement, otherwise the abundance of low-mass halos is suppressed. This can be readily understood as a consequence of the hierarchical particle-mesh algorithm used by Enzo to compute gravitational forces, which tends to deliver lower force resolution than the tree-algorithm of GADGET at early times before any adaptive mesh refinement takes place. At comparable force resolution we find that the latter offers substantially better performance and lower memory consumption than the present gravity solver in Enzo. In simulations that include adiabatic gasdynamics we find general agreement in the distribution functions of temperature, entropy, and density for gas of moderate to high overdensity, as found inside dark matter halos. However, there are also some significant differences in the same quantities for gas of lower overdensity. For example, at z = 3 the fraction of cosmic gas that has temperature log T > 0: 5 is similar to 80% for both Enzo ZEUS and GADGET, while it is 40% - 60% for Enzo PPM. We argue that these discrepancies are due to differences in the shock-capturing abilities of the different methods. In particular, we find that the ZEUS implementation of artificial viscosity in Enzo leads to some unphysical heating at early times in preshock regions. While this is apparently a significantly weaker effect in GADGET, its use of an artificial viscosity technique may also make it prone to some excess generation of entropy that should be absent in Enzo PPM. Overall, the hydrodynamical results for GADGET are bracketed by those for Enzo ZEUS and Enzo PPM but are closer to Enzo ZEUS. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Los Alamos Natl Lab, Los Alamos, NM 87544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP O'Shea, BW (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. EM bwoshea@cosmos.ucsd.edu; knagamin@cfa.harvard.edu; volker@mpa-garching.mpg.de; lars@cfa.harvard.edu; mnorman@cosmos.ucsd.edu NR 49 TC 127 Z9 128 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2005 VL 160 IS 1 BP 1 EP 27 DI 10.1086/432645 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LY UT WOS:000231451000001 ER PT J AU Fish, VL Reid, MJ Argon, AL Zheng, XW AF Fish, VL Reid, MJ Argon, AL Zheng, XW TI Full-polarization observations of OH masers in massive star-forming regions. I. Data SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : magnetic fields; masers; radio lines : ISM; stars : formation ID VLBI SYNTHESIS OBSERVATIONS; ULTRACOMPACT HII-REGIONS; MAGNETIC-FIELD STRUCTURE; HYDROXYL MASERS; PROPER MOTIONS; 4765 MHZ; W3(OH); EMISSION; LINE; RESOLUTION AB We present full-polarization VLBA maps of the ground-state, main-line, (2)Pi(3/2), J = 3/2 OH masers in 18 Galactic massive star-forming regions. This is the first large polarization survey of interstellar hydroxyl masers at VLBI resolution. A total of 184 Zeeman pairs are identified, and the corresponding magnetic field strengths are indicated. We also present spectra of the NH3 emission or absorption in these star-forming regions. Analysis of these data will be presented in a companion paper. C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. RP Fish, VL (reprint author), Natl Radio Astron Observ, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA. EM vfish@nrao.edu; reid@cfa.harvard.edu; aargon@cfa.harvard.edu; xwzheng@nju.edu.cn NR 36 TC 59 Z9 59 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2005 VL 160 IS 1 BP 220 EP 271 DI 10.1086/431669 PG 52 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LY UT WOS:000231451000011 ER PT J AU McShea, WJ Koy, K Clements, T Johnson, A Vongkhamheng, C Aung, M AF McShea, WJ Koy, K Clements, T Johnson, A Vongkhamheng, C Aung, M TI Finding a needle in the haystack: Regional analysis of suitable Eld's deer (Cervus eldi) forest in Southeast Asia SO BIOLOGICAL CONSERVATION LA English DT Article DE cervids; dry dipterocarp forest; landscape ecology; protected areas; suitable forest; northern plains of Cambodia; reintroduction ID CONSERVATION; POPULATIONS; CONTRACTION; DATABASE; ECOLOGY; THAMIN AB For species whose decline preceded the modern era and whose distribution is in the developing world, it is difficult to map suitable habitat across its former range. Eld's deer (Cerrus eldi) is an endangered cervid whose range across Southeast Asia was reduced during the last century to disjoint populations in Myanmar and Cambodia. We used ecological data from the present populations to determine landscape and habitat parameters that would help us predict the occurrence of the species in forests not yet surveyed. The suitable-forest GIs model was created using four readily available datasets for elevation, forest type, canopy closure, and human density. Comparison of the GIs model with 24 verified sightings of Eld's deer during recent large mammal surveys in Cambodil, found 22 sightings (92%) within predicted suitable forest. Use the suitable-forest GIs model to survey a province in southern Lao People's Democratic Republic, located a single. previously unreported population from 9 patches surveyed. In a separate analysis, a logistic regression model to predict Eld's deer habitat in Northern Cambodia found percent tree cover, presence of wetlands, and distance to villages as the best predictors of deer, similar to variables used in the GIs model, with the exception of the importance of wetlands. Using mean annual rainfall to rank suitable-forest patches identified in the GIs model indicated dry dipterocarp forests in Northeastern Cambodia and Northern Myanmar have the highest potential to conserve eld's deer. Examination of the suitable forest GIs map and current protected areas indicated only Cambodia, with 11% suitable forest protected. has placed sufficient dry dipterocarp forest under protected status. Other Southeast Asia countries have not recognized dry dipterocarp forest as a significant ecotype worthy of conservation status. (c) 2005 Elsevier Ltd. All rights reserved. C1 Smithsonian Inst, Wildlife Conservat Soc, Joint Forest Ecol Program, Conservat & Res Ctr, Front Royal, VA 22630 USA. Amer Museum Nat Hist, Ctr Biodivers & Conservat, New York, NY 10024 USA. Wildlife Conservat Soc, Phnom Penh, Cambodia. Wildlife Conservat Soc, Viangchan, Laos. Wildlife Div, Forest Dept, Yangon, Myanmar. RP McShea, WJ (reprint author), Smithsonian Inst, Wildlife Conservat Soc, Joint Forest Ecol Program, Conservat & Res Ctr, Front Royal, VA 22630 USA. EM wmcshea@si.edu NR 62 TC 13 Z9 15 U1 2 U2 9 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD SEP PY 2005 VL 125 IS 1 BP 101 EP 111 DI 10.1016/j.biocon.2005.03.013 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 935WW UT WOS:000229815100009 ER PT J AU Gilbert, GS AF Gilbert, GS TI Nocturnal fungi: Airborne spores in the canopy and understory of a tropical rain forest SO BIOTROPICA LA English DT Article DE Airborne fungi; Australia; canopy; fungal spores; Queensland; tropical rain forest ID VENTURIA-INAEQUALIS; WEATHER VARIABLES; ASCOSPORES; DISCHARGE; MAIZE AB Pathogens and other symbiotic fungi that infect above-ground plant parts commonly disperse as airborne spores. Here we present diel patterns of the density of airborne fungal spores in the canopy and understory of a tropical rain forest. Spores were 52-fold more abundant in the understory than in the canopy. Additionally, spores were 5- to 35-fold more abundant at night than during the day, associated with environmental conditions conducive to germination and plant infection. C1 Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Museum Hist Nat, Los Angeles, CA 90007 USA. 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 16 TC 25 Z9 26 U1 0 U2 5 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 2005 VL 37 IS 3 BP 462 EP 464 DI 10.1111/j.1744-7429.2005.00061.x PG 3 WC Ecology SC Environmental Sciences & Ecology GA 956MR UT WOS:000231304500020 ER PT J AU Philpott, SM Greenberg, R Bichier, P AF Philpott, SM Greenberg, R Bichier, P TI The influence of ants on the foraging behavior of birds in an agroforest SO BIOTROPICA LA English DT Article DE Alchornea latifolia; Azteca instabilis; birds; Chiapas; coffee agroecosystem; exploitative competition; Inga micheliana; Mexico; multiple predator effects ID EURASIAN TREECREEPERS; CERTHIA-FAMILIARIS; FOREST; BIODIVERSITY; PLANTATIONS; COMPETITION; ABUNDANCE AB Ants limit bird foraging success via interference or exploitative competition. We compared bird foraging (number and duration of visits, bird species visiting) on ant (Azteca instabilis)-infested and ant-free tropical trees (Inga micheliana and Alchornea latifolia). Ants did not affect the number of bird visits or the number of species visiting. Ant presence shortened visit duration (overall and for insectivores) only on A. latifolia where ant activity was higher. Ants may thus hinder bird foraging on some tropical trees potentially shaping how predators affect arthropod communities; yet ant effects depend on bird foraging guild and ant activity. C1 Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Philpott, SM (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM philpotts@si.edu RI Philpott, Stacy/F-2330-2011 NR 19 TC 15 Z9 16 U1 2 U2 11 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 2005 VL 37 IS 3 BP 468 EP 471 DI 10.1111/j.1744-7429.2005.00063.x PG 4 WC Ecology SC Environmental Sciences & Ecology GA 956MR UT WOS:000231304500022 ER PT J AU Cairns, SD Bayer, FM AF Cairns, SD Bayer, FM TI A review of the genus Primnoa (Octocorallia : Gorgonacea : Primnoidae), with the description of two new species SO BULLETIN OF MARINE SCIENCE LA English DT Review ID DEEP-SEA; RESEDAEFORMIS; ALASKA; ASSOCIATIONS; CNIDARIA; ANTHOZOA; GROWTH; CORALS; GULF AB The four species and one additional variety of the genus Primnoa are revised, including descriptions and illustrations of all taxa. Two new species are described, Primnoa wingi from the Aleutian Islands and Primnoa notialis from the Subantarctic. Primnoa willeyi Hickson, 1915 is considered to be a variety of Primnoa pacifica Kinoshita, 1907. Primnoa is known to occur in the northern boreal Atlantic and Pacific and Subantarctic South Pacific at depths of 9-1029 m. It is particularly common throughout the Aleutian Islands, where it is often a bycatch of fishery trawling and sometimes made into jewelry. 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 cairns.stephen@nmnh.si.edu NR 62 TC 22 Z9 29 U1 3 U2 8 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD SEP PY 2005 VL 77 IS 2 BP 225 EP 256 PG 32 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 965RT UT WOS:000231968700006 ER PT J AU Eberhard, WG AF Eberhard, WG TI Sexual morphology of male Sepsis cynipsea (Diptera : Sepsidae): lack of support for lock-and-key and sexually antagonistic morphological coevolution hypotheses SO CANADIAN ENTOMOLOGIST LA English DT Article ID FLIES DIPTERA; FUNCTIONAL-MORPHOLOGY; GENITALIC SURSTYLI; MALE ARCHISEPSIS; MATING-BEHAVIOR; FEMALE CHOICE; FRONT LEGS; EVOLUTION; SELECTION; CONFLICT AB Traits that function in male-female sexual interactions tend to diverge rapidly compared with other traits. Several hypotheses attempt to explain this evolutionary pattern. Predictions of two of these hypotheses, lock-and-key and sexually antagonistic morphological co-evolution, were tested by examining how two sets of species-specific male structures fit with female structures during courtship and copulation in the fly Sepsis cynipsea (L., 1758). Contrary to predictions of both hypotheses, neither the species-specific modifications of the male's front legs nor those of his genitalic surstyli were matched by modifications of the female structures with which they meshed (wing bases, 6th abdominal sternite); males damaged small patches of microtrichia on the female's wings with their legs, but the morphology of the female's wings and abdomen showed no sign of the defensive designs expected under antagonistic morphological co-evolution. Data regarding the alternative hypothesis of sexually antagonistic behavioral co-evolution by females in response to male morphology were less conclusive, but this hypothesis failed to explain the sustained, apparently stimulatory rhythmic squeezing by the male genitalia and the lack of female defensive responses to this squeezing. These movements of the male surstyli during copulation suggest that they function to stimulate the female. The wing base of the female has apparent sense organs near the sites contacted by the male, as expected under the alternative hypothesis of traditional female choice to explain rapid divergent evolution. The male's genitalic surstyli were also used in novel precopulatory interactions. A pair of previously undescribed processes at the bases of the surstyli probably grasp and may also rhythmically squeeze the female during copulation. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Excuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. EM archisepsis@biologia.ucr.ac.cr NR 39 TC 16 Z9 16 U1 0 U2 14 PU ENTOMOL SOC CANADA PI OTTAWA PA 393 WINSTON AVE, OTTAWA, ONTARIO K2A 1Y8, CANADA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD SEP-OCT PY 2005 VL 137 IS 5 BP 551 EP 565 PG 15 WC Entomology SC Entomology GA 992XA UT WOS:000233916100006 ER PT J AU von Savigny, C McDade, IC Griffioen, E Haley, CS Sioris, CE Llewellyn, EJ AF von Savigny, C McDade, IC Griffioen, E Haley, CS Sioris, CE Llewellyn, EJ TI Sensitivity studies and first validation of stratospheric ozone profile retrievals from Odin/OSIRIS observations of limb-scattered solar radiation SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID INFRARED IMAGER SYSTEM; ODIN SATELLITE; OPTICAL SPECTROGRAPH; OSIRIS INSTRUMENT; TRANSFER MODEL; O-3 PROFILES; POAM-III; RADIANCE; CLIMATOLOGY; TEMPERATURE AB An error analysis and first validation results are presented for a method of retrieving stratospheric ozone density profiles from spectra of limb-scattered solar radiation, as measured with the OSIRIS instrument on the Odin satellite. The sensitivity study includes geophysical parameters such as ground albedo, stratospheric aerosols, cloud cover, and conditions in the background atmosphere, as well as instrumental parameters such as instrument noise, polarization sensitivity of the spectrograph, and levels of internal and external straylight. The dominating sources of error within the 15-40 km altitude range are found to be stratospheric aerosols, ground albedo, and clouds, with each individual error being generally well below 5%. The total error in this altitude range is estimated to be on the order of 10% for an individual retrieved profile. A comparison of colocated measurements from OSIRIS and the POAM III occultation instrument during August of 2001 at northern-hemisphere mid-latitudes shows agreement to within about 5% between 15 and 35 km. The ozone densities from OSIRIS are found to be systematically lower than those from POAM III. C1 Univ Bremen, Inst Environm Phys, IUP, D-28359 Bremen, Germany. Univ Toronto, CRESS, N York, ON M3J 1P3, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Saskatchewan, Dept Phys & Phys Engn, Saskatoon, SK S7N 5E2, Canada. RP von Savigny, C (reprint author), Univ Bremen, Inst Environm Phys, IUP, Otto Hahn Allee 1, D-28359 Bremen, Germany. EM csavigny@iup.physik.uni-bremen.de RI von Savigny, Christian/B-3910-2014; OI Sioris, Christopher/0000-0003-1168-8755 NR 32 TC 13 Z9 13 U1 0 U2 1 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD SEP PY 2005 VL 83 IS 9 BP 957 EP 972 DI 10.1139/P05-041 PG 16 WC Physics, Multidisciplinary SC Physics GA 964NP UT WOS:000231888100007 ER PT J AU Towe, KM AF Towe, KM TI About the geochemical origin of life SO ELEMENTS LA English DT Letter ID EVOLUTION; IRON C1 Smithsonian Inst, Dept Paleobiol, Tennille, GA 31089 USA. RP Towe, KM (reprint author), Smithsonian Inst, Dept Paleobiol, 230 W Adams St, Tennille, GA 31089 USA. NR 10 TC 1 Z9 1 U1 0 U2 1 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 1811-5209 J9 ELEMENTS JI Elements PD SEP PY 2005 VL 1 IS 4 BP 189 EP 189 PG 1 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 010DG UT WOS:000235166500002 ER PT J AU Ramos, M Coddington, JA Christenson, TE Irschick, DJ AF Ramos, M Coddington, JA Christenson, TE Irschick, DJ TI Have male and female genitalia coevolved? A phylogenetic analysis of genitalic morphology and sexual size dimorphism in web-building spiders (Araneae : Araneoidea) SO EVOLUTION LA English DT Article DE genitalic evolution; Orbiculariae; scaling; sexual size dimorphism; spiders ID BODY-SIZE; CONFIDENCE-INTERVALS; SPERM-STORAGE; EVOLUTION; SELECTION; ALLOMETRY; INSECTS; LIZARDS; PERFORMANCE; FREQUENCY AB Sexual size dimorphism (SSD) can strongly influence the evolution of reproductive strategies and life history. If SSD is extreme, and other characters (e.g., genitalic size) also increase with size, then functional conflicts may arise between the sexes. Spiders offer an excellent opportunity to investigate this issue because of their wide range of SSD. By using modern phylogenetic methods with 16 species of orb-weaving spiders, we provide strong evidence for the "positive genitalic divergence" model, implying that sexual genitalic dimorphism (SGD) increases as SSD increases. This pattern is supported by an evolutionary mismatch between the absolute sizes of male and female genitalia across species. Indeed, our findings reveal a dramatic reversal from male genitalia that are up to 87xlarger than female genitalia in size-monomorphic species to female genitalia that are up to 2.8x larger in extremely size-dimorphic species. We infer that divergence in SGD could limit SSD both in spiders, and potentially in other taxa as well. Further, male and female body size, as well as male and female genitalia size, are decoupled evolutionarily. Finally, we show a negative scaling (hypoallometry) of male and female genitalic morphology within sexes. Evolutionary forces specific to each sex, such as larger female size (increased fecundity) or smaller male size (enhanced mate-searching ability), may be balanced by stabilizing selection on relative genitatic size. C1 Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Tulane Univ, Dept Psychol, New Orleans, LA 70118 USA. RP Irschick, DJ (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, Dinwiddie Hall, New Orleans, LA 70118 USA. EM irschick@tulane.edu NR 61 TC 26 Z9 27 U1 0 U2 8 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD SEP PY 2005 VL 59 IS 9 BP 1989 EP 1999 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 969UB UT WOS:000232259300013 PM 16261736 ER PT J AU Sullivan, MC Cowen, RK Steves, BP AF Sullivan, MC Cowen, RK Steves, BP TI Evidence for atmosphere-ocean forcing of yellowtail flounder (Limanda ferruginea) recruitment in the Middle Atlantic Bight SO FISHERIES OCEANOGRAPHY LA English DT Article DE cold pool; Limanda ferruginea; Middle Atlantic Bight; North Atlantic Oscillation; recruitment ID LARVAL FISH ASSEMBLAGES; EASTERN UNITED-STATES; CONTINENTAL-SHELF; NORTH-ATLANTIC; MARINE FISH; ENVIRONMENTAL-FACTORS; CLIMATE VARIABILITY; GEORGES BANK; NEW-YORK; OSCILLATION AB We investigated the relationship between large-scale climate variability (the North Atlantic Oscillation, NAO), continental shelf hydrography, and year-class strength of yellowtail flounder (Limanda ferruginea) in the Middle Atlantic Bight. Using long-term environmental time series (1963-98), dominant winter NAO phase in the northeast region of the United States was correlated with local air temperature records from Block Island, Rhode Island (December-March). Air temperature also influenced the characteristics of a pool of remnant winter cold water on the continental shelf, such that negative NAO winters produced a colder-than-average summer cold pool, and vice versa. Smoothed data sets of L. ferruginea recruitment over the 36-yr period (using Southern New England VPA and hindcast data) were highly correlated with the NAO and air temperature, highlighting the influence of multi-year variability. Although less robust, the relationship with the NAO remained significant after removing equal-but-opposite long-term linear trends from the series. Surprisingly, recruitment and cold pool bottom temperature were only marginally correlated. Data from independent 2-m beam trawl and submersible sampling in the region (1994, 1996-2000) indicated a strong relationship between the abundance of recent settlers and cold pool temperature; however, this pattern was often modified by subsequent changes in cold pool stratification (fall overturn). These results underscore the dynamic role thermal habitats play in the lives of early stage benthic fishes. For yellowtail flounder, the generation of recruitment variability represents one endpoint of a complex interaction between large-scale phenomena (climate) and more localized, event-scale features (cold pool). C1 Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. Smithsonian Environm Res Ctr, Marine Invas Res Lab, Edgewater, MD 21037 USA. RP Sullivan, MC (reprint author), Rutgers Marine Field Stn, 132 Great Bay Blvd, Tuckerton, NJ 08087 USA. EM sullivan@marine.rutgers.edu NR 55 TC 21 Z9 21 U1 3 U2 6 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1054-6006 J9 FISH OCEANOGR JI Fish Oceanogr. PD SEP PY 2005 VL 14 IS 5 BP 386 EP 399 DI 10.1111/j.1365-2419.2005.00343.x PG 14 WC Fisheries; Oceanography SC Fisheries; Oceanography GA 964TN UT WOS:000231903500005 ER PT J AU Aronson, RB Macintyre, IG Precht, WF AF Aronson, RB Macintyre, IG Precht, WF TI Event preservation in lagoonal reef systems SO GEOLOGY LA English DT Article DE Caribbean; coral reef; event layer; hurricane; preservation potential; taphonomy ID CARIBBEAN CORAL-REEFS; OF-THORNS STARFISH; LONG-TERM DECLINE; COMMUNITY STRUCTURE; RECURRING OUTBREAKS; GEOLOGICAL EVIDENCE; DEATH ASSEMBLAGES; VIRGIN-ISLANDS; CLIMATE-CHANGE; PHASE-SHIFTS AB Paleontological data suggest that coral populations in the Caribbean were consistently healthy for the past 2-3 k.y. Beginning in the 1980s, however, disease outbreaks, bleaching episodes, hurricanes, and other perturbations caused catastrophic coral mortality and regional turnover. An alternative hypothesis, based on historical sources, posits that coral populations were already declining more than a century ago. These hypotheses can be distinguished only if turnover events are reliably preserved in the Holocene record of coral reefs. Push-pores extracted from uncemented lagoonal reefs in Belize showed that a direct hit by Hurricane Iris in 2001 did not disrupt the signature of the recent turnover event, which entered the subfossil record essentially intact. Cores from lagoonal systems in several areas of the Caribbean do not support the hypothesis that corals declined before the 1980s. C1 Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. Univ S Alabama, Dept Marine Sci, Mobile, AL 36688 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. PBS&J, Ecol Sci Div, Miami, FL 33172 USA. RP Aronson, RB (reprint author), Dauphin Isl Sea Lab, 101 Bienville Blvd, Dauphin Isl, AL 36528 USA. EM raronson@disl.org RI kohki, sowa/D-2955-2011 NR 34 TC 11 Z9 13 U1 0 U2 5 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD SEP PY 2005 VL 33 IS 9 BP 717 EP 720 DI 10.1130/G21640.1 PG 4 WC Geology SC Geology GA 960JF UT WOS:000231585800007 ER PT J AU Castro, RMC Casatti, L Santos, HE Vari, RP Melo, ALA Martins, LSE Abreu, TX Benine, RC Gibran, FZ Ribeiro, AC Bockmann, FA Carvalho, M Pelicao, GZP Ferreira, KM Stopiglia, R Akama, A AF Castro, RMC Casatti, L Santos, HE Vari, RP Melo, ALA Martins, LSE Abreu, TX Benine, RC Gibran, FZ Ribeiro, AC Bockmann, FA Carvalho, M Pelicao, GZP Ferreira, KM Stopiglia, R Akama, A TI Structure and composition of the stream ichthyofauna of four tributary rivers of the upper Rio Parana basin, Brazil SO ICHTHYOLOGICAL EXPLORATION OF FRESHWATERS LA English DT Article ID COMMUNITY; STATE AB The ichthyofauna of 24 stretches of streams, all of 100 m length and of fifth or lower order and most of second and third order, were sampled along four left bank tributaries (Rio do Peixe, Rio Aguapei, Rio Sao Jose dos Dourados, lower Rio Tiete of the main channel of the Rio Parana in the state of Sao Paulo, southeastern Brazil. Sampling of the fish fauna at each of the six sites in the four basins incorporated a standardized fish collecting methodology and a standardized documentation of environmental data serving as the basis for a comparative analysis of the collecting locations. The 8,189 fish specimens collected represented six orders, 18 families, 42 genera, and 56 species, with a total biomass of 28.8 kg. Approximately 52% of the collected species were characiforms, 28% siluriforms, 9% gymnotiforms, 5% cyprinodontiforms, 4% perciforms, and 2% synbranchiforms. The most abundant of the species were the characiforms Astyanax altiparanae (15% of total) and Knodus moenkhausii (12% of total). The two species with the largest overall biomasses were A. altiparanae (34% of total biomass) and the siluriform Hypostomus sp. (8% of total biomass). Analysis of the trophic structure of the studied ichthyofauna indicated that the 10 numerically dominant species across the 24 sampled streams can be grouped into five guilds that are in decreasing order of numerical importance: omnivores, insectivores, insectivores/invertivores, periphytivores, and algivores. Species richness in the sampled stream stretches varied from six to 20 species with an average richness of 14. The species richness estimated by extrapolation for all 24 sampled stream stretches was 67 species. The Characidae are predominant among the collected specimens with approximately 50% of both individuals and biomass, a fact hypothesized to be a function of several attributes typical of the family. Six of the 56 collected species were new to science and six other species are of indefinite taxonomic status and require further analysis in order to determine their identity. C1 Univ Sao Paulo, FFCLRP, Dept Biol, LIRP, BR-14040901 Ribeirao Preto, Brazil. Univ Estadual Paulista, IBILCE, Dept Zool & Bot, BR-15054000 Sao Jose Do Rio Preto, SP, Brazil. Natl Museum Nat Hist, Div Fishes, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. Univ Sao Paulo, Museu Zool, BR-04299970 Sao Paulo, Brazil. RP Castro, RMC (reprint author), Univ Sao Paulo, FFCLRP, Dept Biol, LIRP, Av Bandeirantes 3900, BR-14040901 Ribeirao Preto, Brazil. EM rmcastro@ffclrp.usp.br; lcasatti@ibilce.unesp.br; varir@si.edu; aakama@ib.usp.br RI Carvalho, Murilo/B-7950-2012; Gibran, Fernando/G-5844-2012; Gibran, Fernando/I-9377-2012; Ribeiro, Alexandre/K-6599-2012; Benine, Ricardo/B-2354-2013; Casatti, Lilian/C-4749-2012; Ferreira, Katiane/I-1486-2015; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 OI Carvalho, Murilo/0000-0001-6881-5271; Gibran, Fernando/0000-0002-2812-8976; NR 50 TC 17 Z9 24 U1 1 U2 3 PU VERLAG DR FRIEDRICH PFEIL PI MUNICH PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY SN 0936-9902 J9 ICHTHYOL EXPLOR FRES JI Ichthyol. Explor. Freshw. PD SEP PY 2005 VL 16 IS 3 BP 193 EP 214 PG 22 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 962IR UT WOS:000231725300001 ER PT J AU Collins, AG Cartwright, P McFadden, CS Schierwater, B AF Collins, AG Cartwright, P McFadden, CS Schierwater, B TI Phylogenetic context and basal metazoan model systems SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Model Systems for the Basal Metazoans - Cnidarians, Ctenophores and Placozoans CY JAN 05-09, 2004 CL New Orleans, LA ID JELLYFISH PODOCORYNE-CARNEA; CLASS-LEVEL RELATIONSHIPS; RNA GENE-SEQUENCES; 18S RDNA SEQUENCES; PROTEIN-KINASE-C; RIBOSOMAL-RNA; HOMEOBOX GENE; NEMATOSTELLA-VECTENSIS; PHYLUM CNIDARIA; SEA-ANEMONE AB In comparative studies using model organisms, extant taxa are often referred to as basal. The term suggests that such taxa are descendants of lineages that diverged early in the history of some larger taxon. By this usage, the basal metazoans comprise just four phyla (Placozoa, Porifera, Cnidaria, and Cten-ophora) and the large clade Bilateria. We advise against this practice because basal refers to a region at the base or root of a phylogenetic tree. Thus, referring to an extant taxon or species as basal, or as more basal than another, can be misleading. While much progress has been made toward understanding some of the phylogenetic relationships within these groups, the relationships among them are still largely not known with certainty. Thus, sound inferences from comparative studies of model organisms demand continued illumination of phylogeny. Hypotheses about the mechanisms underlying metazoan evolution can be drawn from the study of model organisms in Cnidaria, Ctenophora, Placozoa, and Porifera, but it is clear that these model organisms are likely to be derived in many respects. Therefore, testing these hypotheses requires the study of yet additional model organisms. The most effective tests are those that investigate model organisms with phylogenetic positions among two sister groups comprising a larger clade of interest. C1 ITZ, D-30559 Hannover, Germany. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Harvey Mudd Coll, Dept Biol, Claremont, CA 91711 USA. RP Collins, AG (reprint author), Natl Museum Nat Hist, NMFS, Smithsonian Inst, POB 37012,MRC-153, Washington, DC 20013 USA. EM CollinsA@SI.edu RI Collins, Allen/A-7944-2008 OI Collins, Allen/0000-0002-3664-9691 NR 120 TC 30 Z9 31 U1 1 U2 7 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD SEP PY 2005 VL 45 IS 4 BP 585 EP 594 DI 10.1093/icb/45.4.585 PG 10 WC Zoology SC Zoology GA 967KZ UT WOS:000232091400002 PM 21676805 ER PT J AU Melendez-Ackerman, EJ Speranza, P Kress, WJ Rohena, L Toledo, E Cortes, C Treece, D Gitzendanner, M Soltis, P Soltis, D AF Melendez-Ackerman, EJ Speranza, P Kress, WJ Rohena, L Toledo, E Cortes, C Treece, D Gitzendanner, M Soltis, P Soltis, D TI Microevolutionary processes inferred from AFLP and morphological variation in Heliconia bihai (Heliconiaceae) SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE selection; genetic drift; AFLP; Heliconia; bract color; polymorphisms ID POPULATION GENETIC-STRUCTURE; LENGTH POLYMORPHISM MARKERS; PURPLE-THROATED CARIBS; FLOWER COLOR; SUBDIVIDED POPULATIONS; IPOMOPSIS-AGGREGATA; NATURAL-POPULATIONS; REGRESSION APPROACH; EPIPHYTIC ORCHID; GOLDEN TORCH AB Heliconia bihai is a highly polymorphic species. Populations of the species are distributed throughout the Lesser Antilles and northern South America; the most obvious sign of polymorphism is manifested through differences in bract color. This variation has been attributed to pollinator-mediated selection, but other processes are also plausible. To test the potential contribution of drift in the evolution of phenotypic variation in this system, we examined the distribution of morphological and genetic variation within and between populations of H. bihai in the Caribbean islands of St. Vincent and St. Lucia. Morphological characterization was limited to flower and inflorescence characteristics, including bract color. AFLPs were used to investigate levels of genetic diversity within and between populations. Genetic similarity among individuals was equivalent to that expected for conspecific individuals. Levels of AFLP and population subdivision were high and were comparable to those of outcrossing species in one island, but they were low and comparable with selfing or clonal species in the other, indicating that genetic variation between islands may be under different evolutionary regimes. There was a significant geographical structure in morphological variation, but this was considerably less pronounced than that found at the genetic level except for bract color patterns, which were different for different islands. We found no correlation between genetic similarity and geographic distance or between genetic similarity and morphological similarity. Observed patterns of genetic and morphological variation in H. bihai suggest that genetic drift is likely to have had a minor role in their development. Instead, these patterns are consistent with phenomena such as selection, inbreeding, and habitat fragmentation that may be operating independently at different spatial scales. C1 Univ Puerto Rico Rio Piedras, Inst Trop Ecosyst Studies, San Juan, PR 00931 USA. Univ Puerto Rico Rio Piedras, Ctr Appl Trop Ecol & Conservat, Ctr Res Excellence Sci & Technol, San Juan, PR 00931 USA. Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. Oberlin Coll, Ctr Sci, Oberlin, OH 44074 USA. Univ Florida, Dept Bot, Gainesville, FL 32611 USA. RP Melendez-Ackerman, EJ (reprint author), Univ Puerto Rico Rio Piedras, Inst Trop Ecosyst Studies, POB 23341, San Juan, PR 00931 USA. EM elmelend@upracd.upr.clu.edu OI Speranza, Pablo /0000-0003-3457-0151 NR 91 TC 10 Z9 10 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD SEP PY 2005 VL 166 IS 5 BP 781 EP 794 PG 14 WC Plant Sciences SC Plant Sciences GA 953WS UT WOS:000231112900009 ER PT J AU Looy, CV Collinson, ME Cittert, JHAV Visscher, H Brain, APR AF Looy, CV Collinson, ME Cittert, JHAV Visscher, H Brain, APR TI The ultrastructure and botanical affinity of end-Permian spore tetrads SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Permian; tetrads; spores; ultrastructure; lycopsids ID HETEROSPOROUS LYCOPHYTES; MEGASPORE DEVELOPMENT; SELAGINELLA; LYCOPSIDA; MICROSPORES; PLEUROMEIA; ORIGIN; NOV AB End-Permian palynological assemblages worldwide are characterized by large numbers of unseparated tetrads of lycopsid microspores and occasional megaspore tetrads. These spores are assignable to the form genera Densoisporites, Lundbladispora, Uvaesporites, and Otynisporites. Transmission electron microscopy analysis of preserved sporoderm ultrastructure demonstrates that individual spores are juxtaposed or connected to each other by interlocking of the paraexospores at either the interradial contact areas or equatorial regions. The wall organization of Densoisporites, Lundbladispora, and Otynisporites confirms an isoetalean ( Pleuromeiaceae) affinity. The Uvaesporites wall structure is far more complex than so far recognized in extant Selaginellales and extant and fossil Isoetales. Uvaesporites might be related to a distinct lycopsid lineage, with characteristics of rhizomorphic lycopsids and the Selaginalles. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ London Royal Holloway & Bedford New Coll, Dept Geol, Egham TW20 0EX, Surrey, England. Univ Utrecht, Palaeobot & Palynol Lab, NL-3584 CD Utrecht, Netherlands. Natl Museum Nat Hist, Dept Paleontol, NL-2300 RA Leiden, Netherlands. Kings Coll London, Ctr Ultrastruct Imaging, London SE1 9UL, England. RP Looy, CV (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM looyc@si.edu NR 99 TC 19 Z9 20 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD SEP PY 2005 VL 166 IS 5 BP 875 EP 887 DI 10.1086/431802 PG 13 WC Plant Sciences SC Plant Sciences GA 953WS UT WOS:000231112900015 ER PT J AU Gingerich, O AF Gingerich, O TI Texts for the assimilation of the Copernican theory. SO ISIS LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD SEP PY 2005 VL 96 IS 3 BP 427 EP 427 DI 10.1086/498767 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 974ET UT WOS:000232574800016 ER PT J AU McGrath, JM Sims, JT Maguire, RO Saylor, WW Angel, CR Turner, BL AF McGrath, JM Sims, JT Maguire, RO Saylor, WW Angel, CR Turner, BL TI Broiler diet modification and litter storage: Impacts on phosphorus in litters, soils, and runoff SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article ID WATER-SOLUBLE PHOSPHORUS; PHYTASE SUPPLEMENTATION; MICROBIAL PHYTASE; ANIMAL MANURES; POULTRY LITTER; CORN; MANAGEMENT; PHOSPHATE; EXCRETION; SPECTROSCOPY AB Modifying broiler diets to mitigate water quality concerns linked to excess phosphorus (P) in regions of intensive broiler production has recently increased. Our goals were to evaluate the effects of dietary modification, using phytase and reduced non-phytate phosphorus (NPP) supplementation, on P speciation in broiler litters, changes in litter P forms during long-term storage, and subsequent impacts of diets on P in runoff from litter-amended soils. Four diets containing two levels of NPP with and without phytase were fed to broilers in a three-flock floor pen study. After removal of the third flock, litters were stored for 440 d at their initial moisture content (MC; 24%) and at a MC of 40%. Litter P fractions and orthophosphate and phytate P concentrations were determined before and after storage. After storage, litters were incorporated with a sandy and silt loam and simulated rainfall was applied. Phytase and reduced dietary NPP significantly reduced litter total P. Reducing dietary NPP decreased water-extractable inorganic phosphorus (IP) and the addition of dietary phytase reduced NaOH- and HCl-extractable organic P in litter, which correlated well with orthophosphate and phytic acid measured by P-31 nuclear magnetic resonance (NMR), respectively. Although dry storage caused little change in P speciation, wet storage increased concentrations of water-soluble IP, which increased reactive P in runoff from litter-amended soils. Therefore, diet modification with phytase and reduced NPP could be effective in reducing P additions on a watershed scale. Moreover, efforts to minimize litter MC during storage may reduce the potential for dissolved P losses in runoff. C1 Virginia Polytech Inst & State Univ, Dept Crop & Soil Environm Sci, Blacksburg, VA 24061 USA. Univ Delaware, Dept Plant & Soil Sci, Newark, DE 19716 USA. Univ Delaware, Dept Anim & Food Sci, Newark, DE 19716 USA. N Carolina State Univ, Dept Soil Sci, Raleigh, NC 27695 USA. Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP McGrath, JM (reprint author), Virginia Polytech Inst & State Univ, Dept Crop & Soil Environm Sci, Blacksburg, VA 24061 USA. EM jmcgrath@jhu.edu RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; McGrath, Joshua/0000-0002-1212-8795 NR 56 TC 48 Z9 48 U1 1 U2 15 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 USA SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD SEP-OCT PY 2005 VL 34 IS 5 BP 1896 EP 1909 DI 10.2134/jeq2004.0413 PG 14 WC Environmental Sciences SC Environmental Sciences & Ecology GA 968PK UT WOS:000232174300044 PM 16151241 ER PT J AU Turner, BL Newman, S AF Turner, BL Newman, S TI Phosphorus cycling in wetland soils: The importance of phosphate diesters SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article ID P-31 NMR-SPECTROSCOPY; ORGANIC PHOSPHORUS; NORTHERN EVERGLADES; NUTRIENT ACCUMULATION; INOSITOL PHOSPHATES; FLORIDA EVERGLADES; EXTRACTION; FORMS; MINERALIZATION; IDENTIFICATION AB Productivity in P limited peatlands is regulated in part by the turnover of organic phosphates, which is influenced by the chemical nature of the compounds involved. We used solution P-31 nuclear magnetic resonance (NMR) spectroscopy to quantify organic and inorganic phosphates in benthic floc (a mixture of plant detritus and algae) and underlying soil from sites along P gradients in hard water and soft water areas of the northern Florida Everglades, USA. Phosphorus-enriched sites were dominated by cattail (Typha spp.), while unenriched sites included sawgrass (Cladium jamaicense Crantz) ridges and open-water sloughs. Phosphorus extracted in a solution containing 0.25 M NaOH and 50 mM EDTA (ethylenediaminetetraaeetate) included phosphate, phosphate monoesters, DNA, and pyrophosphate. Signals from phosphate monoesters were consistent with those from alkaline hydrolysis products of RNA and phospholipids formed during extraction and analysis, whereas phytic acid (myoinositol hexakisphosphate), the most abundant organic phosphate in most soils, was not detected. Phosphorus composition was similar among sites, although neither DNA nor pyrophosphate were detected in extracts of benthic floc from a calcareous slough. DNA was a greater proportion of the P extracted from soil compared to benthic floc, while the opposite was true for pyrophosphate. Research on the cycling of organic phosphates in wetlands focuses conventionally on the turnover of phosphate monoesters, but our results suggest strongly that greater emphasis should be given to understanding the role of phosphate diesters and phosphodiesterase activity. C1 Smithsonian Trop Res Inst, Balboa 03092, Ancon, Panama. S Florida Water Management Dist, Everglades Div, W Palm Beach, FL 33406 USA. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843, Balboa 03092, Ancon, Panama. EM turnerbl@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 NR 41 TC 67 Z9 70 U1 7 U2 47 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 USA SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD SEP-OCT PY 2005 VL 34 IS 5 BP 1921 EP 1929 DI 10.2134/jeq2005.0060 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA 968PK UT WOS:000232174300046 PM 16151243 ER PT J AU Suarez, RK Darveau, CA Welch, KC O'Brien, DM Roubik, DW Hochachka, PW AF Suarez, RK Darveau, CA Welch, KC O'Brien, DM Roubik, DW Hochachka, PW TI Energy metabolism in orchid bee flight muscles: carbohydrate fuels all SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE respiratory quotient; hovering flight; Euglossine bee; enzymes; glycolysis; flux; carbohydrate ID HONEYBEES APIS-MELLIFERA; PYRUVATE-CARBOXYLASE; FLYING HONEYBEES; INSECT FLIGHT; RATES; INVERTEBRATES; VERTEBRATES; CAPACITIES; CARNICA; PROLINE AB The widely accepted idea that bees fuel flight through the oxidation of carbohydrate is based on studies of only a few species. We tested this hypothesis as part of our research program to investigate the size-dependence of flight energetics in Panamanian orchid bees. We succeeded in measuring rates Of O-2 consumption and CO2 production in vivo during hovering flight, as well as maximal activities (V-max values) in vitro of key enzymes in flight muscle energy metabolism in nine species belonging to four genera. Respiratory quotients (ratios of rates of CO2 production to O-2 consumption) in all nine species are close to 1.0. This indicates that carbohydrate is the main fuel used for flight. Trehalase, glycogen phosphorylase and hexokinase activities are sufficient to account for the glycolytic flux rates estimated from rates Of CO2 production. High activities of other glycolytic enzymes, as well as high activities of mitochondrial oxidative enzymes, are consistent with the estimated rates of carbohydrate-fueled oxidative metabolism. In contrast, hydroxyacylCoA dehydrogenase, an enzyme involved in fatty acid oxidation, was not detectable in any species. Thoracic homogenates displayed ADP-stimulated oxidition of pyruvate + proline, but did not oxidize palmitoyl-L-carnitine + proline as substrates. A metabolic map, based on data reported herein and information from the literature, is presented. The evidence available supports the hypothesis that carbohydrate serves as the main fuel for flight in bees. C1 Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Univ Alaska, Dept Biol & Wildlife, Fairbanks, AK 99775 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Suarez, RK (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM suarez@lifesci.ucsb.edu RI O'Brien, Diane/B-2919-2010; Welch, Kenneth/F-1276-2011 OI O'Brien, Diane/0000-0001-5807-9661; Welch, Kenneth/0000-0002-3283-6510 NR 31 TC 52 Z9 54 U1 2 U2 32 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 SEP PY 2005 VL 208 IS 18 BP 3573 EP 3579 DI 10.1242/jeb.01775 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 973TZ UT WOS:000232546800018 PM 16155228 ER PT J AU Darveau, CA Hochachka, PW Welch, KC Roubik, DW Suarez, RK AF Darveau, CA Hochachka, PW Welch, KC Roubik, DW Suarez, RK TI Allometric scaling of flight energetics in Panamanian orchid bees: a comparative phylogenetic approach SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE metabolic rate; evolution; allometry; wingbeat frequency; wing loading; phylogenetically independent contrasts; orchid bee ID EUGLOSSINI; APIDAE; HYMENOPTERA; PERFORMANCE; METABOLISM; MORPHOLOGY; FREQUENCY; BIOLOGY; DNA AB The relationship between body size and flight energetics was studied in the clade of tropical orchid bees, in order to investigate energy metabolism and evolution. Body mass, which varied from 47 to 1065 mg, was found to strongly affect hovering flight mass-specific metabolic rates, which ranged from 114 ml CO2 h(-1) g(-1) in small species to 37 ml CO2 h(-1) g(-1) in large species. Similar variation of wingbeat frequency in hovering flight occurred among small to large species, and ranged from 250 to 86 Hz. The direct relationship between such traits was studied by the comparative method of phylogenetically independent contrasts (PIC), using a new molecular phylogeny generated from the cytochrome b gene partial sequences. C1 Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Darveau, CA (reprint author), Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. EM darveau@zoology.ubc.ca RI Welch, Kenneth/F-1276-2011 OI Welch, Kenneth/0000-0002-3283-6510 NR 37 TC 37 Z9 38 U1 0 U2 17 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 SEP PY 2005 VL 208 IS 18 BP 3581 EP 3591 DI 10.1242/jeb.01776 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 973TZ UT WOS:000232546800019 PM 16155229 ER PT J AU Darveau, CA Hochachka, PW Roubik, DW Suarez, RK AF Darveau, CA Hochachka, PW Roubik, DW Suarez, RK TI Allometric scaling of flight energetics in orchid bees: evolution of flux capacities and flux rates SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE enzyme activity; metabolic rate; evolution; allometry; insect flight; orchid bee ID RESTING METABOLIC-RATE; ENERGY-METABOLISM; FLYING HONEYBEES; GLYCOLYTIC-ENZYMES; MUSCLE; HEXOKINASE; PERFORMANCE; TRANSPORT; OXYGEN; PHOSPHORYLATION AB The evolution of metabolic pathways involved in energy production was studied in the flight muscles of 28 species of orchid bees. Previous work revealed that wingbeat frequencies and mass-specific metabolic rates decline in parallel by threefold as body mass increases interspecifically over a 20-fold range. We investigated the correlated evolution of metabolic rates during hovering flight and the flux capacities, i.e. V(max) values, of flight muscle enzymes involved in substrate catabolism, the Krebs cycle and the electron transport chain. V(max) at the hexokinase (HK) step scales allometrically with an exponent almost identical to those obtained for wingbeat frequency and mass-specific metabolic rate. Analysis of this relationship using phylogenetically independent contrasts supports the hypothesis of correlated evolution between HK activity and mass-specific metabolic rate. Although other enzymes scale allometrically with respect to body mass, e.g. trehalase, glycogen phosphorylase and citrate synthase, no other enzyme activities were correlated with metabolic rate after controlling for phylogenetic relatedness. Pathway flux rates were used with enzyme V(max) values to estimate fractional velocities (fraction of V(max) at which enzymes operate) for various reactions to gain insights into enzyme function and how this varies with body mass. Fractional velocity is highly conserved across species at the HK step, but varied at all other steps examined. These results are discussed in the context of the regulation and evolution of pathways of energy metabolism. C1 Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Smithsonian Trop Res Inst, Balboa, Panama. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP Darveau, CA (reprint author), Univ British Columbia, Dept Zool, 6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada. EM darveau@zoology.ubc.ca NR 51 TC 22 Z9 24 U1 1 U2 16 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 SEP PY 2005 VL 208 IS 18 BP 3593 EP 3602 DI 10.1242/jeb.01777 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 973TZ UT WOS:000232546800020 PM 16155230 ER PT J AU Suarez, RK Darveau, CA Hochachka, PW AF Suarez, RK Darveau, CA Hochachka, PW TI Roles of hierarchical and metabolic regulation in the allometric scaling of metabolism in Panamanian orchid bees SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE allometry; metabolism; glycolysis; hovering flight; metabolic scaling; orchid bee ID FLIGHT ENERGETICS; ENERGY-METABOLISM; FLYING HONEYBEES; FLUX CAPACITIES; BODY-SIZE; MITOCHONDRIAL; DESIGN; HEART; RATES; ISOMERASE AB Assessment of the relative importance of variation in enzyme concentration [E] and metabolic regulation in accounting for interspecific variation in metabolic rates is an unrealized area of research. Towards this end, we used metabolic flux rates during hovering and enzymatic flux capacities (V(max) values, equal to [E] x k(cat), where k(cat) is catalytic efficiency) in flight muscles measured in vitro from 14 orchid bee species ranging in body mass from 47 to 1065 mg. Previous studies revealed that, across orchid bee species, wingbeat frequencies and metabolic rates decline in parallel with increasing body mass. V(max) values at some enzymatic steps in pathways of energy metabolism decline with increasing mass while, at most other steps, Vmax values are mass-independent. We quantified the relative importance of 'hierarchical regulation' (alteration in V(max), indicative of alteration in [E]) and 'metabolic regulation' (resulting from variation in substrate, product or modulator concentrations) in accounting for interspecific variation in flux across species. In addition, we applied the method of phylogenetically independent contrasts to remove the potentially confounding effects of phylogenetic relationships among species. In the evolution of orchid bees, hierarchical regulation completely accounts for allometric variation in flux rates at the hexokinase step while, at other reactions, variation in flux is completely accounted for by metabolic regulation. The predominant role played by metabolic regulation is examined at the phosphoglucoisomerase step using the Haldane relationship. We find that extremely small variation in the concentration ratio of [product]/[substrate] is enough to cause the observed interspecific variation in net flux at this reaction in glycolysis. C1 Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Smithsonian Trop Res Inst, Barro Colorado Isl, Panama. RP Suarez, RK (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM suarez@lifesci.ucsb.edu NR 32 TC 18 Z9 18 U1 0 U2 9 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD SEP PY 2005 VL 208 IS 18 BP 3603 EP 3607 DI 10.1242/jeb.01778 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 973TZ UT WOS:000232546800021 PM 16155231 ER PT J AU Pojeta, J Taylor, JE Darrough, G AF Pojeta, J Taylor, JE Darrough, G TI Matthevia (Polyplacophora) invades the Ordovician: The first reported post-Cambrian occurrence SO JOURNAL OF PALEONTOLOGY LA English DT Article C1 Smithsonian Inst, US Geol Survey, Washington, DC 20560 USA. Smithsonian Inst, Museum Nat Hist, Washington, DC 20560 USA. Indiana Univ Penn, Geosci Dept, Indiana, PA 15705 USA. RP Pojeta, J (reprint author), Smithsonian Inst, US Geol Survey, MRC 137, Washington, DC 20560 USA. EM pojetaj@si.edu NR 32 TC 3 Z9 4 U1 0 U2 1 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD SEP PY 2005 VL 79 IS 5 BP 1021 EP 1027 DI 10.1666/0022-3360(2005)079[1021:MPITOT]2.0.CO;2 PG 7 WC Paleontology SC Paleontology GA 959KV UT WOS:000231517500019 ER PT J AU Tamura, Y Tani, K Ishizuka, O Chang, Q Shukuno, H Fiske, RS AF Tamura, Y Tani, K Ishizuka, O Chang, Q Shukuno, H Fiske, RS TI Are arc basalts dry, wet, or both? Evidence from the Sumisu caldera volcano, Izu-Bonin arc, Japan SO JOURNAL OF PETROLOGY LA English DT Article DE degree of melting; hot fingers; isotopes; mantle diapir; mantle wedge ID MEDICINE LAKE VOLCANO; HIGH-ALUMINA BASALTS; SUBDUCTION ZONES; MANTLE INTERACTION; BIMODAL MAGMATISM; SHIRAHAMA GROUP; PHASE-RELATIONS; FRACTIONATION; WEDGE; LAVAS AB Basalt-basaltic andesite (< 55 wt % SiO2) and dacite-rhyolite (66-74 wt % SiO2) are the predominant eruptive products in the Sumisu caldera volcano, Izu-Bonin arc, Japan. The most magnesian basalt (8.5% MgO), as well as some of the other basalts, has a low Zr content (20-25 ppm), and cannot yield basalts with higher Zr contents (29-40 ppm) through fractionation and/or assimilation. The high- and low-Zr basalts have different phenocryst assemblages, olivine, plagioclase and pyroxene phenocryst chemistries, REE (rare earth element) patterns, and fluid-mobile element/immobile element ratios. Estimated primary olivine compositions are more magnesian (> F0(91)) in the low-Zr basalts compared with those in high-Zr basalts (< F0(89)). The low-Zr basalts contain up to 11 vol. % augite, but many high-Zr basalts are free of augite, which appears only in their more differentiated products. The low-Zr basalts are considered to be hydrous magmas in which olivine crystallizes first followed by augite and plagioclase, whereas the high-Zr basalts are dry. The low-Zr basalts have higher U/Th ratios than the high-Zr basalts. We suggest that both dry and wet primary basalts existed in the Sumisu magmatic system, each having different trace element concentrations, mineral assemblages and mineral chemistry. The lower contents of Zr and light REE and magnesian primary olivines in the wet basalts could have resulted from a higher degree of partial melting (similar to 20%) of a hydrous source mantle compared with similar to 10% melting of a dry source mantle. The Sr, Nd and Pb isotope compositions of the wet and dry basalts are similar and are limited in range. These lines of evidence indicate that a mantle diapir model might be applicable to satisfy the configuration of such a mantle source region beneath a single volcanic system such as Sumisu. C1 Japan Agcy Marine Earth Sci & Technol, Inst Res Earth Evolut IFREE, Yokosuka, Kanagawa 2370061, Japan. Geol Survey Japan, AIST, Inst Geosci, Tsukuba, Ibaraki 3058567, Japan. Smithsonian Inst, Washington, DC 20560 USA. RP Tamura, Y (reprint author), Japan Agcy Marine Earth Sci & Technol, Inst Res Earth Evolut IFREE, Yokosuka, Kanagawa 2370061, Japan. EM tamuray@jamstec.go.jp OI Tani, Kenichiro/0000-0003-3374-8608 NR 54 TC 36 Z9 40 U1 0 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 J9 J PETROL JI J. Petrol. PD SEP PY 2005 VL 46 IS 9 BP 1769 EP 1803 DI 10.1093/petrology/egi033 PG 35 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 957IA UT WOS:000231362300002 ER PT J AU Austin, M Firnhaber, N Goldberg, L Hansen, GE Magee, C AF Austin, Michele Firnhaber, Natalie Goldberg, Lisa Hansen, Greta Magee, Catherine TI The legacy of anthropology collections care at the National Museum of Natural History SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article AB Priorities for anthropology collections care have remained remarkably constant over the past 150 years within the Smithsonian Institution's National Museum of Natural History and are consistent with contemporary approaches to preventive conservation. Concerns for adequate staff, storage, pest management, and treatment for deteriorating artifacts throughout the history of the Institution have created a legacy affecting almost all aspects of collections care, research, and repatriation. The details of this history have had profound effects on the current condition of objects and their potential for present and future use. This paper will provide an Institution-specific overview of collections care history which may inform museum professionals about the care and research potential of ethnographic and archaeological material. C1 Smithsonian Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Austin, M (reprint author), 705 Laurel Lane, Severna Pk, MD 21146 USA. EM maustin-conservation@comcast.net; firnhaber@SI.EDU; lgoldberg@stny.rr.com; hanseng@SI.EDU NR 33 TC 0 Z9 0 U1 1 U2 4 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD FAL-WIN PY 2005 VL 44 IS 3 BP 185 EP 202 PG 18 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 063TN UT WOS:000239042700004 ER PT J AU Reinert, JF AF Reinert, JF TI List of species described in the egg stage of tribe Aedini (Diptera : Culicidae) with their literature citations SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Review DE Aedini; eggs; mosquitoes ID SCANNING-ELECTRON-MICROSCOPY; PSOROPHORA-COLUMBIAE; FINE-STRUCTURE; AEDES-AEGYPTI; REPRODUCTIVE ISOLATION; SURFACE-STRUCTURE; MOSQUITOES; MORPHOLOGY; OVIPOSITION; ATROPALPUS AB Species of Aedini with published morphological descriptions and/or illustrations of eggs are listed with their literature citations. Each species has a notation indicating descriptions are written, illustrated or both. Only approximately 16% of aedine species currently have morphological descriptions published for the egg stage. The new classification of tribe Aedini proposed by Reinert et al. (2004) is utilized. C1 USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA. Smithsonian Inst, Natl Museum Nat Hist, Walter Reed Biosystemat Unit, Washington, DC 20560 USA. RP Reinert, JF (reprint author), USDA ARS, Ctr Med Agr & Vet Entomol, 1600 1700 SW 23rd Dr, Gainesville, FL 32608 USA. NR 164 TC 8 Z9 8 U1 1 U2 3 PU AMER MOSQUITO CONTROL ASSOC PI MOUNT LAUREL PA 15000 COMMERCE PARKWAY, SUITE C, MOUNT LAUREL, NJ 08054 USA SN 8756-971X EI 1943-6270 J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD SEP PY 2005 VL 21 IS 3 BP 252 EP 262 DI 10.2987/8756-971X(2005)21[252:LOSDIT]2.0.CO;2 PG 11 WC Entomology SC Entomology GA 965MW UT WOS:000231955600003 PM 16252514 ER PT J AU Kaeppler, AL AF Kaeppler, AL TI Animal designs on Samoan Siapo and other thoughts on West Polynesian barkcloth SO JOURNAL OF THE POLYNESIAN SOCIETY LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 27 TC 2 Z9 2 U1 0 U2 0 PU POLYNESIAN SOC INC PI AUCKLAND PA C/O MAORI STUDIES, UNIV AUCKLAND, PRIVATE BAG, AUCKLAND 92019, NEW ZEALAND SN 0032-4000 J9 J POLYNESIAN SOC JI J. Polyn. Soc. PD SEP PY 2005 VL 114 IS 3 BP 197 EP 225 PG 29 WC Anthropology SC Anthropology GA 978ZS UT WOS:000232912400001 ER PT J AU Reid, HL Deem, SL Citino, SB AF Reid, HL Deem, SL Citino, SB TI Extraosseous osteosarcoma in a maned wolf (Chrysocyon brachyurus) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Chrysocyon brachyurus; extraosseous osteosarcoma; maned wolf; p53 suppressor gene; vaccine-site neoplasia ID EXTRASKELETAL OSTEOSARCOMA; FIBROSARCOMAS; SARCOMAS; CATS; GENE; DOG AB A 6-yr-old maned wolf (Chrysocyon brachyurus) was diagnosed with an extraosseous osteosarcoma on the lateral aspect of the right thigh. Antemortem radiography revealed a calcified mass with no skeletal involvement. The mass was excised, but visible regrowth of the tumor was evident within 5 wk. Histologic examination and immunohistochemistry, including staining for p53 tumor suppression gene protein, were performed on the excised mass. The maned wolf was euthanized 13 wk after the initial diagnosis. The neoplasm was located in a site commonly used for the delivery of intramuscular injections, including vaccinations. Although no definitive association can be made, it is worth noting this relationship, as vaccine-site neoplasias have been observed in other species, most notably the domestic cat (Felis domesticus). C1 Univ Guelph, Ontario Vet Coll, Guelph, ON N1G 2W1, Canada. White Oak Conservat Ctr, Yulee, FL 32097 USA. Univ Florida, Coll Vet Med, Dept Small Anim Clin Sci, Gainesville, FL 32610 USA. RP Deem, SL (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. NR 12 TC 4 Z9 4 U1 0 U2 4 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 2005 VL 36 IS 3 BP 523 EP 526 DI 10.1638/04-043.1 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA 995QG UT WOS:000234118300024 PM 17312777 ER PT J AU Hutchinson, A AF Hutchinson, A TI Portraits of the bison: An illustrated guide to bison society. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst Libs, Natl Museum Nat Hist Bldg,10th & Constitut Ave NW, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 2005 VL 130 IS 14 BP 174 EP 174 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 962HS UT WOS:000231722400293 ER PT J AU Hutchinson, A AF Hutchinson, A TI To save the wild bison: Life on the edge in Yellowstone. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst Libs, Natl Museum Nat Hist Bldg,10th & Constitut Ave NW, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 2005 VL 130 IS 14 BP 174 EP 174 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 962HS UT WOS:000231722400292 ER PT J AU Ward, LA AF Ward, LA TI The publications of Kristian Fauchald and the polychaete taxa named in those works SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE LA English DT Biographical-Item DE annelida; bibliography; polychaeta; species list ID PHYLLODOCIDAE POLYCHAETA; GENUS; ATLANTIC; ANNELIDA; REVISION; MALMGREN; RECORDS; GENERA; MEXICO; OCEAN AB Between 1961 and 2002, Kristian Fauchald produced, 72 single and coauthored publications and named three families, thirty four genera and 256 species of polychaetes. A bibliography of his publications, excluding abstracts, book reviews, thesis and dissertation, along with a list of the polychaete taxa named in these works are given here. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Ward, LA (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, POB 37012,MRC 0163, Washington, DC 20560 USA. NR 31 TC 1 Z9 1 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0173-9565 J9 MAR ECOL-EVOL PERSP JI Mar. Ecol.-Evol. Persp. PD SEP-DEC PY 2005 VL 26 IS 3-4 BP 145 EP 154 DI 10.1111/j.1439-0485.2005.00068.x PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 000SM UT WOS:000234482700002 ER PT J AU Meibom, A Righter, K Chabot, N Dehn, G Antignano, A McCoy, TJ Krot, AN Zolensky, ME Petaev, MI Keil, K AF Meibom, A Righter, K Chabot, N Dehn, G Antignano, A McCoy, TJ Krot, AN Zolensky, ME Petaev, MI Keil, K TI Shock melts in QUE 94411, Hammadah al Hamra 237, and Bencubbin: Remains of the missing matrix? SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ZONED METAL GRAINS; CARBONACEOUS CHONDRITES; CH CHONDRITES; PRIMITIVE CHONDRITE; METEORITIC BRECCIA; NITROGEN ISOTOPE; SOLAR NEBULA; CONDENSATION; ORIGIN; METAMORPHISM AB We have studied the CB carbonaceous chondrites Queen Alexandra Range (QUE) 94411, Hammadah al Hamra (HH) 237, and Bencubbin with an emphasis on the petrographical and mineralogical effects of the shock processing that these meteorite assemblages have undergone. Iron-nickel metal and chondrule silicates are the main components in these meteorites. These high-temperature components are held together by shock melts consisting of droplets of dendritically intergrown Fe,Ni-metal/sulfide embedded in silicate glass, which is substantially more FeO-rich (3040 wt%) than the chondrule silicates (FeO < 5 wt%). Fine-grained matrix material, which is a major component in most other chondrite classes, is extremely scarce in QUE 94411 and HH 237, and has not been observed in Bencubbin. This material occurs as rare, hydrated matrix lumps with major and minor element abundances roughly similar to the ferrous silicate shock melts (and Cl). We infer that hydrated, fine-grained material, compositionally similar to these matrix lumps, was originally present between the Fe,Ni-metal grains and chondrules, but was preferentially shock melted. Other shock-related features in QUE 94411, HH 237, and Bencubbin include an alignment and occasionally strong plastic deformation of metal and chondrule fragments. The existence of chemically zoned and metastable Fe,Ni-metal condensates in direct contact with shock melts indicates that the shock did not substantially increase the average temperature of the rock. Because porphyritic olivine-pyroxene chondrules are absent in QUE 94411, HH 237, and Bencubbin, it is difficult to determine the precise shock stage of these meteorites, but the shock was probably relatively light (S2-S3), consistent with a bulk temperature increase of the assemblages of less than similar to 300 degrees C. The apparently similar shock processing of Bencubbin, Weatherford, Gujba (CBa) and QUE 94411/HH 237 (CBb) supports the idea of a common asteroidal parent body for these meteorites. C1 Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Colorado Coll, Dept Geol, Colorado Springs, CO 80903 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. George Washington Univ, Dept Earth & Environm Sci, Washington, DC 20052 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. 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 Hist Nat, Lab Etud Mat Extraterr, USM 0205 LEME, Case Postale 5257 Rue Cuvier, F-75005 Paris, France. EM meibom@mnhn.fr RI Chabot, Nancy/F-5384-2015 OI Chabot, Nancy/0000-0001-8628-3176 NR 61 TC 15 Z9 15 U1 0 U2 2 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 SEP-OCT PY 2005 VL 40 IS 9-10 BP 1377 EP 1391 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 991LV UT WOS:000233816400010 ER PT J AU Clarke, RS Ewing, HP AF Clarke, RS Ewing, HP TI James Smithson (1765-1829): Smithsonian institution founder and its first meteorite investigator SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Smithsonian Inst, Inst Hist Div, SIA, Washington, DC 20560 USA. EM rclarke@volcano.si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A30 EP A30 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000041 ER PT J AU Corrigan, CM McCoy, TJ Rumble, D McDonough, W Goldstein, J Benedix, G Yang, J Walker, R Ash, R Honesto, J AF Corrigan, CM McCoy, TJ Rumble, D McDonough, W Goldstein, J Benedix, G Yang, J Walker, R Ash, R Honesto, J TI EET 83230: Relationship to group IVA irons, and styles and timing of parent body oxidation SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID METEORITES C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Univ Maryland, Dept Geol, College Pk, MD 20742 USA. Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM cari.corrigan@jhuapl.edu NR 6 TC 2 Z9 2 U1 0 U2 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A34 EP A34 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000048 ER PT J AU Foley, CN Nittler, LR Brown, MRM McCoy, TJ Lim, L AF Foley, CN Nittler, LR Brown, MRM McCoy, TJ Lim, L TI Cr, Mn, and Ni on 433 Eros: Further evidence of ordinary chondrite composition SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID X-RAY SPECTROMETER; ELEMENTAL COMPOSITION C1 Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM foley@dtm.ciw.edu RI Lim, Lucy/C-9557-2012 OI Lim, Lucy/0000-0002-9696-9654 NR 6 TC 0 Z9 0 U1 0 U2 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A50 EP A50 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000081 ER PT J AU Fries, M Cody, G Fogel, M Harvey, R Jull, AJT Nittler, L Rost, D Steele, A Toporski, J Vicenzi, E Wainwright, N AF Fries, M Cody, G Fogel, M Harvey, R Jull, AJT Nittler, L Rost, D Steele, A Toporski, J Vicenzi, E Wainwright, N TI Contamination in meteorites stored since 1977-Preliminary results of Antarctic Meteorite Contamination Study (AMCS) SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Carnegie Inst Washington, Washington, DC 20015 USA. Case Western Reserve Univ, Cleveland, OH 44106 USA. Univ Arizona, Tucson, AZ 85721 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Kiel, Kiel, Germany. Marine Biol Lab, Woods Hole, MA 02543 USA. EM m.fries@gl.ciw.edu RI Fogel, Marilyn/M-2395-2015 OI Fogel, Marilyn/0000-0002-1176-3818 NR 4 TC 0 Z9 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A51 EP A51 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000083 ER PT J AU Fries, M Steele, A McCoy, T AF Fries, M Steele, A McCoy, T TI Carbon and mineral phase distribution in intergrain spaces and inclusions within chondrules SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. EM m.fries@gl.ciw.edu NR 3 TC 0 Z9 0 U1 0 U2 2 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 SEP PY 2005 VL 40 IS 9 SU S BP A52 EP A52 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000084 ER PT J AU Lentz, RCF McCoy, TJ Taylor, GJ AF Lentz, RCF McCoy, TJ Taylor, GJ TI Multiple nakhlite lava flows? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Univ Hawaii Manoa, Inst Geophys & Planetol, Honolulu, HI 96822 USA. Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. EM reflentz@higp.hawaii.edu NR 4 TC 4 Z9 4 U1 1 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2005 VL 40 IS 9 SU S BP A91 EP A91 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000162 ER PT J AU MacPherson, GJ Krot, AN Ulyanov, AA AF MacPherson, GJ Krot, AN Ulyanov, AA TI Forsterite-bearing type BCAIs: Case studies in melt distillation and hybridization SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID ALUMINUM-RICH INCLUSIONS; REFRACTORY INCLUSIONS; ALLENDE METEORITE; EVAPORATION; FRACTIONATION; CONDENSATION; CHONDRITES; EVOLUTION; ELEMENT C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Univ Hawaii Manoa, HIGP, SOEST, Honolulu, HI 96822 USA. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. EM glenn@volcano.si.edu NR 9 TC 3 Z9 3 U1 0 U2 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A94 EP A94 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000169 ER PT J AU Mayne, RG Sunshine, JM McCoy, TJ McSween, HY AF Mayne, RG Sunshine, JM McCoy, TJ McSween, HY TI Spectra and petrography of eucrites as a guide to asteroidal basalts SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. SAIC, Chantilly, VA 20151 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM rmayne@utk.edu NR 5 TC 0 Z9 0 U1 0 U2 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A99 EP A99 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000178 ER PT J AU McCoy, TJ Gale, A Dickinson, TL AF McCoy, TJ Gale, A Dickinson, TL TI The early crystallization history of the aubrite parent body SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. Natl Acad, Space Studies Board, Washington, DC 20001 USA. EM mccoy.tim@nmnh.si.edu NR 5 TC 1 Z9 1 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 SEP PY 2005 VL 40 IS 9 SU S BP A100 EP A100 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000180 ER PT J AU Petaev, MI Krot, AN Weisberg, MK AF Petaev, MI Krot, AN Weisberg, MK TI Chemistry of olivine in AOAs: Evidence for variable redox conditions in the solar nebula SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc ID CHONDRITES C1 Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. CUNY, Kingsborough Coll, Dept Phys Sci, Brooklyn, NY 11235 USA. CUNY, Grad Sch, Dept Phys Sci, Brooklyn, NY 11235 USA. Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. NR 3 TC 1 Z9 1 U1 0 U2 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A122 EP A122 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000224 ER PT J AU Rost, D Vicenzi, EP AF Rost, D Vicenzi, EP TI An SEM-based cathodoluminescence study of mesostasis in the nakhlites nakhla, lafayette, and MIL 03346. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM rostd@si.edu NR 4 TC 1 Z9 1 U1 0 U2 0 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 SEP PY 2005 VL 40 IS 9 SU S BP A130 EP A130 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000240 ER PT J AU Rumble, D Corrigan, CM Blake, RE McCoy, TJ AF Rumble, D Corrigan, CM Blake, RE McCoy, TJ TI A terrestrial fractionation line for the oxygen isotopes of phosphate minerals and its application to meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 68th Annual Meeting of the Meteoritical-Society CY SEP 12-16, 2005 CL Gatlinburg, TN SP Meteorit Soc C1 Geophys Lab, Washington, DC 20015 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. EM rumble@gl.ciw.edu NR 6 TC 0 Z9 0 U1 2 U2 5 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 SEP PY 2005 VL 40 IS 9 SU S BP A132 EP A132 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 006BV UT WOS:000234871000245 ER PT J AU Smith, JL Keyghobadi, N Matrone, MA Escher, RL Fonseca, DM AF Smith, JL Keyghobadi, N Matrone, MA Escher, RL Fonseca, DM TI Cross-species comparison of microsatellite loci in the Culex pipiens complex and beyond SO MOLECULAR ECOLOGY NOTES LA English DT Article DE cross-species amplification; Culex pipiens complex; flanking region polymorphism; microsatellites; population genetics ID WEST-NILE-VIRUS; AVIAN MALARIA; VECTOR; IDENTIFICATION; CULICIDAE; DIPTERA; HAWAII AB In the past, we have developed microsatellite loci from the two most common members of the Culex pipiens complex, Culex quinquefasciatus and Culex pipiens. Here we describe seven additional loci and present an extensive survey of a panel of 20 loci across most of the species and subspecies in the complex as well as in morphologically related species. Because we observed a high degree of polymorphism in the flanking regions, we designed new primers and surveyed multiple populations. We present alternate primers and discuss the cross-species usefulness of these Culex microsatellite loci in a phylogenetic context. C1 Acad Nat Sci Philadelphia, Patrick Ctr Environm Res, Philadelphia, PA 19103 USA. Smithsonian Inst, Genet Program, Washington, DC 20008 USA. Florida Med Entomol Lab, Vero Beach, FL 32962 USA. RP Fonseca, DM (reprint author), Acad Nat Sci Philadelphia, Patrick Ctr Environm Res, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. EM fonseca@acnatsci.org RI Meyer, Julie/D-1021-2010; Fonseca, Dina/B-9951-2011 OI Meyer, Julie/0000-0003-3382-3321; Fonseca, Dina/0000-0003-4726-7100 NR 11 TC 39 Z9 39 U1 0 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD SEP PY 2005 VL 5 IS 3 BP 697 EP 700 DI 10.1111/j.1471-8286.2005.01034.x PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 959PF UT WOS:000231529400074 ER PT J AU Songsasen, N Wildt, DE AF Songsasen, N Wildt, DE TI Size of the donor follicle, but not stage of reproductive cycle or seasonality, influences meiotic competency of selected domestic dog oocytes SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Article DE dog; oocyte; in vitro maturation; follicle; meiotic competence ID IN-VITRO MATURATION; CANINE OOCYTES; DEVELOPMENTAL COMPETENCE; NUCLEAR MATURATION; BITCH OOCYTES; MAP KINASE; SPERM PENETRATION; ESTROUS-CYCLE; GOAT OOCYTES; FERTILIZATION AB Ability of ovarian oocytes from the domestic dog to complete nuclear maturation in vitro (IVM) varies markedly among donors and generally is 20% or less of all oocytes cultured. To identify the cause(s) underlying these significant variations in meiotic maturation (to metaphase II; MII), we retrospectively analyzed data from 1,643 oocytes recovered from 90 bitches for which stage of reproduction and season of year were known. Neither stage of reproduction (proestrus/estrus, diestrus, anestrus, or prepuberty) nor season (P > 0.05) influenced the ability of oocytes to achieve nuclear maturation in vitro. A second study was conducted to examine the impact of follicular size on meiotic maturation. Populations of large oocytes were recovered from four categories of follicles (ranging from < 0.5 to > 2 mm in diameter) and cultured in TCM 199 for 48 hr. Follicular size influenced (P < 0.05) meiotic competence. Mean percentages of MII oocytes were 16.9 +/- 9.2, 26.1 +/- 7.6, 38.4 +/- 9.2, and 79.5 +/- 10.9 for oocytes recovered from < 0.5 mm, > 0.5-< 1 mm, 1-2 mm, and > 2 mm diameter follicles, respectively. In summary, stage of reproduction and season have no impact on the ability of dog oocytes to achieve nuclear maturation in vitro. However, we demonstrated for the first time that dog oocytes acquire meiotic competency during follicular development. IVM success of selected oocytes from large size follicles (almost 80%) is about 60% higher than measured in most previous studies involving randomly collected oocytes. (c) 2005 Wiley-Liss, Inc. C1 Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. RP Songsasen, N (reprint author), Conservat & Res Ctr, Dept Reprod Sci, Smithsonians Natl Zool Pk, Front Royal, VA 22630 USA. EM songsasenn@si.edu NR 53 TC 34 Z9 38 U1 1 U2 3 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1040-452X J9 MOL REPROD DEV JI Mol. Reprod. Dev. PD SEP PY 2005 VL 72 IS 1 BP 113 EP 119 DI 10.1002/mrd.20330 PG 7 WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology GA 948RO UT WOS:000230733600014 PM 15915515 ER PT J AU Copperwheat, C Cropper, M Soria, R Wu, KW AF Copperwheat, C Cropper, M Soria, R Wu, KW TI Optical and infrared signatures of ultra-luminous X-ray sources 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 MASS BLACK-HOLES; NEARBY SPIRAL GALAXIES; HIGH-RESOLUTION CAMERA; BINARY-SYSTEMS; IRRADIATION; M82; POPULATION; DISCOVERY; NGC-4559; HERCULIS AB We have constructed a model to describe the optical emission from ultra-luminous X-ray sources (ULXs). We assume a binary model with a black hole accreting matter from a Roche lobe filling companion star. We consider the effects of radiative transport and radiative equilibrium in the irradiated surfaces of both the star and a thin accretion disc. We have developed this model as a tool with which to positively identify the optical counterparts of ULXs, and subsequently derive parameters such as the black hole mass and the luminosity class and spectral type of the counterpart. We examine the dependence of the optical emission on these and other variables. We extend our model to examine the magnitude variation at infrared wavelengths, and we find that observations at these wavelengths may have more diagnostic power than in the optical. We apply our model to existing HST observations of the candidates for the optical counterpart of ULX X-7 in NGC 4559. All candidates could be consistent with an irradiated star alone, but we find that a number of them are too faint to fit with an irradiated star and disc together. Were one of these the optical counterpart to X-7, it would display a significant temporal variation. 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 33 TC 28 Z9 28 U1 2 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2005 VL 362 IS 1 BP 79 EP 88 DI 10.1111/j.1365-2966.2005.09223.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 963KP UT WOS:000231803500007 ER PT J AU Patel, NA Curiel, S Sridharan, TK Zhang, QZ Hunter, TR Ho, PTP Torrelles, JM Moran, JM Gomez, JF Anglada, G AF Patel, NA Curiel, S Sridharan, TK Zhang, QZ Hunter, TR Ho, PTP Torrelles, JM Moran, JM Gomez, JF Anglada, G TI A disk of dust and molecular gas around a high-mass protostar SO NATURE LA English DT Article ID THERMAL RADIO JET; CEPHEUS-A HW2; CONTINUUM EMISSION; STAR-FORMATION; ACCRETION; CLOUD; OUTFLOW; OBJECTS; SYSTEM; CORES AB The processes leading to the birth of low-mass stars such as our Sun have been well studied(1), but the formation of high-mass ( over eight times the Sun's mass, M-.) stars remains poorly understood(2). Recent studies suggest that high-mass stars may form through accretion of material from a circumstellar disk(3), in essentially the same way as low-mass stars form, rather than through the merging of several low-mass stars(4). There is as yet, however, no conclusive evidence(5,6). Here we report the presence of a flattened disk-like structure around a massive 15M(.) protostar in the Cepheus A region, based on observations of continuum emission from the dust and line emission from the molecular gas. The disk has a radius of about 330 astronomical units (AU) and a mass of 1 to 8 M(: It is oriented perpendicular to, and spatially coincident with, the central embedded powerful bipolar radio jet, just as is the case with low-mass stars, from which we conclude that high-mass stars can form through accretion. 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. Consejo Super Invest Cient, IEEC, E-08034 Barcelona, Spain. INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. RP Patel, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS78, Cambridge, MA 02138 USA. EM npatel@cfa.harvard.edu RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085; Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589; Moran, James/0000-0002-3882-4414 NR 30 TC 125 Z9 126 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD SEP 1 PY 2005 VL 437 IS 7055 BP 109 EP 111 DI 10.1038/nature04011 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 960AC UT WOS:000231560400050 PM 16136136 ER PT J AU Vencl, FV Nogueira-de-Sa, F Allen, BJ Windsor, DM Futuyma, DJ AF Vencl, FV Nogueira-de-Sa, F Allen, BJ Windsor, DM Futuyma, DJ TI Dietary specialization influences the efficacy of larval tortoise beetle shield defenses SO OECOLOGIA LA English DT Article DE chemical defense; Chrysomelidae; enemy-free space; failure-time analysis; plant/herbivore ID ENEMY-FREE SPACE; HOST-PLANT; PHYTOPHAGOUS INSECTS; NATURAL ENEMIES; GENERALIST PREDATOR; LEPIDOPTERAN LARVAE; CHEMICAL DEFENSE; CATERPILLAR PREY; CASSIDINE LARVAE; PRAYING MANTIDS AB Plant chemical defenses and escape from natural enemies have been postulated to select for dietary specialization in herbivorous insects. In field and laboratory bioassays, we evaluated the effectiveness of intact and chemically modified larval shield defenses of the generalist Chelymorpha alternans and the specialists Acromis sparsa and Stolas plagiata (Chrysomelidae: Cassidinae) against three natural predators, using larvae reared on two morning glory (Convolvulaceae) species. We assessed whether: (1) specialists were better defended than generalists when both were fed and assayed on the same plant; (2) larval shield defenses were chemical, physical, or both; and (3) specialists exploit chemistry better than generalists. Live specialist larvae survived at higher rates than did generalists in predator bioassays with the bug Montina nigripes (Reduviidae), but there were no differences among groups against two species of Azteca ants (Hymenoptera: Dolichoderinae). Solvent leaching by H2O or MeOH significantly reduced shield efficacy for all species compared to larvae with intact shields. In contrast, freshly killed specialist larvae exhibited significantly lower capture rates and frequencies than the generalists. Although solvent leaching significantly reduced overall shield efficacy for freshly killed larvae of all species, the pattern of leaching effects differed between specialists and generalists, with H2O-leaching having a greater impact on the specialists. The overall vulnerability of the generalists appears due to lower chemical protection, which is ameliorated by increased escape behaviors, suggesting a selective trade-off between these defensive components. These experiments indicate that shield defenses are essential for larval survival and that specialists are superior at exploiting plant compounds residing in the aqueous fraction. Our results support the hypothesis that diet-specialized herbivorous insects have more effective defenses than generalists when both feed on the same plant due to the differential ability to exploit defensive precursors obtained from the host. The evolution of dietary specialization may therefore confer the advantage of enhanced enemy-free space. C1 SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. Univ Estadual Campinas, Inst Biol, Dept Zool, Lab Ecol Quim, BR-13083970 Campinas, SP, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. RP Vencl, FV (reprint author), SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. EM fvencl@life.bio.sunysb.edu NR 61 TC 20 Z9 21 U1 2 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD SEP PY 2005 VL 145 IS 3 BP 404 EP 414 DI 10.1007/s00442-005-0138-9 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 971RN UT WOS:000232401800007 PM 16001225 ER PT J AU Behrensmeyer, AK Fursich, FT Gastaldo, RA Kidwell, SM Kosnik, MA Kowalewski, M Plotnick, RE Rogers, RR Alroy, J AF Behrensmeyer, AK Fursich, FT Gastaldo, RA Kidwell, SM Kosnik, MA Kowalewski, M Plotnick, RE Rogers, RR Alroy, J TI Are the most durable shelly taxa also the most common in the marine fossil record? SO PALEOBIOLOGY LA English DT Article ID DEATH ASSEMBLAGES; BODY-SIZE; PATTERNS; ENVIRONMENTS; BIODIVERSITY; DISSOLUTION; DIVERSITY; BIAS; PALEOECOLOGY; DESTRUCTION AB This paper tests whether the most common fossil brachiopod, gastropod, and bivalve genera also have intrinsically more durable shells. Commonness was quantified using occurrence frequency of the 450 most frequently occurring genera of these groups in the Paleobiology Database (PBDB). Durability was scored for each taxon on the basis of shell size, thickness, reinforcement (ribs, folds, spines), mineralogy, and microstructural organic content. Contrary to taphonomic expectation, common genera in the PBDB are as likely to be small, thin-shelled, and unreinforced as large, thick-shelled, ribbed, folded, or spiny. In fact, only six of the 30 tests we performed showed a statistically significant relationship between durability and occurrence frequency, and these six tests were equally divided in supporting or contradicting the taphonomic expectation. Thus, for the most commonly occurring genera in these three important groups, taphonomic effects are either neutral with respect to durability or compensated for by other factors (e.g., less durable taxa were more common in the original communities). These results suggest that biological information is retained in the occurrence frequency patterns of our target groups. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Univ Wurzburg, Inst Palaontol, D-97070 Wurzburg, Germany. Colby Coll, Dept Geol, Waterville, ME 04901 USA. Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Ctr Ctr Reef Biodivers, Townsville, Qld 4811, Australia. Virginia Polytech Inst & State Univ, Dept Geosci, Blacksburg, VA 24061 USA. Univ Illinois, Dept Earth & Environm Sci, Chicago, IL 60607 USA. Macalester Coll, Dept Geol, St Paul, MN 55105 USA. Univ Calif Santa Barbara, Natl Ctr Anal & Synth, Santa Barbara, CA 93101 USA. RP Behrensmeyer, AK (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM Behrensa@si.edu; franz.fuersich@mail.uni-wuerzburg.de; ragastal@colby.edu; skidwell@uchicago.edu; mkosnik@alumni.uchicago.edu; michalk@vt.edu; plotnick@uic.edu; rogers@macalester.edu; alroy@nceas.ucsb.edu RI Kowalewski, Michal/B-4263-2008; Alroy, John/B-4585-2009; Kosnik, Matthew/G-2312-2010; Plotnick, Roy/B-4534-2008 OI Kowalewski, Michal/0000-0002-8575-4711; Kosnik, Matthew/0000-0001-5380-7041; Plotnick, Roy/0000-0001-6177-3355 NR 48 TC 33 Z9 34 U1 0 U2 13 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD FAL PY 2005 VL 31 IS 4 BP 607 EP 623 DI 10.1666/0094-8373(2005)031[0607:ATMDST]2.0.CO;2 PG 17 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 973LP UT WOS:000232524500005 ER PT J AU O'Keefe, FR Carrano, MT AF O'Keefe, FR Carrano, MT TI Correlated trends in the evolution of the plesiosaur locomotor system SO PALEOBIOLOGY LA English DT Article ID CALIFORNIA SEA-LION; ZALOPHUS-CALIFORNIANUS; INDEPENDENT CONTRASTS; MARINE REPTILES; COPES RULE; MAMMALS; SIZE; SAUROPTERYGIA; MECHANISMS; ALLOMETRY AB This paper investigates trends in the evolution of body size and shape in the Plesiosauria, a diverse clade of Mesozoic marine reptiles. Using measures from well-preserved plesiosaur specimens, we document and interpret evolutionary patterns in relative head size, body size, and locomotor variables. Size increase is a significant trend in the clade as a whole, and in constituent clades. The trend in relative head size is of variance increase; observed head sizes are both smaller and larger than ancestral values. In the locomotor system, changes in propodial and girdle proportions appear concomitant with body size increase and are interpreted as allometric responses to the physical constraints of large body size. Other trends in the locomotor system are significantly correlated with both body size and relative head size. These locomotor trends evolved convergently in several clades of plesiosaurs, and may have had an ecomorphological basis, although data are lacking to constrain speculation on this point. The evolution of the locomotor system in plesiosaurs sheds new light on the response of aquatic tetrapods to the physical constraints of foraging at large body size. C1 New York Inst Technol, NYCOM 2, Dept Anat, Old Westbury, NY 11568 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP O'Keefe, FR (reprint author), New York Inst Technol, NYCOM 2, Dept Anat, Room 326, Old Westbury, NY 11568 USA. EM frokeefe@nyit.edu; Carrano.Matthew@nmnh.si.edu RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 81 TC 38 Z9 40 U1 0 U2 6 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD FAL PY 2005 VL 31 IS 4 BP 656 EP 675 PG 20 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 973LP UT WOS:000232524500008 ER PT J AU Chu, X Dalgarno, A Groenenboom, GC AF Chu, X Dalgarno, A Groenenboom, GC TI Polarizabilities of Sc and Ti atoms and dispersion coefficients for their interaction with helium atoms SO PHYSICAL REVIEW A LA English DT Article ID STATES; TRANSITIONS; COLLISIONS; HE AB The dynamic scalar and tensor polarizabilities of Sc and Ti are computed with time-dependent density functional theory. These polarizabilities are used to compute the isotropic and anisotropic dispersion interactions in ScHe and TiHe. We find C-6,C-0(ScHe)=30.00, C-6,C-2(ScHe)=-1.63, C-6,C-0(TiHe)=28.40, and C-6,C-2(TiHe)=-0.90 (E(h)a(0)(6)). We show that an estimate of the dispersion anisotropy based on static polarizabilities results in an overestimation by a factor of 2. C1 ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nijmegen, Inst Theoret Chem, NL-6525 ED Nijmegen, Netherlands. RP Chu, X (reprint author), ITAMP, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Groenenboom, Gerrit/F-9692-2015 NR 22 TC 19 Z9 19 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 SEP PY 2005 VL 72 IS 3 AR 032703 DI 10.1103/PhysRevA.72.032703 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 969IR UT WOS:000232228300083 ER PT J AU Afshordi, N Zaldarriaga, M Kohri, K AF Afshordi, N Zaldarriaga, M Kohri, K TI Instability of dark energy with mass-varying neutrinos SO PHYSICAL REVIEW D LA English DT Article ID COSMOLOGICAL CONSTANT AB An interesting dynamical model for dark energy which does not require extremely light scalar fields such as quintessence, and at the same time explains the (near) coincidence between the neutrino and dark energy densities is the model of dark energy coupled to mass-varying neutrinos (MaVaNs). Despite the attractions of this model, we show that, generically, this model contains a catastrophic instability which occurs when neutrinos become nonrelativistic. As a result of this instability, as neutrinos become nonrelativistic, they condense into neutrino nuggets which redshift away similar to cold dark matter, and thus cease to act as dark energy. Any stable MaVaNs dark energy model is extremely contrived and is virtually indistinguishable from a cosmological constant. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. RP Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, MS-51,60 Garden St, Cambridge, MA 02138 USA. EM nafshordi@cfa.harvard.edu; mzaldarriaga@cfa.harvard.edu; kkohri@cfa.harvard.edu NR 22 TC 102 Z9 102 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 SEP PY 2005 VL 72 IS 6 AR 065024 DI 10.1103/PhysRevD.72.065024 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 969JJ UT WOS:000232230100081 ER PT J AU Sobrino, C Neale, PJ Montero, O Lubian, LM AF Sobrino, C Neale, PJ Montero, O Lubian, LM TI Biological weighting function for xanthophyll de-epoxidation induced by ultraviolet radiation SO PHYSIOLOGIA PLANTARUM LA English DT Article ID UV-B RADIATION; DIATOM PHAEODACTYLUM-TRICORNUTUM; PHOTOSYSTEM-II; NANNOCHLOROPSIS-GADITANA; DIADINOXANTHIN CYCLE; ELECTRON-TRANSPORT; VIOLAXANTHIN CYCLE; HIGHER-PLANTS; INHIBITION; LIGHT AB The light-induced de-epoxidation of xanthophylls is an important photoprotective mechanism in plants and algae. Exposure to ultraviolet radiation (UVR, 280-400 nm) can change the extent of xanthophyll de-epoxidation, but different types of responses have been reported. The de-epoxidation of violaxanthin (V) to zeaxanthin (Z), via the intermediate antheraxanthin, during exposure to UVR and photosynthetically active radiation (PAR, 400-700 nm) was studied in the marine picoplankter Nannochloropsis gaditana (Eustigmatophyceae) Lubian. Exposures used a filtered xenon lamp, which gives PAR and UVR similar to natural proportions. Exposure to UVR plus PAR increased de-epoxidation compared with under PAR alone. In addition, de-epoxidation increased with the irradiance and with the inclusion of shorter wavelengths in the spectrum. The spectral dependence of light-induced de-epoxidation under UVR and PAR exposure was well described by a model of epoxidation state (EPS) employing a biological weighting function (BWF). This model fit measured EPS in eight spectral treatments using Schott long pass filters, with six intensities for each filter, with a R-2 = 0.90. The model predicts that 56% of violaxanthin is de-epoxidated, of which UVR can induce as much as 24%. The BWF for EPS was similar in shape to the BWF for UVR inhibition of photosynthetic carbon assimilation in N. gaditana but with about 22-fold lower effectiveness. These results demonstrate a connection between the presence of de-epoxidated Z and the inhibition under UVR exposures in N. gaditana. Nevertheless, they also indicate that de-epoxidation is insufficient to prevent UVR inhibition in this species. C1 CSIC, Inst Ciencias Marinas Andalucia, Puerto Real, Cadiz, Spain. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Sobrino, C (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM sobrinoc@si.edu RI Neale, Patrick/A-3683-2012; Sobrino, Cristina/J-3534-2012; LUBIAN, LUIS/L-7241-2014; Montero, Olimpio/L-8263-2014; OI Montero, Olimpio/0000-0002-0241-8756; Sobrino, Cristina/0000-0003-0431-1220 NR 52 TC 23 Z9 23 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-9317 EI 1399-3054 J9 PHYSIOL PLANTARUM JI Physiol. Plant. PD SEP PY 2005 VL 125 IS 1 BP 41 EP 51 DI 10.1111/j.1399-3054.2005.00538.x PG 11 WC Plant Sciences SC Plant Sciences GA 959ID UT WOS:000231510500005 ER PT J AU Winter, K Holtum, JAM AF Winter, K Holtum, JAM TI The effects of salinity, crassulacean acid metabolism and plant age on the carbon isotope composition of Mesembryanthemum crystallinum L., a halophytic C(3)-CAM species SO PLANTA LA English DT Article DE carbon isotope composition; crassulacean acid metabolism; CO(2) exchange; Mesembryanthemum; salinity; stress ID DIFFERENT ENVIRONMENTAL-CONDITIONS; VASCULAR EPIPHYTES; DELTA-C-13 VALUES; ICE PLANT; CAM PLANT; INDUCTION; CO2; DISCRIMINATION; PHOTOSYNTHESIS; EXCHANGE AB The carbon isotope composition of the halophyte Mesembryanthemum crystallinum L. (Aizoaceae) changes when plants are exposed to environmental stress and when they shift from C(3) to crassulacean acid metabolism (CAM). We examined the coupling between carbon isotope composition and photosynthetic pathway by subjecting plants of different ages to salinity and humidity treatments. Whole shoot delta(13)C values became less negative in plants that were exposed to 400 mM NaCl in the hydroponic solution. The isotopic change had two components: a direct NaCl effect that was greatest in plants still operating in the C(3) mode and decreased proportionally with increasing levels of dark fixation, and a second component related to the degree of CAM expression. Ignoring the presumably diffusion-related NaCl effect on carbon isotope ratios results in an overestimation of nocturnal CO(2) gain in comparison to an isotope versus nocturnal CO(2) gain calibration established previously for C(3) and CAM species grown under well-watered conditions. It is widely taken for granted that the shift to CAM in M. crystallinum is partially under developmental control and that CAM is inevitably expressed in mature plants. Plants, cultivated under non-saline conditions and high relative humidity ( RH) for up to 63 days, maintained diel CO(2) gas-exchange patterns and delta(13)C values typical of C(3) plants. However, a weak CAM gas-exchange pattern and an increase in delta(13)C value were observed in non-salt-treated plants grown at reduced RH. These observations are consistent with environmental control rather than developmental control of the induction of CAM in mature M. crystallinum under non-saline conditions. C1 Smithsonian Trop Res Inst, Ancona, Italy. James Cook Univ, Trop Plant Sci, Townsville, Qld 4811, Australia. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Ancona, Italy. EM winter@si.edu RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 NR 43 TC 32 Z9 35 U1 2 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0032-0935 J9 PLANTA JI Planta PD SEP PY 2005 VL 222 IS 1 BP 201 EP 209 DI 10.1007/s00425-005-1516-6 PG 9 WC Plant Sciences SC Plant Sciences GA 968LJ UT WOS:000232163700020 PM 15968514 ER PT J AU Warner, DJ AF Warner, DJ TI True north - And why it mattered in eighteenth-century America SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 73 TC 1 Z9 1 U1 0 U2 0 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD SEP PY 2005 VL 149 IS 3 BP 372 EP 385 PG 14 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 978SG UT WOS:000232892700006 ER PT J AU Gingerich, O AF Gingerich, O TI I Bernard Cohen - 1 March 1914 - 20 June 2003 - Biographical memoirs SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Biographical-Item C1 Harvard Univ, Cambridge, MA 02138 USA. Smithsonian Astrophys Observat, Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Univ, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD SEP PY 2005 VL 149 IS 3 BP 395 EP 398 PG 4 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 978SG UT WOS:000232892700008 ER PT J AU Reach, WT Megeath, ST Cohen, M Hora, J Carey, S Surace, J Willner, SP Barmby, P Wilson, G Glaccum, W Lowrance, P Marengo, M Fazio, GG AF Reach, WT Megeath, ST Cohen, M Hora, J Carey, S Surace, J Willner, SP Barmby, P Wilson, G Glaccum, W Lowrance, P Marengo, M Fazio, GG TI Absolute calibration of the infrared array camera on the Spitzer Space Telescope SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SPECTRAL IRRADIANCE CALIBRATION; STANDARD STARS; SIRTF AB The Infrared Array Camera ( IRAC) on the Spitzer Space Telescope is absolutely calibrated by comparing photometry of a set of A stars near the north ecliptic pole to predictions based on ground- based observations and a stellar atmosphere model. The brightness of point sources is calibrated to an accuracy of 3%, relative to models for A- star stellar atmospheres, for observations performed and analyzed in the same manner as for the calibration stars. This includes corrections for the location of the star in the array and the location of the centroid within the peak pixel. Long- term stability of the IRAC photometry was measured by monitoring the brightness of A dwarfs and K giants ( near the north ecliptic pole) observed several times per month; the photometry is stable to 1.5% ( rms) over a year. Intermediate- timescale stability of the IRAC photometry was measured by monitoring at least one secondary calibrator ( near the ecliptic plane) every 12 hr while IRAC was in nominal operations; the intermediate- term photometry is stable, with a 1% dispersion ( rms). One of the secondary calibrators was found to have significantly time- variable ( 5%) mid- infrared emission, with a period ( 7.4 days) matching the optical light curve; it is possibly a Cepheid variable. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. RP Reach, WT (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM reach@ipac.caltech.edu RI Reach, William/C-4710-2008; Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Hora, Joseph/0000-0002-5599-4650; Reach, William/0000-0001-8362-4094 NR 18 TC 430 Z9 430 U1 4 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2005 VL 117 IS 835 BP 978 EP 990 DI 10.1086/432670 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958LZ UT WOS:000231451100012 ER PT J AU Grabow, JU Palmer, ES McCarthy, MC Thaddeus, P AF Grabow, JU Palmer, ES McCarthy, MC Thaddeus, P TI Supersonic-jet cryogenic-resonator coaxially oriented beam-resonator arrangement Fourier transform microwave spectrometer SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID LABORATORY DETECTION; INTERFERENCE SPECTROSCOPY; MASER INTERFEROMETER; ROTATIONAL SPECTRA; MODES; MIRRORS AB The design and performance of a cryogenic (T=77 K) microwave spectrometer are reported. This instrument, being a time domain experiment in microwave molecular spectroscopy, consists of three basic components: a near-confocal Fabry-Perot-type resonator, a pulsed microwave excitation Fourier transform system, and a pulsed molecular-beam source in a coaxially oriented beam-resonator arrangement. With the recently developed spectrometer, which employs confocal reflectors cooled to liquid-nitrogen temperature, we were able to reduce the system noise of the instrument significantly. The high sensitivity of this next generation spectrometer allows the detection of transient species produced in a dc-discharge nozzle, other short-lived molecules and complexes at low abundance, or nearly nonpolar molecules. We will discuss the spectrometer design with respect to critical considerations of the resonator theory in the context of cryogenic operation, as well as important aspects of classical circuit theory applied to excitation and detection of molecular systems in a resonator. Following the description of the dc-discharge source, the performance of the instrument is demonstrated. (c) 2005 American Institute of Physics. C1 Leibniz Univ Hannover, Inst Phys Chem & Elektrochem, D-30167 Hannover, Germany. Harvard Smithsonian Ctr Astrophys, Geo & Radioastron Div, Cambridge, MA 02138 USA. Harvard Univ, Sch Med, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Leibniz Univ Hannover, Inst Phys Chem & Elektrochem, Callinstr 3-3A,Lehrgebiet A, D-30167 Hannover, Germany. EM jens-uwe.grabow@pci.uni-hannover.de OI McCarthy, Michael/0000-0001-9142-0008 NR 36 TC 41 Z9 41 U1 1 U2 10 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD SEP PY 2005 VL 76 IS 9 AR 093106 DI 10.1063/1.2039347 PG 11 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 966PZ UT WOS:000232034400007 ER PT J AU Solis, MA Davis, DR Nishida, K AF Solis, MA Davis, DR Nishida, K TI Life history and systematics of Albusambia elaphoglossumae (Lepidoptera : Crambidae): A new genus and species of musotimine with leaf-mining biology from Costa Rica SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE Elaphoglossum conspersum; F. biolleyi gregarious larvae; fern; leaf ruiner; neotropical; Neurophyseta; Proacrias; Undulambia ID LYGODIUM-MICROPHYLLUM SCHIZAEACEAE; FERNS; MOTHS AB Albusambia elaphoglossumae Solis & Davis. a new genus and species, is described. It was discovered mining, the fronds of the fern Elaphoglossum conspersum in Costa Rica (San Jose and Cartago Provinces, at elevations of 2300-3100 m). The type series was obtained by rearing of the immature stap in laboratory. The adult is defined by unique genital characters, and the Pupa with a medial depression on the vertex and with two anterolateral horn-like structures on the prothorax. The larva is a gregarious leaf ruiner with its body flattened dorsoventrally and head prognathous morphological adaptations to its leaf-mining habit are new to the Musotiminae. Fern-feeding musotimines are important to the discovery of new biological control agents for invasive ferns. C1 USDA, ARS, Natl Museum Nat Hist, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. Univ Costa Rica, Escuela Biol, Sistema Estudios Posgrado Biol, San Jose 2060, Costa Rica. RP Solis, MA (reprint author), USDA, ARS, Natl Museum Nat Hist, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. EM asolis@sel.barc.usda.gov; davis.don@nmnh.si.edu; knishida@cariari.ucr.ac.cr NR 26 TC 4 Z9 4 U1 0 U2 0 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD SEP-DEC PY 2005 VL 53 IS 3-4 BP 487 EP 501 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 022ER UT WOS:000236038200017 PM 17354458 ER PT J AU Leytem, AB Turner, BL Raboy, V Peterson, KL AF Leytem, AB Turner, BL Raboy, V Peterson, KL TI Linking manure properties to phosphorus solubility in calcareous SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID PHOSPHATE SORPTION; SOIL-PHOSPHORUS; RUNOFF; IRON; INCEPTISOLS; VERTISOLS AB Land application of manure can increase P transfer in runoff, although the risk depends in part on the characteristics of the manure. We assessed this for calcareous soils using manures from swine (Sus domesticus) fed one of five barley varieties (Hordeum vulgare L.), including four low phytate mutants and a normal variety, to produce manures with a range of total P (6.8-4.9 g P kg(-1)), water-soluble P (4.3-8.0 g P kg(-1)), total N/P ratios (2.5:1-5.5:1), and total C/P ratios (31:1-67:1). Two experiments were conducted. First, manures were incorporated into three soils on a N (150 mg N kg(-1) soil) or P (27.5 mg P kg(-1) soil) basis three times during a 7-wk incubation. Second, 10 additional soils were incubated for 2 wk following a single P-based manure application (82.5 mg P kg(-1) soil). Water and NaHCO3 (Olsen) extractable P were determined at regular intervals, with microbial P determined by fumigation-extraction after each incubation. For N-based application (i.e., variable P amendment), extractable P increased with total P applied. For P-based applications, the increase in soil P was more closely correlated to microbial P concentration than manure P composition or soil properties. These results suggest that stimulation of the microbial biomass by added organic C is important in determining soil P solubility following manure application. C1 USDA, ARS, NW Irrigat & Soils Res Lab, Kimberly, ID 83341 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. USDA, ARS, Small Grains & Potato Germplasm Res Unit, Aberdeen, ID 83210 USA. RP Leytem, AB (reprint author), USDA, ARS, NW Irrigat & Soils Res Lab, 3793N 3600E, Kimberly, ID 83341 USA. EM leytem@nwisrl.ars.usda.gov RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 NR 47 TC 27 Z9 27 U1 1 U2 10 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD SEP-OCT PY 2005 VL 69 IS 5 BP 1516 EP 1524 DI 10.2136/sssaj2004.0315 PG 9 WC Soil Science SC Agriculture GA 963PY UT WOS:000231817500019 ER PT J AU LaPolla, JS Cover, SP AF LaPolla, JS Cover, SP TI New species of Pheidole (Hymenoptera : Formicidae) from Guyana, with a list of species known from the country SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Formicidae; Guyana; Myrmecinae; Pheidole; scrobifera-group; tachigaliae-group AB Two new species of Pheidole from Guyana are described, P. funki LaPolla and P schultzi LaPolla. One species, P. funki, belongs to the scrobifera-group and is only the second member of the species-group known from South America. The other species, P schultzi, belongs to the tachigaliae-group. P. tachigaliae is also illustrated to identify morphological differences with P. schultzi. Modified versions of Wilson's (2003) key are provided. Recent biotic survey work across Guyana revealed that at least 86 Pheidole species are present in the country. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. Harvard Univ, Dept Entomol, Museum Comparat Zool, Cambridge, MA 02138 USA. RP LaPolla, JS (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, POB 37012,NHB,CE518,MRC 188, Washington, DC 20013 USA. EM lapollaj@si.edu; cover@oeb.harvard.edu NR 6 TC 3 Z9 3 U1 0 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD SEP-DEC PY 2005 VL 131 IS 3-4 BP 365 EP 374 PG 10 WC Entomology SC Entomology GA 001PZ UT WOS:000234550100004 ER PT J AU Holtum, JAM Winter, K AF Holtum, JAM Winter, K TI Carbon isotope composition of canopy leaves in a tropical forest in Panama throughout a seasonal cycle SO TREES-STRUCTURE AND FUNCTION LA English DT Article DE canopy; carbon isotope composition; crassulacean acid metabolism; tropical trees; water-use efficiency ID CRASSULACEAN ACID METABOLISM; FICUS-INSIPIDA WILLD; WATER-USE EFFICIENCY; DELTA-C-13 VALUES; PIONEER TREE; DRY FOREST; PLANTS; CO2; PHOTOSYNTHESIS; RATIOS AB The seasonal variation in delta(13)C values was measured in leaves from 17 upper canopy, five mid-canopy and in four gap tree species, as well as in five epiphyte and five vine species, in a seasonally dry lowland tropical forest at Parque Natural Metropolitano near Panama City, Republic of Panama. No seasonal variation was detected in the delta(13)C values of mature exposed leaves from either the upper or mid- canopy. However, canopy position did influence the delta(13)C value. The mean isotopic composition of leaves from the mid- canopy was more negative than that of the upper canopy throughout the year. The delta(13)C value was also influenced by leaf development, with juvenile leaves on average 1.5 parts per thousand less negative than mature leaves. The five epiphyte species exhibited delta(13)C values that were typical of crassulacean acid metabolism ( CAM). Codonanthe uleana, with isotopic values of -19.9 to -22.1 parts per thousand, is only the second species in the Gesneriaceae reported to express CAM, whereas values between -14.6 and -22.0 parts per thousand indicate that Peperomia macrostachya can exhibit different degrees of CAM. The isotopic composition of exposed mature leaves from the vines showed little interspecific variation and was similar to the upper-canopy leaves of the trees. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. James Cook Univ N Queensland, Townsville, Qld 4811, Australia. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. EM winterk@tivoli.si.edu RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 NR 38 TC 25 Z9 35 U1 4 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0931-1890 J9 TREES-STRUCT FUNCT JI Trees-Struct. Funct. PD SEP PY 2005 VL 19 IS 5 BP 545 EP 551 DI 10.1007/s00468-005-0413-8 PG 7 WC Forestry SC Forestry GA 961EP UT WOS:000231645000007 ER PT J AU Didham, RK Tylianakis, JM Hutchison, MA Ewers, RM Gemmell, NJ AF Didham, RK Tylianakis, JM Hutchison, MA Ewers, RM Gemmell, NJ TI Are invasive species the drivers of ecological change? SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID BIOLOGICAL INVASIONS; COMPETITION; GRASSLAND; BIODIVERSITY; EXTINCTION; ECOSYSTEMS; REGIMES AB Invasive species are widely accepted as one of the leading direct causes of biodiversity loss. However, much of the evidence for this contention is based on simple correlations between exotic dominance and native species decline in degraded systems. Although appealing, direct causality is not the only possible interpretation. A plausible alternative hypothesis is that exotic dominance could be the indirect consequence of habitat modification driving native species loss. In a new paper, MacDougall and Turkington now provide the first direct test of whether invasive species are the drivers of community change, or merely I passengers' along for the environmental ride. C1 Univ Canterbury, Sch Biol Sci, Christchurch, New Zealand. Univ Gottingen, Fac Agrarokol, D-37073 Gottingen, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Didham, RK (reprint author), Univ Canterbury, Sch Biol Sci, Private Bag 4800, Christchurch, New Zealand. EM raphael.didham@canterbury.ac.nz RI Gemmell, Neil/C-6774-2009; Didham, Raphael/B-5953-2011; Tylianakis, Jason/B-6634-2011 OI Gemmell, Neil/0000-0003-0671-3637; Tylianakis, Jason/0000-0001-7402-5620 NR 28 TC 299 Z9 321 U1 18 U2 227 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 SEP PY 2005 VL 20 IS 9 BP 470 EP 474 DI 10.1016/j.tree.2005.07.006 PG 5 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 967YV UT WOS:000232128300003 PM 16701420 ER PT J AU Smith, DA Ralls, K Cypher, BL Maldonado, JE AF Smith, DA Ralls, K Cypher, BL Maldonado, JE TI Assessment of scat-detection dog surveys to determine kit fox distribution SO WILDLIFE SOCIETY BULLETIN LA English DT Article DE California; detection dogs; endangered species; fecal analysis; fecal DNA; kit fox; scats; Vulpes macrotis mutica ID VULPES-MACROTIS-MUTICA; MOLECULAR TRACKING; ROCKY-MOUNTAINS; NEW-MEXICO; CONSERVATION; POPULATIONS; SPOTLIGHT; ABUNDANCE; DNA AB Developing sound conservation strategies for carnivores in fragmented landscapes relies on accurate distribution information. Fecal (scat) surveys can provide an effective survey technique, especially when collection of scats is followed by genetic analysis of DNA extracted from scats. Furthermore, use of specially trained detection dogs to locate scats on survey routes may greatly enhance scat recovery. We evaluated utility of scat-detection dog surveys as a method to determine current distribution of kit foxes (Vulpes macrotis mutica). We used a trained dog to locate scats in core and satellite population areas with various densities and different habitat conditions. We compared number of scats found per kilometer on transects along different road and vegetation types. Scat-detection dog surveys detected the presence of kit foxes in each population area searched, regardless of relative fox density and vegetation type. We found a greater number of scats on unpaved than paved roads, suggesting unpaved roads are more appropriate for monitoring of foxes. Additionally, we found a greater number of scats in saltbush (Atriplex polycarpa) scrub than in non-native grassland. This result was strongly influenced by latitude, and was probably related to a north-south precipitation gradient. Our results demonstrate that scat-detection dog surveys can provide an effective conservation tool to map current kit fox distribution. This survey method has a wide application to other carnivore species, and can be used to survey multiple species simultaneously. C1 Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Calif State Coll Bakersfield, Endangered Species Recovery Program, Bakersfield, CA 93389 USA. Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. RP Smith, DA (reprint author), Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. EM debsmith@u.washington.edu NR 33 TC 28 Z9 29 U1 1 U2 25 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 USA SN 0091-7648 J9 WILDLIFE SOC B JI Wildl. Soc. Bull. PD FAL PY 2005 VL 33 IS 3 BP 897 EP 904 DI 10.2193/0091-7648(2005)33[897:AOSDST]2.0.CO;2 PG 8 WC Biodiversity Conservation SC Biodiversity & Conservation GA 997QN UT WOS:000234261800013 ER PT J AU Stockley, B Smith, AB Littlewood, T Lessios, HA Mackenzie-Dodds, JA AF Stockley, B Smith, AB Littlewood, T Lessios, HA Mackenzie-Dodds, JA TI Phylogenetic relationships of spatangoid sea urchins (Echinoidea): taxon sampling density and congruence between morphological and molecular estimates SO ZOOLOGICA SCRIPTA LA English DT Article ID ECHINODERM CLASSES; ACCURACY; RECONSTRUCTION; INCONGRUENCE; REAPPRAISAL; CHARACTERS; EVOLUTION AB A phylogeny for 21 species of spatangoid sea urchins is constructed using data from three genes and results compared with morphology-based phylogenies derived for the same taxa and for a much larger sample of 88 Recent and fossil taxa. Different data sets and methods of analysis generate different phylogenetic hypotheses, although congruence tests show that all molecular approaches produce trees that are congruent with each other. By contrast, the trees generated from morphological data differ significantly according to taxon sampling density,and only those with dense sampling (after a posteriori weighting) are congruent with molecular estimates. With limited taxon sampling, secondary reversals in deep-water taxa are interpreted as plesiomorphies, pulling them to a basal position. The addition of fossil taxa with their unique character combinations reveals hidden homoplasy and generates a phylogeny that is compatible with molecular estimates. As homoplasy levels were found to be broadly similar across different anatomical structures in the echinoid test, no one suite of morphological characters can be considered to provide more reliable phylogenetic information. Some traditional groupings are supported, including the grouping of Loveniidae, Brissidae and Spatangidae within the Micrasterina, but the Asterostomatidae is shown to be polyphyletic with members scattered amongst at least five different clades. As these are mostly deep-sea taxa, this finding implies multiple independent invasions into the deep sea. C1 Nat Hist Museum, London SW67 5BD, England. Smithsonian Trop Res Inst, Balboa, Panama. RP Stockley, B (reprint author), Nat Hist Museum, Cromwell Rd, London SW67 5BD, England. EM a.smith@nbm.ac.uk; Lessiosh@stri.org RI Smith, Andrew/B-9849-2009; Littlewood, Tim/B-5230-2008 OI Littlewood, Tim/0000-0002-2718-4001 NR 44 TC 32 Z9 37 U1 1 U2 9 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD SEP PY 2005 VL 34 IS 5 BP 447 EP 468 DI 10.1111/j.1463-6409.2005.00201.x PG 22 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 963YN UT WOS:000231842700001 ER PT J AU Zanata, AM Vari, RP AF Zanata, AM Vari, RP TI The family Alestidae (Ostariophysi, Characiformes): a phylogenetic analysis of a trans-Atlantic clade SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE African Characidae; Chalceus; fossil evidence; gigantism; miniaturization; phylogeny; sindacharax ID FISHES TELEOSTEI; CHARACOID FISH; WEST-AFRICA; CHARACIDAE; SERRASALMINAE; PISCES; INTERRELATIONSHIPS; REDESCRIPTION; REVISION; BRYCINUS AB The overall most parsimonious hypothesis of relationships based on 200 characters indicates that the Alestidae is the closest relative of Chalceus, a genus previously assigned to the Neotropical Characidae. Chalceus is shifted into the Alestidae, which becomes the only trans-Atlantic family level group within the Characiformes. Various previously proposed suprageneric assemblages within the Alestidae (e.g. Petersiini) failed to delimit monophyletic groups under the intrafamilial phylogenetic analysis. The evaluation of fossil alestids within the context of the phylogeny indicates that the ancestors of Alestes, Arnoldichthys, Brycinus, Bryconaethiops and Hydrocynus evolved prior to the early Eocene (Cuisian of Upper Ypresian), 49-54.8 million years ago, with the fossil Alestoides most closely related to Alestes. The phylogenetic information further indicates a minimum age of 90-112 million years for the Alestidae. Contrary to previous hypotheses, the fossil African Sindacharax was found to be most similar to the clade including the alestid genus Bryconaethiops rather than most closely related to the South American subfamily Serrasalminae. Evaluation of the fossil Mahengecharax carrolli fails to support its hypothesized placement as the sister group to all Recent members of the Alestidae. Two separate episodes of miniaturization and one episode of gigantism occurred within the evolution of the Alestidae. (C) 2005 The Linnean Society of London. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. Univ Fed Bahia, Inst Biol, Dept Zool, BR-40170290 Salvador, BA, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-159,POB 37012, Washington, DC 20013 USA. EM varir@si.edu NR 185 TC 78 Z9 80 U1 1 U2 6 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 SEP PY 2005 VL 145 IS 1 BP 1 EP 144 DI 10.1111/j.1096-3642.2005.00183.x PG 144 WC Zoology SC Zoology GA 965UB UT WOS:000231974700001 ER PT J AU Konstantinov, AS Duckett, CN AF Konstantinov, AS Duckett, CN TI A description of four new species of Clavicornaltica Scherer from Continental Asia (vol 1037, pg 39, 2005) SO ZOOTAXA LA English DT Correction C1 Smithsonian Inst, Natl Museum Nat Hist, USDA ARS, PSI,Systemat Entomol Lab, Washington, DC 20013 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Konstantinov, AS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA ARS, PSI,Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM akonstan@sel.barc.usda.gov; duckettc@si.edu NR 1 TC 1 Z9 1 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 AUG 30 PY 2005 IS 1042 BP 64 EP 64 PG 1 WC Zoology SC Zoology GA 959HL UT WOS:000231508700005 ER PT J AU Soon, WWH AF Soon, WWH TI Variable solar irradiance as a plausible agent for multidecadal variations in the Arctic-wide surface air temperature record of the past 130 years SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VARIABILITY; PERIOD AB This letter offers new evidence motivating a more serious consideration of the potential Arctic temperature responses as a consequence of the decadal, multidecadal and longer-term persistent forcing by the ever-changing solar irradiance both in terms of total solar irradiance (TSI, i.e., integrated over all wavelengths) and the related UV irradiance. The support for such a solar modulator can be minimally derived from the large (> 75%) explained variance for the decadally-smoothed Arctic surface air temperatures (SATs) by TSI and from the time-frequency structures of the TSI and Arctic SAT variability as examined by wavelet analyses. The reconstructed Arctic SAT time series based on the inverse wavelet transform, which includes decadal ( 5 - 15 years) and multidecadal ( 40 - 80 years) variations and a longer-term trend, contains nonstationary but persistent features that are highly correlated with the Sun's intrinsic magnetic variability especially on multidecadal time scales. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Soon, WWH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. EM wsoon@cfa.harvard.edu NR 13 TC 34 Z9 36 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 27 PY 2005 VL 32 IS 16 AR L16712 DI 10.1029/2005GL023429 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 960CY UT WOS:000231569000002 ER PT J AU Zillio, T Volkov, I Banavar, JR Hubbell, SP Maritan, A AF Zillio, T Volkov, I Banavar, JR Hubbell, SP Maritan, A TI Spatial scaling in model plant communities SO PHYSICAL REVIEW LETTERS LA English DT Article ID TROPICAL FORESTS; BETA-DIVERSITY AB We present an analytically tractable variant of the voter model that provides a quantitatively accurate description of beta diversity (two-point correlation function) in two tropical forests. The model exhibits novel scaling behavior that leads to links between ecological measures such as relative species abundance and the species-area relationship. C1 SISSA, Int Sch Adv Studies, INFM, I-34014 Trieste, Italy. Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. INFM, I-35131 Padua, Italy. RP Zillio, T (reprint author), SISSA, Int Sch Adv Studies, INFM, Via Beirut 2-4, I-34014 Trieste, Italy. NR 16 TC 35 Z9 35 U1 1 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 26 PY 2005 VL 95 IS 9 AR 098101 DI 10.1103/PhysRevLett.95.098101 PG 4 WC Physics, Multidisciplinary SC Physics GA 959FR UT WOS:000231503600065 PM 16197253 ER PT J AU Narita, N Suto, Y Winn, JN Turner, EL Aoki, W Leigh, CJ Sato, B Tamura, M Yamada, T AF Narita, N Suto, Y Winn, JN Turner, EL Aoki, W Leigh, CJ Sato, B Tamura, M Yamada, T TI Errata: Subaru HDS transmission spectroscopy of the transiting extrasolar planet HD 209458b (vol 57, pg 471, 2005) SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Correction C1 Univ Tokyo, Sch Sci, Dept Phys, Tokyo 1130033, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Kobe Univ, Grad Sch Sci & Technol, Kobe, Hyogo 6578501, Japan. RP Univ Tokyo, Sch Sci, Dept Phys, Tokyo 1130033, Japan. EM narita@utap.phys.s.u-tokyo.ac.jp; suto@phys.s.u-tokyo.ac.jp; jwinn@cfs.harvard.edu; elt@astro.princeton.edu; aoki.wako@nao.ac.jp; cjl@astro.livjm.ac.uk; satobn@kobe-u.ac.jp; tamuramt@cc.noa.ac.jp; yamada@optik.mtk.nao.ac.jp RI Turner, Edwin/A-4295-2011 NR 1 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD AUG 25 PY 2005 VL 57 IS 4 BP 705 EP 705 DI 10.1093/pasj/57.4.705 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 963VP UT WOS:000231834600017 ER PT J AU Zhang, JH Yang, D Mathis, WN AF Zhang, JH Yang, D Mathis, WN TI A new genus and species of Ephydridae (Diptera) from the Oriental Region SO ZOOTAXA LA English DT Article DE Diptera; Ephydridae; Sinops; new genus; new species; China AB A new genus and species of the tribe Dagini ( subfamily Ephydrinae), Sinops sichuanensis, are described from specimens collected in China (Sichuan: Emeishan Mountain), and three species formerly comprising "the fluvialis group" of Psilephydra Hendel are transferred to the new genus ( S. fluvialis (Miyagi), S. kaskiensis (Mathis) and S. nepalensis ( Mathis)) as new combinations. A cladistic analysis of the new genus with related genera in the tribe Dagini is presented and discussed, and keys to the genera of Dagini and to the species of the new genus are presented. C1 China Agr Univ, Dept Entomol, Beijing 100094, Peoples R China. Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Zhang, JH (reprint author), China Agr Univ, Dept Entomol, Beijing 100094, Peoples R China. NR 10 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 AUG 23 PY 2005 IS 1040 BP 31 EP 43 PG 13 WC Zoology SC Zoology GA 958EX UT WOS:000231428600003 ER PT J AU Wilson, E Pedretti, E Bregman, J Mah, RW Traub, WA AF Wilson, E Pedretti, E Bregman, J Mah, RW Traub, WA TI Adaptive DFT-based interferometer fringe tracking SO EURASIP JOURNAL ON APPLIED SIGNAL PROCESSING LA English DT Article DE fringe tracking; DFT; interferometry; IOTA; real time ID IOTA INTERFEROMETER; PREDICTION AB An automatic interferometer fringe tracking system has been developed, implemented, and tested at the Infrared Optical Telescope Array (IOTA) Observatory at Mount Hopkins, Arizona. The system can minimize the optical path differences (OPDs) for all three baselines of the Michelson stellar interferometer at IOTA. Based on sliding window discrete Fourier-transform (DFT) calculations that were optimized for computational efficiency and robustness to atmospheric disturbances, the algorithm has also been tested extensively on offline data. Implemented in ANSI C on the 266 MHz PowerPC processor running the VxWorks real-time operating system, the algorithm runs in approximately 2.0 milliseconds per scan (including all three interferograms), using the science camera and piezo scanners to measure and correct the OPDs. The adaptive DFT-based tracking algorithm should be applicable to other systems where there is a need to detect or track a signal with an approximately constant-frequency carrier pulse. One example of such an application might be to the field of thin-film measurement by ellipsometry, using a broadband light source and a Fourier-transform spectrometer to detect the resulting fringe patterns. C1 Intellizat, Redwood Shores, CA 94065 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wilson, E (reprint author), Intellizat, 454 Barkentine Lane, Redwood Shores, CA 94065 USA. EM ed.wilson@intellization.com; epedrett@umich.edu; jesse.bregman-1@nasa.gov; robert.w.mah@nasa.gov; wtraub@cfa.harvard.edu NR 25 TC 0 Z9 0 U1 0 U2 1 PU HINDAWI PUBLISHING CORPORATION PI NEW YORK PA 410 PARK AVENUE, 15TH FLOOR, #287 PMB, NEW YORK, NY 10022 USA SN 1110-8657 J9 EURASIP J APPL SIG P JI EURASIP J Appl. Signal Process. PD AUG 21 PY 2005 VL 2005 IS 15 BP 2559 EP 2572 DI 10.1155/ASP.2005.2559 PG 14 WC Engineering, Electrical & Electronic SC Engineering GA 007FH UT WOS:000234953500014 ER PT J AU Jardine, M van Ballegooijen, AA AF Jardine, M van Ballegooijen, AA TI Slingshot prominences above stellar X-ray coronae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : activity; stars : imaging; stars : individual : AB Dor; stars : rotation; stars : spots ID RAPIDLY ROTATING STARS; XMM-NEWTON VIEW; AB-DORADUS; DIFFERENTIAL ROTATION; EXPLORER OBSERVATIONS; MAGNETIC TOPOLOGY; DOPPLER IMAGES; AR LACERTAE; 44I BOOTIS; COOL STARS AB We present a new model for the coronal structure of rapidly rotating solar-type stars. The presence of prominences trapped in co-rotation 2-5 stellar radii above the stellar surface has been taken as evidence that the coronae of these stars must be very extended. The observed surface magnetic fields, however, cannot contain X-ray emitting gas out to these distances. We present an alternative model: that these prominences are trapped in long thin loops embedded not in the X-ray corona, but in the wind. Above coronal helmet streamers, oppositely directed wind-bearing field lines reconnect to form closed loops, which then fill up with gas that was originally part of the wind. We demonstrate that static equilibria exist for these loops at a range of pressures and temperatures. The maximum loop height falls as the rotation rate increases, but rises as the loop temperature decreases. For a solar mass star with a rotation period of 0.5 d, whose X-ray corona extends 1 R-star above the surface, loops at temperatures of 10(4) K can extend out to 5 R-star. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jardine, M (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM moira.jardine@st-and.ac.uk OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 43 TC 24 Z9 24 U1 2 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2005 VL 361 IS 4 BP 1173 EP 1179 DI 10.1111/j.1365-2966.2005.09256.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958PF UT WOS:000231459500007 ER PT J AU Mandelbaum, R Hirata, CM Seljak, U Guzik, J Padmanabhan, N Blake, C Blanton, MR Lupton, R Brinkmann, J AF Mandelbaum, R Hirata, CM Seljak, U Guzik, J Padmanabhan, N Blake, C Blanton, MR Lupton, R Brinkmann, J TI Systematic errors in weak lensing: application to SDSS galaxy-galaxy weak lensing SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; galaxies : distances and redshifts; galaxies : halos ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; ANGULAR-CORRELATION FUNCTION; MASS CORRELATION-FUNCTION; EARLY DATA RELEASE; REDSHIFT SURVEY; INTRINSIC CORRELATION; PHOTOMETRIC REDSHIFTS; LUMINOSITY FUNCTION; ALIGNMENTS AB Weak lensing is emerging as a powerful observational tool to constrain cosmological models, but is at present limited by an incomplete understanding of many sources of systematic error. Many of these errors are multiplicative and depend on the population of background galaxies. We show how the commonly cited geometric test, which is rather insensitive to cosmology, can be used as a ratio test of systematics in the lensing signal at the I per cent level. We apply this test to the galaxy-galaxy lensing analysis of the Sloan Digital Sky Survey (SDSS), which at present is the sample with the highest weak lensing signal-to-noise ratio and has the additional advantage of spectroscopic redshifts for lenses. This allows one to perform meaningful geometric tests of systematics for different subsamples of galaxies at different mean redshifts, such as brighter galaxies, fainter galaxies and high-redshift luminous red galaxies, both with and without photometric redshift estimates. We use overlapping objects between SDSS and the DEEP2 and 2df-Sloan LRG and Quasar (2SLAQ) spectroscopic surveys to establish accurate calibration of photometric redshifts and to determine the redshift distributions for SDSS. We use these redshift results to compute the projected surface density contrast Delta Sigma around 259 609 spectroscopic galaxies in the SDSS; by measuring Delta Sigma with different source samples we establish consistency of the results at the 10 per cent level (1 sigma). We also use the ratio test to constrain shear calibration biases and other systematics in the SDSS survey data to determine the overall galaxy-galaxy weak lensing signal calibration uncertainty. We find no evidence of any inconsistency among many subsamples of the data. C1 Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. Abdus Salaam Int Ctr Theoret Phys, I-34014 Trieste, Italy. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Apache Point Observ, Sunspot, NM 88349 USA. RP Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA. EM rmandelb@princeton.edu RI Padmanabhan, Nikhil/A-2094-2012; Mandelbaum, Rachel/N-8955-2014 OI Mandelbaum, Rachel/0000-0003-2271-1527 NR 83 TC 143 Z9 144 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2005 VL 361 IS 4 BP 1287 EP 1322 DI 10.1111/j.1365-2966.2005.09282.x PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958PF UT WOS:000231459500019 ER PT J AU Nicastro, F Mathur, S Elvis, M Drake, J Fiore, F Fang, T Fruscione, A Krongold, Y Marshall, H Williams, R AF Nicastro, F Mathur, S Elvis, M Drake, J Fiore, F Fang, T Fruscione, A Krongold, Y Marshall, H Williams, R TI Chandra detection of the first X-ray forest along the line of sight to Markarian 421 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (Markarian 421); intergalactic medium; quasars : absorption lines ID HOT INTERGALACTIC MEDIUM; LY-ALPHA FOREST; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; PROBE WMAP OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; QUASI-STELLAR OBJECTS; HIGH-VELOCITY CLOUDS; LOCAL GROUP; FUSE OBSERVATIONS; ABSORPTION-LINES AB We present the first >= 3.5 (conservative) or >= 5.8 sigma (sum-of-lines significance) detection of two warm-hot intergalactic medium (WHIM) filaments at z > 0, which we find along the line of sight to the blazar Mrk 421. These systems are detected through highly ionized resonant metal absorption in high-quality Chandra ACIS and HRC Low Energy Transmission Grating (LETG) spectra of Mrk 421, obtained following our two Target of Opportunity requests during two outburst phases (F0.5-2 keV = 40 and 60 mcrab; 1 crab 2; 10(-8) ergs s(-1) cm(-2)). Columns of He-like oxygen and H-like nitrogen can be detected in the co-added LETG spectrum of Mrk 421 down to a sensitivity of N-O VII >= 8 x 10(14) cm(-2) and N-N (VII) >= 10(15) cm(-2), respectively, at a significance >= 3 sigma. The two intervening WHIM systems that we detect have O (VII) and N (VII) columns of N-O (VII) (1.0 +/- 0.3)x10(15) cm(-2), N-N (VII) = (0.8 +/- 0.4) x 10(15) cm(-2) and N-O (VII) ( 0.7 +/- 0.3) x 10(15) cm(-2), N-N (VII) (1.4 +/- 0.5) x 10(15) cm(-2), respectively. We identify the closest of these two systems with an intervening WHIM filament at cz 3300 +/- 300 km s(-1). The second system, instead, at cz 8090 +/- 300 km s(-1), is identified with an intervening WHIM filament located similar to 13 Mpc from the blazar. The filament at cz 3300 +/- 300 lies <= 5 Mpc from a known H (I) Ly alpha system at cz 3046 +/- 12 km s(-1) (Shull and coworkers) whose 3 sigma maximal H (I) kinetic temperature, as derived from the observed line FWHM, is T <= 1.2 x 10(5) K. This temperature is inconsistent with the temperature measured for the X-ray filament, so if the systems are related, a multiphase WHIM is required. Combining UV and far-ultraviolet (FUV) upper limits on the H (I) Ly alpha and the O (VI2s -> 2p) transitions with our measurements in the X-rays, we show that, for both filaments, equilibrium collisional ionization ( with residual photoionization by both the diffuse UV and X-ray background and the beamed emission of Mrk 421 along our line of sight) provides acceptable solutions. These solutions define ranges of temperatures, metallicity ratios, and equivalent H column densities, which are in good agreement with the predictions of hydrodynamical simulations for the formation of large-scale structures in the universe. From the detected number of WHIM filaments along this line of sight we can estimate the number of O (VII) filaments per unit redshift with columns larger than 7 x 10(14) cm(-2), dN(OVII)/dz(NOVII >= 7 x 10(14)) 67(-43)(+88), consistent, within the large 1 sigma errors, with the hydrodynamical simulation predictions of dN (O VII) / dz(N-O VII >= 7 x 10(14)) = 30. Finally, we measure a cosmological mass density of X-ray WHIM filaments Omega(b) = 0.027(-0.019)(+0.038) x 10([O/H]-1), consistent with both model predictions and the estimated number of "missing" baryons at low redshift. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. MIT, Cambridge, MA 02139 USA. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Fiore, Fabrizio/0000-0002-4031-4157; Nicastro, Fabrizio/0000-0002-6896-1364 NR 67 TC 97 Z9 98 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 AUG 20 PY 2005 VL 629 IS 2 BP 700 EP 718 DI 10.1086/431270 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500010 ER PT J AU Herrnstein, JR Moran, JM Greenhill, LJ Trotter, AS AF Herrnstein, JR Moran, JM Greenhill, LJ Trotter, AS TI The geometry of and mass accretion rate through the maser accretion disk in NGC 4258 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies : active; galaxies : individual (NGC 4258); galaxies : nuclei; masers ID ACTIVE GALACTIC NUCLEI; NGC 4258; GALAXY NGC-4258; BLACK-HOLES; BRAIDED JETS; EMISSION; RADIO; LUMINOSITY; NGC4258; ALTERNATIVES AB A maximum likelihood analysis of the NGC 4258 maser positions and velocities reveals a similar to 2 sigma deviation from Keplerian motion in the projected rotation curve of the high-velocity features, corresponding to a similar to 9 km s(-1), or 0.8%, flattening of the LOS velocities with respect to Keplerian motion over the range of the high-velocity masers. While there are a number of potential explanations for this flattening, we argue for pure Keplerian rotation in an inclination-warped disk on the basis of the ability of this model to explain a number of otherwise puzzling features of the system. A radial gradient in the disk inclination of 0.034 mas(-1) is not only consistent with the observed rotation curve, but it generates a bowl along the near edge of the disk that naturally explains the otherwise puzzling narrow spread in the declinations of the systemic masers. It also explains the existence and location of an apparently recurring flare among the systemic masers. There is no significant evidence for non-Keplerian rotation in the inclination-warped disk. An additional implication of the inclination warp is that the disk rises in front of and obscures the central engine at a disk radius of about 8.3 mas, or 0.29 pc. By comparing the observed X-ray column to conditions in the disk at this radius, we argue that the disk must be atomic at 0.29 pc. Hence, we conclude that the molecular-to-atomic transition occurs just beyond the outermost maser at 0.28 pc, and from this we infer an accretion rate of similar to 10(-4)alpha M-circle dot yr(-1), where alpha (<= 1) is the standard dimensionless parameterization of the kinematic viscosity. Our model suggests that most of the observed X-ray column arises in the warped accretion disk at 0.29 pc and that the maser emission is truncated at large radii predominantly as a result of the molecular-to-atomic phase transition originally proposed by Neufeld & Maloney. The inferred accretion rate is consistent with the jet-dominated accretion models of Yuan et al. C1 Renaissance Techol Corp, E Setauket, NY 11733 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. RP Herrnstein, JR (reprint author), Renaissance Techol Corp, 600 Route 25A, E Setauket, NY 11733 USA. OI Moran, James/0000-0002-3882-4414 NR 46 TC 95 Z9 95 U1 2 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 719 EP 738 DI 10.1086/431421 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500011 ER PT J AU Chandra, P Ray, A Schlegel, EM Sutaria, FK Pietsch, W AF Chandra, P Ray, A Schlegel, EM Sutaria, FK Pietsch, W TI Chandra's tryst with SN1995N SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; line : identification; nuclear reactions, nucleosynthesis, abundances; supernovae : individual (SN 1995N); techniques : image processing; X-rays : stars ID X-RAY-EMISSION; CIRCUMSTELLAR INTERACTION; SUPERNOVAE; EVOLUTION; SPECTRUM; PLASMAS; ORIGIN; RATES AB We present the spectroscopic and imaging analysis of Type IIn supernova SN 1995N observed with the Chandra X- Ray Observatory on 2004 March 27. We compare the spectrum obtained from our Chandra observation with that of the previous observation with ASCA in 1998. We find the presence of neon lines in the Chandra spectrum that were not reported in the ASCA observation. We see no evidence of iron in either epoch. The observed absorption column depth indicates an extra component over and above the Galactic absorption component and is possibly due to a cool dense shell between the reverse shock and the contact discontinuity in the ejecta. The ASCA and the ROSAT observations suggested a nonlinear behavior of the X- ray light curve. However, with the higher spatial resolution and sensitivity of Chandra, we separate out many nearby sources in the supernova field of view that had additionally contributed to the supernova flux due to the large point-spread function of ASCA. Taking out the contribution of those nearby sources, we find that the light curves are consistent with a linear decline profile. We consider the light curve in the high-energy band separately. We discuss our results in the context of models of nucleosynthesis and the interaction of the shock waves with the circumstellar medium in core-collapse supernovae. C1 Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tech Univ Munich, Phys Dept T30, D-85748 Garching, Germany. RP Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. EM poonam@tifr.res.in; akr@tifr.res.in; eschlegel@cfa.harvard.edu; fsutaria@ph.tum.de; wnp@mpe.mpg.de NR 36 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP 933 EP 943 DI 10.1086/431573 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500031 ER PT J AU Graves, GJM Challis, PM Chevalier, RA Crotts, A Filippenko, AV Fransson, C Garnavich, P Kirshner, RP Li, W Lundqvist, P McCray, R Panagia, N Phillips, MM Pun, CJS Schmidt, BP Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC AF Graves, GJM Challis, PM Chevalier, RA Crotts, A Filippenko, AV Fransson, C Garnavich, P Kirshner, RP Li, W Lundqvist, P McCray, R Panagia, N Phillips, MM Pun, CJS Schmidt, BP Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC TI Limits from the Hubble Space Telescope on a point source in SN 1987A SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; stars : neutron; supernovae : individual (SN 1987A) ID LARGE-MAGELLANIC-CLOUD; X-RAY PULSAR; SUPERNOVA REMNANT CTB-109; ROTATING MASSIVE STARS; NEUTRON-STAR; BLACK-HOLE; PRESUPERNOVA EVOLUTION; BEPPOSAX OBSERVATIONS; SPHERICAL ACCRETION; MAGNETIC-FIELDS AB We observed supernova 1987A ( SN 1987A) with the Space Telescope Imaging Spectrograph ( STIS) on the Hubble Space Telescope ( HST) in 1999 September and again with the Advanced Camera for Surveys ( ACS) on the HST in 2003 November. Our spectral observations cover ultraviolet ( UV) and optical wavelengths from 1140 to 10266 8, and our imaging observations cover UV and optical wavelengths from 2900 to 9650 angstrom. No point source is observed in the remnant. We obtain a limiting flux of F-opt <= 1. 6; 10(-14) ergs s(-1) cm(-2) in the wavelength range 2900 - 9650 angstrom for any continuum emitter at the center of the supernova remnant ( SNR). This corresponds to an intrinsic luminosity of L-opt <= 5 x 10(33) ergs s (-1). It is likely that the SNR contains opaque dust that absorbs UV and optical emission, resulting in an attenuation of similar to 35% due to dust absorption in the SNR. Correcting for this level of dust absorption would increase our upper limit on the luminosity of a continuum source by a factor of 1.54. Taking into account dust absorption in the remnant, we find a limit of L-opt 8 x 10(33) ergs s (-1). We compare this upper bound with empirical evidence from point sources in other supernova remnants and with theoretical models for possible compact sources. We show that any survivor of a possible binary systemmust be nomore luminous than an F6 main- sequence star. Bright young pulsars such as Kes 75 or the Crab pulsar are excluded by optical and X- ray limits on SN 1987A. Other nonplerionic X- ray point sources have luminosities similar to the limits on a point source in SN 1987A; RCW103 and Cas A are slightly brighter than the limits on SN 1987A, while Pup A is slightly fainter. Of the young pulsars known to be associated with SNRs, those with ages <= 5000 yr are all too bright in X- rays to be compatible with the limits on SN 1987A. Examining theoretical models for accretion onto a compact object, we find that spherical accretion onto a neutron star is firmly ruled out and that spherical accretion onto a black hole is possible only if there is a larger amount of dust absorption in the remnant than predicted. In the case of thin- disk accretion, our flux limit requires a small disk, no larger than 1010 cm, with an accretion rate no more than 0.3 times the Eddington accretion rate. Possible ways to hide a surviving compact object include the removal of all surrounding material at early times by a photon- driven wind, a small accretion disk, or very high levels of dust absorption in the remnant. It will not be easy to improve substantially on our optical- UV limit for a point source in SN 1987A, although we can hope that a better understanding of the thermal infrared emission will provide a more complete picture of the possible energy sources at the center of SN 1987A. C1 Univ Calif Santa Cruz, Dept Astron, UCO, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Columbia Univ, Astrophys Lab, Inst Strings Cosmol & Astroparticle Phys, New York, NY 10027 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Stockholm Univ, Dept Astron, Stockholm Observ, AlbaNova, SE-10691 Stockholm, Sweden. Univ Notre Dame, Dept Phys & Astron, Notre Dame, IN 46556 USA. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Lab Astron & Space Phys, Greenbelt, MD 20771 USA. Mt Stromlo & Siding Spring Observ, Canberra, ACT 2611, Australia. Cerro Tololo Interamer Observ, La Serena, Chile. Univ Calif Berkeley, Lawrence Berkeley Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Graves, GJM (reprint author), Univ Calif Santa Cruz, Dept Astron, UCO, Lick Observ, Santa Cruz, CA 95064 USA. EM graves@astro.ucsc.edu OI Schmidt, Brian/0000-0001-6589-1287; Schmidt, Brian/0000-0002-8538-9195 NR 109 TC 41 Z9 41 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 AUG 20 PY 2005 VL 629 IS 2 BP 944 EP 959 DI 10.1086/431422 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MP UT WOS:000231159500032 ER PT J AU Brogan, CL Gaensler, BM Gelfand, JD Lazendic, JS Lazio, TJW Kassim, NE McClure-Griffiths, NM AF Brogan, CL Gaensler, BM Gelfand, JD Lazendic, JS Lazio, TJW Kassim, NE McClure-Griffiths, NM TI Discovery of a radio supernova remnant and nonthermal X-rays coincident with the TeV source HESS J1813-178 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; ISM : individual (G12.8-0.0, HESS J1813+178); radio lines : ISM; supernova remnants; X-rays : ISM ID GALACTIC PLANE; MILKY-WAY; PARTICLE-ACCELERATION; MOLECULAR CLOUDS; CONTINUUM SURVEY; SN 1006; SHELL; W33; RADIATION; EMISSION AB We present the discovery of nonthermal radio and X-ray emission positionally coincident with the TeV gammaray source HESS J1813 - 178. We demonstrate that the nonthermal radio emission is due to a young shell-type supernova remnant (SNR), G12.8 - 0.0, and constrain its distance to be greater than 4 kpc. The X-ray emission is primarily nonthermal and is consistent with either an SNR shell or unidentified pulsar or pulsar wind nebula origin; pulsed emission is not detected in archival ASCA data. A simple synchrotron plus inverse Compton model for the broadband emission assuming that all of the emission arises from the SNR shell implies maximum energies of (30 - 450)[B/(10 mu G)](-0.5) TeV. Further observations are needed in order to confirm that the broadband emission has a common origin and to better constrain the X-ray spectrum. C1 Inst Astron, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Brogan, CL (reprint author), Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA. EM cbrogan@ifa.hawaii.edu RI Gaensler, Bryan/F-8655-2010; Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; McClure-Griffiths, Naomi/0000-0003-2730-957X; Gaensler, Bryan/0000-0002-3382-9558 NR 36 TC 51 Z9 51 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP L105 EP L108 DI 10.1086/491471 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MT UT WOS:000231159900009 ER PT J AU Sharon, K Ofek, EO Smith, GP Broadhurst, T Maoz, D Kochanek, CS Oguri, M Suto, Y Inada, N Falco, EE AF Sharon, K Ofek, EO Smith, GP Broadhurst, T Maoz, D Kochanek, CS Oguri, M Suto, Y Inada, N Falco, EE TI Discovery of multiply imaged galaxies behind the cluster and lensed quasar SDSS J1004+4112 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : individual (SDSS J1004+4112); gravitational lensing; large-scale structure of universe ID HUBBLE-SPACE-TELESCOPE; LENSING ANALYSIS; MASS PROFILE; SDSS-J1004+4112; MODELS; A1689 AB We have identified three multiply imaged galaxies in Hubble Space Telescope images of the redshift z = 0.68 cluster responsible for the large-separation quadruply lensed quasar, SDSS J1004 + 4112. Spectroscopic 0.68 redshifts have been secured for two of these systems using the Keck I 10 m telescope. The most distant lensed galaxy, at, forms at least four images, and an Einstein ring encompassing 3.1 times more area than z = 3.332 the Einstein ring of the lensed QSO images at, due to the greater source distance. For a second multiply z = 1.74 imaged galaxy, we identify Ly alpha emission at a redshift of. The cluster mass profile can be constrained z = 2.74 from near the center of the brightest cluster galaxy, where we observe both a radial arc and the fifth image of the lensed quasar, to the Einstein radius of the highest redshift galaxy, similar to 110 kpc. Our preliminary modeling indicates that the mass approximates an elliptical body, with an average projected logarithmic gradient of similar or equal to -0.5. The system is potentially useful for a direct measurement of world models in a previously untested redshift range. C1 Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Tokyo, Dept Phys, Sch Sci, Tokyo 1130033, Japan. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Univ Tokyo, Inst Astron, Fac Sci, Tokyo 1810015, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sharon, K (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RI Oguri, Masamune/C-6230-2011 NR 18 TC 44 Z9 44 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2005 VL 629 IS 2 BP L73 EP L76 DI 10.1086/452633 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 954MT UT WOS:000231159900001 ER PT J AU Orth, K Day, JW Boesch, DF Clairain, EJ Mitsch, WJ Shabman, L Simenstad, C Streever, B Watson, C Wells, J Whigham, D AF Orth, K Day, JW Boesch, DF Clairain, EJ Mitsch, WJ Shabman, L Simenstad, C Streever, B Watson, C Wells, J Whigham, D TI Lessons learned: An assessment of the effectiveness of a National Technical Review Committee for oversight of the plan for the restoration of the Mississippi Delta SO ECOLOGICAL ENGINEERING LA English DT Article DE Mississippi Delta; coastal restoration; technical oversight review; US Army Corps of Engineers AB This paper presents lessons learned about the function of a national review Committee (National Technical Review Committee-NTRC) for a major U.S. Corps of Engineers water resources study, the Louisiana Coastal Area Study (the restoration of the Mississippi Delta). Lessons learned are based on responses to five questions to the NTRC. What was the best thing about the experience? What was the worst thing about the experience? What one thing was not done that should have been done? What is the most important lesson for similar future committees? Are there any other lessons? Several important cross-cutting themes were recommended for future national review groups: (1) a national review group adds value and (2) the Corps must early on think through the structure, process and use of the review group, including: the group's purpose, the degree of independence or interaction, treatment of Committee members, the use of the group's comments, scheduling of group activities, and needs to support the group. While the NTRC found much that should lead to improvements for future groups, it strongly recommends that seeking top professional advice during the course of study is appropriate for the Corps. Committee members found their experiences to be professionally and personally rewarding. (c) 2005 Published by Elsevier B.V. C1 US Army Corps Engineers, Inst Water Resources, Alexandria, VA 22315 USA. Louisiana State Univ, Sch Coast & Environm, 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. Ohio State Univ, Columbus, OH 43202 USA. Resources Future Inc, Washington, DC 20036 USA. Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. BP Explorat Alaska Inc, Anchorage, AK 99519 USA. Colorado State Univ, Civil Engn Dept, Ft Collins, CO 80523 USA. Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Orth, K (reprint author), US Army Corps Engineers, Inst Water Resources, 7701 Telegraph Rd, Alexandria, VA 22315 USA. EM kenneth.d.orth@usace.army.mil OI Whigham, Dennis/0000-0003-1488-820X NR 7 TC 3 Z9 3 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 J9 ECOL ENG JI Ecol. Eng. PD AUG 20 PY 2005 VL 25 IS 2 BP 153 EP 167 DI 10.1016/j.ecoleng.2005.04.002 PG 15 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA 971VL UT WOS:000232412800003 ER PT J AU Konstantinov, AS Duckett, CN AF Konstantinov, AS Duckett, CN TI New species of Clavicornaltica Scherer (Coleoptera : Chrysomelidae) from continental Asia SO ZOOTAXA LA English DT Article DE Chrysomelidae; Clavicornaltica; new species; female genitalia; China; Vietnam ID FLEA BEETLES; ALTICINAE; EVOLUTION; GENUS AB Four new species of Clavicornaltica Scherer are described and illustrated, of which two are from China (C. dali new species and C. longsheng new species) and two are from Vietnam (C. tamdao new species and C. vietnamensis new species). The wing and metathorax are described and illustrated for the genus for the first time. A key to the newly described species is presented. Male genitalia of Clavicornaltica australis Konstantinov are illustrated for the first time. C1 ARS, Systemat Entomol Lab, PSI,USDA, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. RP Konstantinov, AS (reprint author), ARS, Systemat Entomol Lab, PSI,USDA, Smithsonian Inst,Natl Museum Nat Hist, POB 37012,MRC 168, Washington, DC 20013 USA. EM akonstan@sel.barc.usda.gov; duckettc@si.edu NR 15 TC 8 Z9 8 U1 2 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 19 PY 2005 IS 1037 BP 49 EP 64 PG 16 WC Zoology SC Zoology GA 956HG UT WOS:000231290200005 ER PT J AU Staines, CL AF Staines, CL TI Franz Spaeth: Publications and proposed taxa SO ZOOTAXA LA English DT Biographical-Item DE Spaeth; biography; bibliography; proposed taxa AB Franz Spaeth (1863-1946) was an Austrian lawyer who became an authority on world Cassidinae (Coleoptera: Chrysomelidae). From 1885 until 1961 he published 145 papers in which he described 111 genera and 1212 species. This article presents a brief biographical sketch, a bibliography of his published works, and a list of proposed taxa. 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 0 TC 1 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 AUG 15 PY 2005 IS 1035 BP 1 EP 49 PG 49 WC Zoology SC Zoology GA 954TA UT WOS:000231176500001 ER PT J AU DeMajistre, R Brandt, PC Immel, TJ Yee, JH Dalgarno, A Paxton, LJ Kharchenko, V AF DeMajistre, R Brandt, PC Immel, TJ Yee, JH Dalgarno, A Paxton, LJ Kharchenko, V TI Storm-time enhancement of mid-latitude ultraviolet emissions due to energetic neutral atom precipitation SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EQUATORIAL AURORA; LOW-LATITUDE; IMAGE/HENA; MISSION; IMAGER AB In this work we present a direct connection between Energetic Neutral Atom (ENA) precipitation and enhanced ultraviolet emissions from the mid-latitude thermosphere during times of geomagnetic disturbance. Data from the IMAGE/HENA instrument provides information about ENA emission from the ring current, the IMAGE/FUV instrument shows the temporal response of the ultraviolet airglow, and data from TIMED/GUVI is used to infer the vertical distribution of the airglow enhancement. We find that the airglow signature is well correlated with energetic atom precipitation. The ultraviolet emission has a maximum above 120 km tangent altitude and is dominated by OI 135.6 nm emission. The relative brightness of 135.6 nm emission and OI 130.4 nm radiance suggest a lack of an electron cascade. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP DeMajistre, R (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM robert.demajistre@jhuapl.edu RI Paxton, Larry/D-1934-2015; Brandt, Pontus/N-1218-2016 OI Paxton, Larry/0000-0002-2597-347X; Brandt, Pontus/0000-0002-4644-0306 NR 15 TC 7 Z9 7 U1 1 U2 5 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 AUG 12 PY 2005 VL 32 IS 15 AR L15105 DI 10.1029/2005GL023059 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 957OT UT WOS:000231380600003 ER PT J AU Agre, PC Altman, S Curl, RF Wiesel, TN West-Eberhard, MJ AF Agre, PC Altman, S Curl, RF Wiesel, TN West-Eberhard, MJ TI Using ethics to fight bioterrorism SO SCIENCE LA English DT Letter C1 Johns Hopkins Sch Med, Dept Biol Chem, Baltimore, MD 21205 USA. Yale Univ, Dept Mol Cellular & Dev Biol, New Haven, CT 06520 USA. Rice Univ, Dept Chem, Houston, TX 77005 USA. Rockefeller Univ, New York, NY 10021 USA. Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. RP Agre, PC (reprint author), Johns Hopkins Sch Med, Dept Biol Chem, 725 N Wolfe St, Baltimore, MD 21205 USA. NR 2 TC 0 Z9 0 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 12 PY 2005 VL 309 IS 5737 BP 1013 EP 1014 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 955MN UT WOS:000231230100017 ER PT J AU Hansen, FK Branchini, E Mazzotta, P Cabella, P Dolag, K AF Hansen, FK Branchini, E Mazzotta, P Cabella, P Dolag, K TI A full-sky prediction of the Sunyaev-Zeldovich effect from diffuse hot gas in the local universe and the upper limit from the WMAP data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; methods : statistical; techniques : image processing; cosmology : cosmic microwave background; cosmology : observations ID MICROWAVE BACKGROUND MAPS; DETECT NON-GAUSSIANITY; LARGE-SCALE STRUCTURE; CONSTRAINED SIMULATIONS; SPHERICAL WAVELETS; CROSS-CORRELATION; POWER-SPECTRUM; REAL UNIVERSE; COBE-DMR; SUPERCLUSTER AB We use the Point Source Catalogue Redshift Survey galaxy redshift catalogue combined with constrained simulations based on the IRAS 1.2-Jy galaxy density field to estimate the contribution of hot gas in the local universe to the Sunyaev-Zeldovich (SZ) effect on a large scale. We produce a full-sky HEALPIX map predicting the SZ effect from clusters as well as diffuse hot gas within 80 h(-1) Mpc. Performing cross-correlation tests between this map and the WMAP data in pixel, harmonic and wavelet space we can put an upper limit on the effect. We conclude that the SZ effect from diffuse gas in the local universe cannot be detected in current cosmic microwave background (CMB) data and is not a large-scale contaminating factor (l < 60) in studies of CMB angular anisotropies. We derive an upper limit for the mean temperature decrement of AT < 0.33 mu K at the 2 sigma confidence level for the 61-GHz frequency channel. However, for future high-sensitivity experiments observing at a wider range of frequencies, the predicted large-scale SZ effect could be of importance. C1 Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Univ Roma TRE, Dipartimento Fis, I-00146 Rome, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Hansen, FK (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. EM frodekh@astro.uio.no; branchin@fis.uniroma3.it; pasquale.mazzotta@roma2.infn.it; Paolo.Cabella@roma2.infn.it; kdolag@MPA-Garching.MPG.DE RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; Branchini, Enzo/0000-0002-0808-6908 NR 57 TC 21 Z9 21 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 AUG 11 PY 2005 VL 361 IS 3 BP 753 EP 762 DI 10.1111/j.1356-2966.2005.09210.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958AY UT WOS:000231418300001 ER PT J AU Springel, V Di Matteo, T Hernquist, L AF Springel, V Di Matteo, T Hernquist, L TI Modelling feedback from stars and black holes in galaxy mergers SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : active; galaxies : interactions; galaxies : starburst; galaxies : structure ID SMOOTHED PARTICLE HYDRODYNAMICS; DARK-MATTER HALOS; ULTRALUMINOUS INFRARED GALAXIES; REGION NEARBY SURVEY; INFALL REGION; GALACTIC NUCLEI; TIDAL TAILS; COSMOLOGICAL SIMULATIONS; INTERACTING GALAXIES; VELOCITY DISPERSION AB We describe techniques for incorporating feedback from star formation and black hole (BH) accretion into simulations of isolated and merging galaxies. At present, the details of these processes cannot be resolved in simulations on galactic scales. Our basic approach therefore involves forming coarse-grained representations of the properties of the interstellar medium (ISM) and BH accretion starting from basic physical assumptions, so that the impact of these effects can be included on resolved scales. We illustrate our method using a multiphase description of star-forming gas. Feedback from star formation pressurizes highly overdense gas, altering its effective equation of state (EOS). We show that this allows the construction of stable galaxy models with much larger gas fractions than possible in earlier numerical work. We extend the model by including a treatment of gas accretion onto central supermassive BHs in galaxies. Assuming thermal coupling of a small fraction of the bolometric luminosity of accreting BHs to the surrounding gas, we show how this feedback regulates the growth of BHs. In gas-rich mergers of galaxies, we observe a complex interplay between starbursts and central active galactic nuclei (AGN) activity when the tidal interaction triggers intense nuclear inflows of gas. Once an accreting supermassive BH has grown to a critical size, feedback terminates its further growth and expels gas from the central region in a powerful quasar-driven wind. Our simulation methodology is therefore able to address the coupled processes of gas dynamics, star formation and BH accretion during the formation of galaxies. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Springel, V (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM volker@mpa-garching.mpg.de; tiziana@mpa-garching.mpg.de; lars@cfa.harvard.edu RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 87 TC 1023 Z9 1025 U1 6 U2 26 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2005 VL 361 IS 3 BP 776 EP 794 DI 10.1111/j.1365-2966.2005.09238.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958AY UT WOS:000231418300003 ER PT J AU Broderick, AE AF Broderick, AE TI Supernovae in helium star-compact object binaries: a possible gamma-ray burst mechanism SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : close; pulsars : general; supemovae : general; gamma-rays : bursts ID NEUTRON-STARS; DISK ACCRETION; LIGHT CURVES; PULSAR WINDS; BLACK-HOLES; EVOLUTION; ENERGY; MODEL; AFTERGLOWS; JET AB Helium star-compact object binaries, and helium star-neutron star binaries in particular, are widely believed to be the progenitors of the observed double-neutron-star systems. In these, the second neutron star is presumed to be the compact remnant of the helium star supernova. In this paper, the observational implications of such a supernova are discussed, and in particular are explored as a candidate gamma-ray burst mechanism. In this scenario, the supernova results in a transient period of rapid accretion on to the compact object, extracting via magnetic torques its rotational energy at highly super-Eddington luminosities in the form of a narrowly beamed, strongly electromagnetically dominated jet. Compton scattering of supernova photons advected within the ejecta, and photons originating at shocks driven into the ejecta by the jet, will cool the jet and can produce the observed prompt emission characteristics, including the peak-inferred isotropic energy relation, X-ray flash characteristics, subpulse light curves, energy-dependent time lags and subpulse broadening, and late time spectral softening. The duration of the burst is limited by the rate of Compton cooling of the jet, eventually creating an optically thick, moderately relativistically expanding fireball that can produce the afterglow emission. If the black hole or neutron star stays bound to a compact remnant, late term light curve variability may be observed as in SN 2003dh. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM abroderick@cfa.harvard.edu NR 57 TC 9 Z9 9 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2005 VL 361 IS 3 BP 955 EP 964 DI 10.1111/j.1365-2966.2005.09220.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 958AY UT WOS:000231418300020 ER PT J AU Afshordi, N Lin, YT Sanderson, AJR AF Afshordi, N Lin, YT Sanderson, AJR TI Wilkinson microwave anisotropy probe constraints on the intracluster medium SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; dark matter; diffuse radiation; galaxies : clusters : general; radio continuum : galaxies; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; MASS-TEMPERATURE RELATION; NEARBY GALAXY CLUSTERS; SLOAN DIGITAL SKY; SCALING RELATIONS; WMAP OBSERVATIONS; DARK-MATTER; COSMOLOGICAL PARAMETERS; LUMINOSITY FUNCTION; HALO CONCENTRATIONS AB We devise a Monte Carlo-based, optimized filter match method to extract the thermal Sunyaev-Zel'dovich (SZ) signature of a catalog of 116 low-redshift X-ray clusters from the first-year data release of the Wilkinson Microwave Anisotropy Probe (WMAP). We detect an overall amplitude for the SZ signal at the similar to 8 sigma level, yielding a combined constraint of f(gas)h = 0.08 +/- 0.01(ran) +/- 0.01(sys) on the gas mass fraction of the intracluster medium. We also compile X-ray-estimated gas fractions from the literature for our sample and find that they are consistent with the SZ estimates at the 2 sigma level, while both show an increasing trend with X-ray temperature. Nevertheless, our SZ estimated gas fraction is 30%-40% smaller than the concordance Lambda CDM cosmic average. We also express our observations in terms of the SZ flux-temperature relation and compare it with other observations, as well as with numerical studies. Based on its spectral and spatial signature, we can also extract the microwave point-source signal of the clusters at the 3 sigma level, which puts the average microwave luminosity ( at similar to 41 GHz) of bright cluster members (M-K <= -21) at (2.4 +/- 0.8); 10(27) h(-2) ergs s(-1) Hz(-1). Furthermore, we can constrain the average dark matter halo concentration parameter to c(vir) 3/4(-0.9)(+0.6) for clusters with T-X > 5 keV. Our work serves as an example for how correlation of SZ surveys with cluster surveys at other frequencies can significantly increase our physical understanding of the intracluster medium. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. Princeton Univ, Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. 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 NR 84 TC 28 Z9 28 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 1 EP 14 DI 10.1086/431274 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600001 ER PT J AU Nevalainen, J Markevitch, M Lumb, D AF Nevalainen, J Markevitch, M Lumb, D TI XMM-Newton epic background modeling for extended sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual ( A1795); X-rays : galaxies ID GALAXY CLUSTERS; MAPS AB We use XMM-Newton blank-sky and closed-cover background data to explore background subtraction methods for large extended sources filling the EPIC field of view, such as nearby galaxy clusters, for which local background estimation is difficult. In particular, we investigate the uncertainties of the background modeling in the 0.8-7.0 keV band that affect cluster analyses. To model the background, we have constructed composite data sets from the blank-sky observations and compared them to the individual blank-sky observations to evaluate the modeling error. Our results apply to data obtained with thin and medium optical filters and in full frame and extended full frame modes. As expected, the modeling uncertainty is determined by how the EPIC background flares are filtered. We find that to keep this uncertainty tolerable, one has to use a much more restrictive filter than that commonly applied. In particular, because flares have highly variable spectra, not all of them are identified by filtering the E > 10 keV light curve. We tried using the outer part of the EPIC field of view for monitoring the background in a softer band (1-5 keV). We find that one needs to discard the time periods when either the hard-band or the soft-band rate exceeds the nominal value by more than 20% in order to limit the 90% CL background uncertainty to between +/- 5% at E = 4-7 keV and +/- 20% at E = 0.8-1 keV, for both MOS and PN. This compares to a 10%-30% respective PN uncertainty when only the hard-band light curve is used for filtering, and to a 15%-45% PN uncertainty when applying the commonly used 2-3 sigma filtering method. Adding such a soft-band filter on average results in only a 5%-10% reduction of the useful exposure time. We illustrate our method on the nearby cluster A1795. The above background uncertainties convert into systematic temperature uncertainties between about +/- 1% at r = 3'-4' and +/- 20%-25% (about +/- 1 keV for A1795) at r = 10'-15'. For comparison, the commonly applied 2-3 sigma clipping of the hard-band light curve misses a significant number of flares, rendering the temperatures beyond r 100 unconstrained. Thus, the background uncertainties do not prohibit the EPIC temperature profile analysis of low-brightness regions, such as outer regions of galaxy clusters, provided a conservative flare filtering such as the double-filtering method with +/- 20% limits is used. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Helsinki, Observatory, FIN-00014 Helsinki, Finland. Space Res Inst IKI, Moscow 117997, Russia. European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. RP Nevalainen, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 19 TC 56 Z9 56 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 AUG 10 PY 2005 VL 629 IS 1 BP 172 EP 191 DI 10.1086/431198 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600017 ER PT J AU Teixeira, PS Lada, CJ Alves, JF AF Teixeira, PS Lada, CJ Alves, JF TI From dusty filaments to cores to stars: An infrared extinction study of Lupus 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust,extinction; infrared : ISM; ISM : clouds; stars : formation ID SOUTHERN DARK CLOUDS; HERBIG-HARO OBJECTS; MOLECULAR CLOUDS; CORONA-AUSTRALIS; ALPHA ABSORPTION; FORMING REGIONS; IMAGING SURVEY; LOW-MASS; IC 5146; GAS AB We present deep near-infrared observations of a dense region of the Lupus 3 cloud obtained with the ESO NTT and VLT. Using the NICE method, we construct a detailed high angular resolution dust extinction map of the cloud. The dust extinction map reveals embedded globules, a dense filament, and a dense ring structure. We derive dust column densities and masses for the entire cloud and for the individual structures therein. We construct radial extinction profiles for the embedded globules and find a range of profile shapes from relatively shallow profiles for cores with low peak extinctions, to relatively steep profiles for cores with high extinction. Overall, the profiles are similar to those of pressure-truncated isothermal spheres of varying center-to-edge density contrast. We apply Bonnor-Ebert analysis to compare the density profiles of the embedded cores in a quantitative manner and derive physical parameters such as temperatures, central densities, and external pressures. We examine the stability of the cores and find that two cores are likely stable and two are likely unstable. One of these latter cores is known to harbor an active protostar. Finally, we discuss the relation between an emerging cluster in the Lupus 3 cloud and the ring structure identified in our extinction map. Assuming that the ring is the remnant of the core within which the cluster originally formed, we estimate that a star formation efficiency of similar to 30% characterized the formation of the small cluster. Our observations of the Lupus 3 cloud suggest an intimate link between the structure of a dense core and its state of star-forming activity. The dense cores in this cloud are found to span the entire range of evolution from a stable, starless core of modest central concentration, to an unstable, star-forming core that is highly centrally concentrated, to a significantly disrupted core from which a cluster of young stars is emerging. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. RP Teixeira, PS (reprint author), Univ Lisbon, Fac Ciencias, Dept Fis, P-1200 Lisbon, Portugal. EM pteixeira@cfa.harvard.edu; clada@cfa.harvard.edu; jalves@eso.org RI Teixeira, Paula Stella/O-2289-2013; OI Teixeira, Paula Stella/0000-0002-3665-5784; Alves, Joao/0000-0002-4355-0921 NR 38 TC 38 Z9 38 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 276 EP 287 DI 10.1086/430849 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600026 ER PT J AU Kohri, K Narayan, R Piran, T AF Kohri, K Narayan, R Piran, T TI Neutrino-dominated accretion and supernovae SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; neutrinos; supernovae : general ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; ROTATING MASSIVE STARS; R-PROCESS NUCLEOSYNTHESIS; DRIVEN WINDS; 3 DIMENSIONS; MAGNETOHYDRODYNAMIC SIMULATIONS; PRESUPERNOVA EVOLUTION; ASYMMETRIC SUPERNOVAE; II SUPERNOVAE AB We suggest that part of the infalling material during the core collapse of a massive star goes into orbit around the compact core to form a hot, dense, centrifugally supported accretion disk whose evolution is strongly influenced by neutrino interactions. Under a wide range of conditions, this neutrino-dominated accretion flow will be advection dominated and will develop a substantial outflowing wind. We estimate the energy carried out in the wind and find that it exceeds 10(50) ergs for a wide range of parameters and even exceeds 10(51) ergs for reasonable parameter choices. We propose that the wind energy will revive a stalled shock and will help produce a successful supernova explosion. We discuss the role of the disk wind in both prompt and delayed explosions. While both scenarios are feasible, we suggest that a delayed explosion is more likely and perhaps even unavoidable. Finally, we suggest that the disk wind may be a natural site for r-process nucleosynthesis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. CALTECH, Pasadena, CA 91125 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kkohri@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 91 TC 106 Z9 108 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 AUG 10 PY 2005 VL 629 IS 1 BP 341 EP 361 DI 10.1086/431354 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600033 ER PT J AU Afshordi, N Mukhopadhyay, B Narayan, R AF Afshordi, N Mukhopadhyay, B Narayan, R TI Bypass to turbulence in hydrodynamic accretion: Lagrangian analysis of energy growth SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; hydrodynamics; instabilities; turbulence ID TRANSIENT GROWTH; SHEAR TURBULENCE; KEPLERIAN DISKS; COUETTE-FLOW; INSTABILITY; STABILITY; TRANSPORT; TRANSITION; DYNAMICS AB Despite observational evidence for cold neutral astrophysical accretion disks, the viscous process that may drive the accretion in such systems is not yet understood. While molecular viscosity is too small to explain the observed accretion efficiencies by more than 10 orders of magnitude, the absence of any linear instability in Keplerian accretion flows is often used to rule out the possibility of turbulent viscosity. Recently, the fact that some fine-tuned disturbances of any inviscid shear flow can reach arbitrarily large transient growth has been proposed as an alternative route to turbulence in these systems. We present an analytic study of this process for three-dimensional plane wave disturbances of a general rotating shear flow in Lagrangian coordinates and demonstrate that large transient growth is a generic feature of nonaxisymmetric disturbances with near radial leading wavevectors. The maximum energy growth is slower than quadratic but faster than linear in time. The fastest growth occurs for two-dimensional perturbations and is only limited by viscosity, and ultimately by the disk vertical thickness. After including viscosity and vertical structure, we find that, as a function of the Reynolds number R, the maximum energy growth is approximately 0.4(R/ log R)(2/3) and put forth a heuristic argument for why R greater than or similar to 10(4) is required to sustain turbulence in Keplerian disks. Therefore, assuming that there exists a nonlinear feedback process to replenish the seeds for transient growth, astrophysical accretion disks must be well within the turbulent regime. However, large three-dimensional numerical simulations running for many orbital times, and/or with fine-tuned initial conditions, are required to confirm Keplerian hydrodynamic turbulence on the computer. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 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; bmukhopadhyay@cfa.harvard.edu; narayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 28 TC 44 Z9 44 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 AUG 10 PY 2005 VL 629 IS 1 BP 373 EP 382 DI 10.1086/431418 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600035 ER PT J AU Mukhopadhyay, B Afshordi, N Narayan, R AF Mukhopadhyay, B Afshordi, N Narayan, R TI Bypass to turbulence in hydrodynamic accretion disks: An eigenvalue approach SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; hydrodynamics; instabilities; turbulence ID WEAKLY MAGNETIZED DISKS; VISCOUS SHEAR-FLOW; TRANSIENT GROWTH; KEPLERIAN DISKS; DENSITY WAVES; COUETTE-FLOW; BLACK-HOLES; STABILITY; INSTABILITY; PERTURBATIONS AB Cold accretion disks with temperatures below similar to 3000 K are likely to be composed of highly neutral gas. The magnetorotational instability may cease to operate in such disks, so it is of interest to consider purely hydrodynamic mechanisms of generating turbulence and angular momentum transport. With this motivation, we investigate the growth of hydrodynamic perturbations in a linear shear flow sandwiched between two parallel walls. The unperturbed flow is similar to plane Couette flow, but with a Coriolis force included. Although there are no exponentially growing eigenmodes in this system, nevertheless, because of the nonnormal nature of the eigenmodes, it is possible to have a large transient growth in the energy of perturbations. For a constant angular momentum disk, we find that the perturbation with maximum growth is axisymmetric with vertical structure. The energy grows by more than a factor of 100 for a Reynolds number R = 300 and more than a factor of 1000 for R = 1000. Turbulence can be easily excited in such a disk, as found in previous numerical simulations. For a Keplerian disk, on the other hand, similar perturbations with vertical structure grow by no more than a factor of 4, explaining why the same simulations did not find turbulence in this system. However, certain other two-dimensional perturbations with no vertical structure do exhibit modest growth. For the optimum two-dimensional perturbation, the energy grows by a factor of similar to 100 for R similar to 10(4.5) and by a factor of 1000 for R similar to 10(6). Such large Reynolds numbers are hard to achieve in numerical simulations, and so the nonlinear development of these kinds of perturbations is only beginning to be investigated. It is conceivable that these nearly two-dimensional disturbances might lead to self-sustained three-dimensional turbulence, although this remains to be demonstrated. The Reynolds numbers of cold astrophysical disks are much larger even than 10(6); therefore, hydrodynamic turbulence may be possible in disks through transient growth. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Mukhopadhyay, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM bmukhopa@cfa.harvard.edu; nafshord@cfa.harvard.edu; rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 47 TC 49 Z9 49 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 AUG 10 PY 2005 VL 629 IS 1 BP 383 EP 396 DI 10.1086/431419 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600036 ER PT J AU Cooper, RL Narayan, R AF Cooper, RL Narayan, R TI Theoretical models of superbursts on accreting neutron stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE dense matter; nuclear reactions, nucleosynthesis, abundances; stars : neutron; X-rays : binaries; X-rays : bursts ID X-RAY-BURSTS; THERMONUCLEAR REACTION-RATES; CARBON FLASHES; DENSE MATTER; WHITE-DWARFS; INNER CRUST; 4U 1636-53; RP-PROCESS; LOW-MASS; EVOLUTION AB We carry out a general relativistic global linear stability analysis of the amassed carbon fuel on the surface of an accreting neutron star to determine the conditions under which superbursts occur. We reproduce the general observational characteristics of superbursts, including burst fluences, recurrence times, and the absence of superbursts on stars with accretion rates (M) over dot < 0.1. (M) over dot (Edd), where (M) over dot(Edd) denotes the Eddington limit. By comparing our results with observations, we are able to set constraints on neutron star parameters such as the stellar radius and neutrino cooling mechanism in the core. Specifically, we find that accreting neutron stars with ordered crusts and highly efficient neutrino emission in their cores ( due to direct Urca or pionic reactions, for example) produce extremely energetic (> 10(44) ergs) superbursts that are inconsistent with observations, in agreement with previous investigations. Also, because of pycnonuclear burning of carbon, they do not have superbursts in the range of accretion rates at which superbursts are actually observed unless the crust is very impure. Stars with less efficient neutrino emission ( due to modified Urca reactions, for example) produce bursts that agree better with observations. Stars with highly inefficient neutrino emission in their cores produce bursts that agree best with observations. Furthermore, we find that neutron stars with large radii ( R similar to 16 km) produce very energetic superbursts that conflict with observations, even if the core neutrino emission mechanism is highly inefficient. Superburst characteristics are quite sensitive to several other parameters as well, most notably the composition of the accreted gas, concentration of carbon in the ignition region, and degree of crystallization of the crust. All systems that accrete primarily hydrogen and in which superbursts are observed show evidence of H- and He-burning delayed mixed bursts. We speculate that delayed mixed bursts provide sufficient amounts of carbon fuel for superbursts and are thus a prerequisite for having superbursts. We compare our global stability analysis to approximate one-zone criteria used by other authors and identify a particular set of approximations that give accurate results for most choices of parameters. 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 68 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 422 EP 437 DI 10.1086/431273 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600041 ER PT J AU Lin, J van Ballegooijen, AA AF Lin, J van Ballegooijen, AA TI Equilibrium and evolution in multipolar magnetic configurations resulting from interactions among active regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun : activity; Sun : filaments; Sun : magnetic fields ID CORONAL MASS EJECTIONS; FLUX-ROPE MODELS; SOLAR PROMINENCES; ERUPTIVE FLARES; QUIESCENT PROMINENCES; HEMISPHERIC PATTERN; FILAMENT CHANNELS; CURRENT SHEETS; FORCE-FREE; FIELDS AB The evolution of magnetic configurations with a current-carrying flux rope for modeling a prominence is investigated. The configurations evolve as a result of the interaction between two or more magnetic source regions. The background field of the system is produced by either two dipoles or four monopoles located on the boundary surface. Our purpose is to study the catastrophic behaviors of the systems' evolutions in response to the change in either the distance between source regions or the strength of background field, and to find the maximum heights that the flux rope can attain before it loses equilibrium and catastrophe occurs. We find that the domain in parameter space over which the flux rope remains in equilibrium is smaller than in the simpler configurations that have been previously investigated. Consequently, the equilibrium heights of the flux rope studied in this work are fairly low, such that the maximum values of these heights compared to the corresponding distances between the active regions vary from less than 3% to about 23%, with an average of about 13.2%, all of which are below 25%. This result has an important observational consequence, namely that a prominence appearing between different active regions will tend to be located in the low corona and will tend to become unstable if its height increases. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI LIN, JUN/B-9890-2017; OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 56 TC 13 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP 582 EP 591 DI 10.1086/431352 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JK UT WOS:000230999600055 ER PT J AU Esser, R Lie-Svendsen, O Janse, AM Killie, MA AF Esser, R Lie-Svendsen, O Janse, AM Killie, MA TI Solar wind from coronal funnels and transition region Ly alpha SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : corona; Sun : transition region ID TRANSPORT-EQUATIONS; PHYSICAL-PROPERTIES; HOLES; CHROMOSPHERE; OUTFLOW; NETWORK; HELIUM; ORIGIN; MODEL; LINES AB Using a newly developed gyrotropic solar wind model that extends continuously from the mid-chromosphere to 1 AU and that accounts for radiative losses in the transition region, we have studied the difference between the fast solar wind emanating from a funnel geometry and a "traditional" rapidly expanding wind. The main aim is to determine whether or not observations of the Ly alpha intensity in the low transition region can be reconciled with solar wind models. In a rapidly expanding geometry, we are not able to produce a Ly alpha intensity much higher than 1/10 of the observed values without creating a large pressure in the transition region and, as a result, a mass flux much higher than observed. In a funnel, on the other hand, we can easily obtain the observed Ly alpha intensity, while still having a wind solution in agreement with observations. The main reason for this is that the fast flow in the funnel causes hydrogen to be very far from ionization equilibrium, with the Ly alpha intensity coming from temperatures of about 5 x 10(4) K. At these elevated temperatures, the radiative loss is much more efficient. The results of this Letter support the idea that the solar wind originates from small coronal funnels. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Norwegian Def Res Estab, N-2027 Kjeller, Norway. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. RP Esser, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM resser@cfa.harvard.edu; oystein.lie-svendsen@ffi.no; a.m.janse@astro.uio.no; m.a.killie@astro.ui.no NR 33 TC 17 Z9 18 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 AUG 10 PY 2005 VL 629 IS 1 BP L61 EP L64 DI 10.1086/444497 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JN UT WOS:000230999900016 ER PT J AU Gaudi, BS Stanek, KZ Hartman, JD Holman, MJ McLeod, BA AF Gaudi, BS Stanek, KZ Hartman, JD Holman, MJ McLeod, BA TI On the rotation period of (90377) Sedna SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper Belt; minor planets; asteroids; Oort Cloud; solar system : general ID 2003 VB12 SEDNA; IMAGE SUBTRACTION; SLOW ROTATION; SPACED DATA; OBJECTS; ORBITS; PHOTOMETRY; ASTEROIDS; ORIGIN AB We present precise, similar to 1%, r-band relative photometry of the unusual solar system object ( 90377) Sedna. Our data consist of 143 data points taken over eight nights in 2004 October and 2005 January 2005. The rms variability over the longest contiguous stretch of five nights of data spanning 9 days is only similar to 1.3%. This subset of data alone constrains the amplitude of any long-period variations with period P to be A less than or similar to 1%(P/20 days)(2). Over the course of any given similar to 5 hr segment, the data exhibit significant linear trends not seen in a comparison star of similar magnitude, and in a few cases these segments show clear evidence of curvature at the level of a few millimagnitudes per hour squared. These properties imply that the rotation period of Sedna is O(10 hr); it cannot be less than or similar to 5 hr nor can it be greater than or similar to 10 days, unless the intrinsic light curve has significant and comparable power on multiple timescales, which is unlikely. A sinusoidal fit yields a period of and a semiamplitude P = 10.273 +/- 0.002 hr and a semiamplitude of A = 1.1% +/- 0.1%. There are additional acceptable fits with flanking periods separated by similar to 3 minutes as well as another class of fits with, although these later fits appear less viable based on visual inspection. P similar to 18 hr Our results indicate that the period of Sedna is likely consistent with typical rotation periods of solar system objects, thus obviating the need for a massive companion to slow its rotation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaudi, BS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sgaudi@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012; OI Hartman, Joel/0000-0001-8732-6166 NR 18 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2005 VL 629 IS 1 BP L49 EP L52 DI 10.1086/444355 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JN UT WOS:000230999900013 ER PT J AU Risaliti, G Elvis, M AF Risaliti, G Elvis, M TI The SDSS/XMM-Newton quasar sample. I. First results SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; X-rays : galaxies ID DIGITAL SKY SURVEY; X-RAY OBSERVATIONS; RADIO-QUIET QUASARS; REDSHIFT QUASARS; EMISSION; CHANDRA; GALAXIES; ASCA; ABSORPTION; RELEASE AB We have searched in the XMM-Newton public archive for quasars in the Sloan Digital Sky Survey First Data Release and found 55 lying in the field of an XMM-Newton observation with exposure times >20 ks (as of 2004 August). The 35 quasars that yielded good X-ray spectra span redshifts from 0.5 to 2.5. The large collecting area of XMM-Newton allows us to investigate the dependence of the X-ray spectra of quasars on luminosity, redshift, and optical colors. We find ( 1) no evolution of X-ray slope (Gamma) with either redshift or luminosity; ( 2) no correlation between G ( or absorbing column density) and the optical - to - X-ray ratio, alpha(OX); and (4) no relation between alpha(OX) and optical colors. The two latter results suggest that obscuration is not the dominant cause of the spread in X-ray slope or optical color. We find four unusual quasars (i.e., 10% of the sample): three are absorbed (N-H > 10(22) cm(-2)), of which one has high luminosity (1.5 x 10(44) ergs s(-1)); the fourth has Gamma = 0.6 +/- 0.2 which is far flatter than the typical value of 1.8 - 2.0, and a strong emission line (EW = 1.2 +/- 0.4 keV), which, if Fe K, implies a redshift of similar to 1.4. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), INAF, Osservatorio Astron Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM grisaliti@cfa.harvard.edu OI Risaliti, Guido/0000-0002-3556-977X NR 33 TC 14 Z9 14 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 AUG 10 PY 2005 VL 629 IS 1 BP L17 EP L20 DI 10.1086/444413 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 952JN UT WOS:000230999900005 ER PT J AU Pogue, MG AF Pogue, MG TI The Plusiinae (Lepidoptera : Noctuidae) of Great Smoky Mountains National Park SO ZOOTAXA LA English DT Article DE systematics; All Taxa Biodiversity Inventory; North Carolina; Tennessee; moths AB Seventeen species of Plusiinae have been found in Great Smoky Mountains National Park, in Tennessee and North Carolina, USA. These species are documented with adult images, description, flight period, abundance, elevation range, Park and general distribution, and larval hosts from the literature. Maps illustrate the known distribution of each species within the Park. Sixteen of the 17 species occur above 4,000 feet in elevation. The most diverse locality in the Park has 14 species. C1 Smithsonian Inst, Systemat Entomol Lab,PSI, ARS, USDA, Washington, DC 20013 USA. RP Pogue, MG (reprint author), Smithsonian Inst, Systemat Entomol Lab,PSI, ARS, USDA, POB 37012,NMNH,MRC-168, Washington, DC 20013 USA. EM mpogue@sel.barc.usda.gov NR 10 TC 8 Z9 9 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 AUG 8 PY 2005 IS 1032 BP 1 EP 28 PG 28 WC Zoology SC Zoology GA 953UX UT WOS:000231107400001 ER PT J AU Smith, ABT Evans, AV AF Smith, ABT Evans, AV TI A supplement to the checklist of the New World chafers (Coleoptera : Scarabaeidae : Melolonthinae) with notes on their tribal classification SO ZOOTAXA LA English DT Article DE Coleoptera; Scarabaeidae; Melolonthinae; chafers; New World ID ADULT SCARABAEOIDEA COLEOPTERA; PHYLOGENETIC SIGNIFICANCE; REVISION; GENUS; SPIRACLES; GENERA; MEXICO AB The checklist of the New World Melolonthinae published in 2003 by Evans is updated to 30 June 2005. Corrections and omissions to the previous checklist are also noted and necessary taxonomic changes are made. Melolontha elongata Fabricius, 1792 is designated as the type species of Philochloenia Dejean, 1833, syn. nov. thereby placing this genus as a junior synonym of Dichelonyx Harris, 1827. Phyllophaga guatemalica ( Moser, 1918), syn. nov. and Phyllophaga longiclava ( Moser, 1918), syn. nov. are placed in synonymy with Phyllophaga ravida ( Blanchard, 1851). The Australian genus Deuterocaulobius Dalla Torre, 1912, stat. nov. is brought out of synonymy and considered the valid name for "Phyllochlaenia Blanchard, 1846." Warwickia, nom. nov. is proposed as a replacement name for the junior homonym Benedictia Sanderson, 1939 ( non Dybowski, 1875) and consequently, Warwickia pilosa ( Sanderson, 1939), comb. nov. is a new combination for the single species in this genus. A brief overview of the tribal classification of Melolonthinae is presented. C1 Canadian Museum Nat, Div Res, Ottawa, ON K1P 6P4, Canada. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Virginia Museum Nat Hist, Dept Recent Invertebrates, Richmond, VA 23227 USA. RP Smith, ABT (reprint author), Canadian Museum Nat, Div Res, POB 3443,Stn D, Ottawa, ON K1P 6P4, Canada. EM asmith@mus-nature.ca; arthurevans@verizon.net NR 98 TC 10 Z9 13 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 AUG 8 PY 2005 IS 1032 BP 29 EP 60 PG 32 WC Zoology SC Zoology GA 953UX UT WOS:000231107400002 ER PT J AU Hilton, EJ Kley, NJ AF Hilton, EJ Kley, NJ TI Osteology of the quillfish, Ptilichthys goodei (Perciformes : Zoarcoidei : Ptilichthyidae) SO COPEIA LA English DT Article AB The Quillfish, Ptilichthys goodei, is a slender, elongate fish distributed along the coastline of the North Pacific from Oregon to the Sea of Japan. It is the sole member of the monotypic family Ptilichthyidae, which is classified among the Zoarcoidei (eelpouts and their allies). Little is known of its osteology and there is much conflicting information in the literature regarding its morphology. In this paper we describe the skeleton of Ptilichthys based on newly collected and prepared specimens. Because of the small number and size range of our specimens, the emphasis of our study is on the juvenile skeleton, although the adult skeleton is also described as far as our material allows. We conclude by briefly discussing the phenomenon of axial elongation in Ptilichthys. C1 Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. SUNY Stony Brook, Ctr Hlth Sci, Dept Anat Sci, Stony Brook, NY 11794 USA. RP Hilton, EJ (reprint author), Smithsonian Inst, Div Fishes, POB 37012,NMNH,MRC 0159, Washington, DC 20013 USA. EM Hilton.Eric@nmnh.si.edu; Nathan.Kley@stonybrook.edu NR 48 TC 9 Z9 11 U1 0 U2 1 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD AUG 2 PY 2005 IS 3 BP 571 EP 585 PG 15 WC Zoology SC Zoology GA 952WD UT WOS:000231035500012 ER PT J AU Hilton, EJ Bemis, WE AF Hilton, EJ Bemis, WE TI Grouped tooth replacement in the oral jaws of the tripletail, Lobotes surinamensis (Perciformes : Lobotidac), with a discussion of its proposed relationship to Datnioides SO COPEIA LA English DT Article ID PHYLOGENY AB Lobotes surinamensis is a widely distributed marine perciform and is the sole member of the family Lobotidae, which has unclear phylogenetic affinities. In this paper we describe and illustrate a mode of tooth replacement in Lobotes that we name "grouped" tooth replacement. Lateral oral teeth are replaced intraosseously, i.e., developing replacement teeth can clearly be seen beneath them within both the dentary and premaxillary bones. In contrast to the more typically seen pattern of alternate replacement, the replacement teeth of Lobotes develop as a group within the bone, lying directly beneath the group of teeth that they win replace. Within each tooth replacement group, the teeth show an anteroposterior gradient in age. Within the category of fully functional teeth there is a clear anterior to posterior gradient of eruption within a tooth group. Grouped tooth replacement may be a synapomorphy of Lobotes and Datnioides. As in Lobotes, the lateral oral teeth of Datnioides also are replaced intraosseously and in groups, although they are smaller and the groups are neither as distinct nor as regular. The significance and polarity of this character, as well as other osteological similarities of Lobotes and Datnioides, are difficult to evaluate given the lack of understanding of higher level relationships among perciforms and the paucity of information about modes of their tooth replacement. C1 Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. RP Hilton, EJ (reprint author), Smithsonian Inst, Div Fishes, POB 37012,NMNH Rm WG-12,MRC 0159, Washington, DC 20013 USA. EM Hilton.Eric@nmnh.si.edu; web24@cornell.edu NR 26 TC 3 Z9 3 U1 3 U2 6 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 AUG 2 PY 2005 IS 3 BP 665 EP 672 PG 8 WC Zoology SC Zoology GA 952WD UT WOS:000231035500022 ER PT J AU Collette, BB Smith, DG AF Collette, BB Smith, DG TI William Ralph Taylor - 1919-2004 - Obituary SO COPEIA LA English DT Biographical-Item C1 Museum Natl Hist Nat, Nalt Marine Fisheries Serv Systemat Lab, Smithsonian Inst, Washington, DC USA. Museum Natl Hist Nat, Div Fishes, Smithsonian Inst, Washington, DC USA. RP Collette, BB (reprint author), Museum Natl Hist Nat, Nalt Marine Fisheries Serv Systemat Lab, Smithsonian Inst, POB 37012,MRC-153, Washington, DC USA. EM collettb@si.edu; smithd@si.edu NR 1 TC 1 Z9 1 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD AUG 2 PY 2005 IS 3 BP 709 EP 711 DI 10.1643/OT-05-035 PG 3 WC Zoology SC Zoology GA 952WD UT WOS:000231035500028 ER PT J AU Dick, CW Wright, SJ AF Dick, CW Wright, SJ TI Tropical mountain cradles of dry forest diversity SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID DIVERSIFICATION; HISTORY; ORIGIN C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Michigan, Herbarium, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Ecol & Evolut, Ann Arbor, MI 48109 USA. RP Dick, CW (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM dickc@si.edu RI Dick, Christopher/A-8744-2008; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 18 TC 11 Z9 11 U1 0 U2 3 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 AUG 2 PY 2005 VL 102 IS 31 BP 10757 EP 10758 DI 10.1073/pnas.0505013102 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 953TC UT WOS:000231102400001 PM 16046534 ER PT J AU Wurdack, KJ Hoffmann, P Chase, MW AF Wurdack, KJ Hoffmann, P Chase, MW TI Molecular phylogenetic analysis of uniovulate Euphorbiaceae (Euphorbiaceae sensu stricto) using plastid rbcL and trnL-F DNA sequences SO AMERICAN JOURNAL OF BOTANY LA English DT Review DE Cheilosoideae; Euphorbiaceae; malpighiales; molecular phylogenetics; morphology; Peroideae ID NONCODING CHLOROPLAST DNA; ACALYPHOIDEAE EUPHORBIACEAE; POLLEN MORPHOLOGY; FLOWERING PLANTS; EXINE STRUCTURE; SYSTEMATIC IMPLICATIONS; PRO PARTE; CROTONOIDEAE EUPHORBIACEAE; HIPPOMANEAE EUPHORBIACEAE; SPECIES EUPHORBIACEAE AB Parsimony and Bayesian analyses of plastid rbcL and trnL-F DNA sequence data of the pantropical family Euphorbiaceae sensu stricto (s.s.) are presented. Sampling includes representatives of all three Subfamilies (Acalyphoideae, Crotonoideae, and Euphorbioideae), 35 of 37 tribes and 179 of the 247 genera of uniovulate Euphorbiaceae sensu lato (s.l.). Euphorbiaceae s.s. were recovered as a monophyletic group with no new adjustments in circumscription. Two clades containing taxa previously placed in Acalyphoideae are found to be Successive sisters to all other Euphorbiaceae s.s. and ire proposed here at subfumilial rank as Peroideae and Cheilo-soideae. The remainder of the family fall into seven major lineages including Erismantheae and Acalyphoideae s.s. (parts of Acalyphoideae), Adenoclineae s.l.. Gelonieae, articulated crotonoids and inaperturate crotonoids (parts of Crotonoideae), and Euphorbioideae. Potential synapomorphics and biogeographical trends are suggested for these clades. Acalyphoideae s.s., inaperturate crotonoids, and Euphorbioideae tribe Hippomaneae each have two major subclades that represent novel groupings without apparent morphological synapomorphies. Two subfamilies, 14 tribes, and 10 genera were found to be para- or polyphyletic. Noteworthy among these, Omphaleae are embedded in Adenoclineae, Hureae + Pachystromateae in Hippomaneae, Ditta in Tetrorchidium, and Sapium s.s. in Stillingia. C1 Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. Royal Bot Gardens, Herbarium, Richmond TW9 3AB, Surrey, England. Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. RP Wurdack, KJ (reprint author), Smithsonian Inst, Dept Bot, POB 37012, Washington, DC 20013 USA. EM kwurdack@lab.si.edu RI Chase, Mark /A-6642-2011 NR 184 TC 133 Z9 162 U1 3 U2 16 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 AUG PY 2005 VL 92 IS 8 BP 1397 EP 1420 DI 10.3732/ajb.92.8.1397 PG 24 WC Plant Sciences SC Plant Sciences GA 950UC UT WOS:000230882500018 PM 21646159 ER PT J AU Hunt, DR Albanese, J AF Hunt, DR Albanese, J TI History and demographic composition of the Robert J. Terry anatomical collection SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE history of physical anthropology; history of human skeletal collections; Hamann-Todd collection; Huntington collection ID PHYSICAL-ANTHROPOLOGY; SEX DETERMINATION; HUMAN SKELETONS; RACE CONCEPT; BLIND TESTS; ASH WEIGHT; DEATH; AGE; STATURE; BONES AB Robert J. Terry began collecting human skeletal remains in the area of St. Louis, Missouri for research and educational purposes in 1898. He continued collecting skeletal specimens in the Anatomy Department at Washington University until his retirement in 1941. Mildred Trotter succeeded Terry as anatomy professor and continued his collecting, and strove to balance the demographic distribution of the collection. In 1967, after her retirement, the collection was moved to the Smithsonian Institution's National Museum of Natural History. As with several other well-documented collections, the Terry Collection is widely used for a diverse range of anthropological and medical research. Despite its extensive use, there has been limited discussion of the collection's history and incomplete description of holdings and associated materials of this collection. In this paper, the historical background of the collection and the collection process is described; the demographic composition of the collection, and a description of the documentary and supporting data are presented; and the quality and of these data are assessed. The Terry Collection consists of 1,728 individuals. Age at death ranges from 14-102 years, with the majority of the individuals ranging from 20-80 years. Year of birth ranges from 1828-1943; the mean year of birth for males is 1880, and for females it is 1884. The mean age at death for males is 53 years, and for females it is 58 years. Terry's strict protocols for the processing of cadavers and the recording of documentary data make the Terry Collection a valuable resource for anthropological and medical research. (c) 2004 Wiley-Liss, Inc. C1 Natl Museum Nat Hist, Dept Anthropol, Phys Anthropol Div, Smithsonian Inst, Washington, DC 20560 USA. Univ Toronto, Dept Anthropol, Toronto, ON M5S 3G3, Canada. RP Hunt, DR (reprint author), Natl Museum Nat Hist, Dept Anthropol, Phys Anthropol Div, Smithsonian Inst, MRC 112, Washington, DC 20560 USA. EM HUNT.DAVID@NMNH.SI.EDU NR 56 TC 71 Z9 74 U1 1 U2 8 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD AUG PY 2005 VL 127 IS 4 BP 406 EP 417 DI 10.1002/ajpa.20135 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 947RO UT WOS:000230664100004 PM 15624209 ER PT J AU Dupuis, AP Marra, PP Reitsma, R Jones, MJ Louie, KL Kramer, LD AF Dupuis, AP Marra, PP Reitsma, R Jones, MJ Louie, KL Kramer, LD TI Short report: Serologic evidence for West Nile virus transmission in Puerto Rico and Cuba SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID CROSS-NEUTRALIZATION; BIRDS; INFECTION; STATE; FLAVIVIRUSES; ARBOVIRUSES; HORSES; MEXICO AB During the spring of 2004, approximately 1,950 blood specimens were collected from resident and Nearctic-Neotropical migratory birds on the Caribbean islands of Puerto Rico and Cuba prior to northerly spring migrations. Eleven birds and seven birds, collected in Puerto Rico and Cuba, respectively, showed evidence of antibody in a flavivirus enzyme-linked immunosorbent assay. Confirmatory plaque-reduction neutralization test results indicated neutralizing antibodies to West Nile virus in non-migratory resident birds from Puerto Rico and Cuba, which indicated local transmission. C1 New York State Dept Hlth, Wadsworth Ctr, Arbovirus Labs, Slingerlands, NY 12159 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Dupuis, AP (reprint author), New York State Dept Hlth, Wadsworth Ctr, Arbovirus Labs, 5668 State Farm Rd, Slingerlands, NY 12159 USA. EM dupuis@wadsworth.org; marrap@si.edu FU ODCDC CDC HHS [U50/CCU320544-01] NR 20 TC 40 Z9 47 U1 0 U2 3 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD AUG PY 2005 VL 73 IS 2 BP 474 EP 476 PG 3 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 956BA UT WOS:000231272700048 PM 16103626 ER PT J AU Derivera, CE AF Derivera, CE TI Long searches for male-defended breeding burrows allow female fiddler crabs, Uca crenulata, to release larvae on time SO ANIMAL BEHAVIOUR LA English DT Article ID MATE CHOICE; PREDATION RISK; GASTEROSTEUS-ACULEATUS; ADAPTIVE SIGNIFICANCE; MATING SYSTEM; PUGILATOR; BEHAVIOR; COSTS; SEX; STICKLEBACKS AB When individuals benefit from highly selective mate choice and search costs are negligible, they should sample all or at least many potential mates. Most animals sample just a few mates, presumably because search costs override the benefits of lengthy searches. Observations on mate-searching female California fiddler crabs, Uca crenulata, showed that these crabs conducted much longer searches than have been reported for other animals. Moreover, large and small females used different sampling strategies. Searches may be long in this species because females use multiple criteria to select mates and benefit from finding a burrow of the right size. They chose mates that (1) were near to their size (2) had small claws given their body size, and (3) defended long burrows with entrances that matched the size of the female. Females sampled many burrows that did not match their size, indicating that they assessed burrows on contact and not before. An experiment examining why females use male burrow diameter as a mate choice criteria revealed that burrow opening diameter, or a correlate, affected incubation duration and therefore release time of larvae. Larvae were successfully released during high-amplitude nocturnal tides only when females incubated in burrows that allowed the larvae to exit the estuary swiftly and thus reduce predation risk, but not when females incubated in burrows that were too wide or narrow. The effect of burrow aperture on incubation duration may explain why females sampled many male burrows as they searched for a mate and why females of different size classes selected and sampled differently. C1 Univ Calif San Diego, Dept Biol, San Diego, CA 92103 USA. RP Derivera, CE (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM deriverac@si.edu NR 43 TC 41 Z9 42 U1 4 U2 14 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 2005 VL 70 BP 289 EP 297 DI 10.1016/j.anbehav.2004.10.027 PN 2 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 952NM UT WOS:000231011100005 ER PT J AU Koy, K McShea, WJ Leimgruber, P Aung, M AF Koy, K McShea, WJ Leimgruber, P Aung, M TI Percentage canopy cover - using Landsat imagery to delineate habitat for Myanmar's endangered Eld's deer (Cervus eldi) SO ANIMAL CONSERVATION LA English DT Article ID TROPICAL DEFORESTATION; CLASSIFICATION TREES; SATELLITE DATA; VEGETATION; FORESTS; AMAZON AB Percentage canopy cover data derived from Landsat Enhanced Thematic Mapper (ETM+) sensor data, validated with field measurements, provide a useful tool for delineating Myanmar's Eld's deer (Cervus eldi) habitat. The current extent and condition of remaining Eld's deer habitat is unknown, but the species prefers dry dipterocarp forest. This habitat type has widely varying canopy cover and cannot be accurately delineated with traditional remote sensing techniques. New maps based on estimates of percentage canopy cover represent the variability of dry dipterocarp forests more accurately than maps of strict classes of habitat. Over 500 field measurements of canopy cover were used to train Landsat ETM+ data that were analysed with regression-tree analysis. The resulting satellite-based estimates of canopy cover were compared with an independent set of field validation points (r = 0.539, P < 0.001, n = 114). The satellite-based estimates also showed potential for predicting the presence of Eld's deer (r = 0.636, P < 0.01, n = 14). The results from the predictive maps are in accordance with previous field studies demonstrating the species' preference for dense, dry dipterocarp forest. Patterns of percentage tree-canopy cover across the Study area were negatively correlated with human population density (r = -0.307, P < 0.001, n = 223), suggesting potential further threats to Eld's deer populations if the human population continues to grow. C1 Amer Museum Nat Hist, Ctr Biodivers & Conservat, New York, NY 10024 USA. Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. George Mason Univ, Fairfax, VA 22030 USA. Nat & Wildlife Conservat Div, Forest Dept, Insein, Yangon, Myanmar. RP Koy, K (reprint author), Amer Museum Nat Hist, Ctr Biodivers & Conservat, Central Pk W 79th St, New York, NY 10024 USA. EM kkoy@amnh.org RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 NR 31 TC 19 Z9 21 U1 3 U2 13 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD AUG PY 2005 VL 8 BP 289 EP 296 DI 10.1017/S1367943005002209 PN 3 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 970FG UT WOS:000232290000007 ER PT J AU Wisely, SM Santymire, RM Livieri, TM Marinari, PE Kreeger, JS Wildt, DE Howard, J AF Wisely, SM Santymire, RM Livieri, TM Marinari, PE Kreeger, JS Wildt, DE Howard, J TI Environment influences morphology and development for in situ and ex situ populations of the black-footed ferret (Mustela nigripes) SO ANIMAL CONSERVATION LA English DT Article ID VISON; SIZE; RECOVERY; GROWTH AB For selected species, conservation breeding has become integrated into recovery plans, most often through the production of offspring for reintroduction into nature. As these programs increase in size and scope, it is imperative that conservation managers retain the biological integrity of the species. This study investigated the causes of morphological changes that are known to occur in black-footed ferrets (Mustela nigripes) maintained ex situ. In a previous study, ferrets maintained in captivity were 5-10% smaller in body size than pre-captive, in situ animals. In the present study, the authors compared nine morphological characters among ex situ animals and their in situ descendants. Within the ex situ population, cage types were compared to determine whether housing influenced morphometry. Black-footed ferrets born to reintroduced individuals quickly returned to their pre-captive size suggesting that a diminutive morphology ex situ did not have a genetic basis. Furthermore, cage type affected overall body size and shape; ulnas and tibias were as much as 9% shorter for ex situ animals. The authors hypothesise that small cage size and environmental homogeneity inhibit the mechanical stimuli necessary for long bone development. These findings have ramifications for ex situ managers who need to create artificial captive settings that promote natural physical development. In the absence of such an environment, 'unnatural' morphologies can result that may contribute to poor fitness or perhaps even domestication. C1 Kansas State Univ, Div Biol, Manhattan, KS 66506 USA. Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Prairie Wildlife Res, Wall, SD 57790 USA. US Fish & Wildlife Serv, Natl Black Footed Ferret Conservat Ctr, Laramie, WY 82070 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Washington, DC 20008 USA. RP Wisely, SM (reprint author), Kansas State Univ, Div Biol, 232 Ackert Hall, Manhattan, KS 66506 USA. EM wisely@ksu.edu NR 42 TC 15 Z9 16 U1 1 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1367-9430 EI 1469-1795 J9 ANIM CONSERV JI Anim. Conserv. PD AUG PY 2005 VL 8 BP 321 EP 328 DI 10.1017/S1367943005002283 PN 3 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 970FG UT WOS:000232290000010 ER PT J AU Ghavamian, P Blair, WP Long, KS Sasaki, M Gaetz, TJ Plucinsky, PP AF Ghavamian, P Blair, WP Long, KS Sasaki, M Gaetz, TJ Plucinsky, PP TI Revealing the supernova remnant population of M33 with Chandra SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M33); galaxies : ISM; shock waves; supernova remnants ID X-RAY SOURCES; LARGE MAGELLANIC CLOUD; XMM-NEWTON SURVEY; H-II REGIONS; NOVA REMNANTS; SPIRAL GALAXIES; EMISSION; M-33; MORPHOLOGY; SUPERSOFT AB We present results of a search for supernova remnants (SNRs) in archival Chandra images of M33. We have identified X-ray SNRs by comparing the list of Chandra X-ray sources in M33 with tabulations of SNR candidates identified from ( 1) elevated [S II]/H alpha ratios in the optical and ( 2) radio spectral indices. In addition, we have searched for optical counterparts to soft sources in the Chandra images and X-ray SNR candidates identified in the XMM-Newton survey of M33. Of the 98 optically known SNRs in M33, 22 have been detected at > 3 sigma level in the soft band (0.35 - 1.1 keV). At least four of these SNR candidates are spatially extended based on a comparison of the data to simulated images of point sources. Aside from the optically matching SNRs, we have found one soft X-ray source in M33 that exhibits no optical emission and is coincident with a known radio source. The radio spectral index of this source is consistent with particle acceleration in shocks, leading us to suggest that it is a nonradiative SNR. We have also found new optical counterparts to two soft X-ray SNRs in M33. These counterparts exhibit enhanced [S II]/H alpha ratios characteristic of radiative shocks. Pending confirmation from optical spectroscopy, the identification of these two optical counterparts increases the total number of known optically emitting SNRs in M33 to 100. This brings the total number of identified SNRs with X-ray counterparts, including those exclusively detected by the XMM-Newton survey of M33, to 37 SNRs. We find that while there are a similar number of confirmed X-ray SNRs in M33 and the LMC with X-ray luminosities in excess of 10(35) ergs s(-1), nearly 40% of the LMC SNRs are brighter than 10(36) ergs s(-1), while only 13% of the M33 sample exceed this luminosity. Including X-ray SNR candidates from the XMM-Newton survey ( objects lacking optical counterparts) increases the fraction of M33 SNRs brighter than 10(36) ergs s(-1) to 22%, still only half the LMC fraction. The differences in luminosity distributions cannot be fully explained by uncertainty in spectral model parameters and are not fully accounted for by abundance differences between the galaxies. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ghavamian, P (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM parviz@pha.jhu.edu; wpb@pha.jhu.edu; long@stsci.edu; sasaki@cfa.harvard.edu; gaetz@cfa.harvard.edu; plucinsky@cfa.harvard.edu RI Sasaki, Manami/P-3045-2016 OI Sasaki, Manami/0000-0001-5302-1866 NR 43 TC 22 Z9 22 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 AUG PY 2005 VL 130 IS 2 BP 539 EP 553 DI 10.1086/431481 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948NC UT WOS:000230721600013 ER PT J AU Eiroa, C Torrelles, JM Curiel, S Djupvik, AA AF Eiroa, C Torrelles, JM Curiel, S Djupvik, AA TI Very Large Array 3.5 cm continuum sources in the Serpens cloud core SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (Serpens); radio continuum : stars; stars : formation ID YOUNG STELLAR OBJECTS; STAR-FORMING REGION; MOLECULAR CLOUD; INFRARED IMAGES; OPHIUCHI CLOUD; PROPER MOTIONS; RHO-OPHIUCHI; DARK CLOUD; SVS 20; OUTFLOW AB We present Very Large Array (VLA) 3.5 cm continuum observations of the Serpens cloud core. Twenty-two radio continuum sources are detected. Sixteen out of the 22 centimeter sources are suggested to be associated with young stellar objects ( Class 0, Class I, flat spectrum, and Class II) of the young Serpens cluster. The rest of the VLA sources are plausibly background objects. Most of the Serpens centimeter sources likely represent thermal radio jets; on the other hand, the radio continuum emission of some sources could be due to a gyrosynchroton mechanism arising from coronally active young stars. The Serpens VLA sources are spatially distributed into two groups; one of them located toward the northwest clump of the Serpens core, where only Class 0 and Class I protostars are found to present centimeter emission, and a second group located toward the southeast clump, where radio continuum sources are associated with objects in evolutionary classes from Class 0 to Class II. This subgrouping is similar to that found in the near-IR, mid-IR, and millimeter wavelength regimes. C1 Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. CSIC, Inst Ciencias Espacio, Barcelona 08034, Spain. Inst Estudis Espacials Catalunya, Barcelona 08034, Spain. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nord Opt Telescope, Santa Cruz De La Palma 38700, Canary Islands, Spain. RP Eiroa, C (reprint author), Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, C-XI, E-28049 Madrid, Spain. EM carlos.eiroa@uam.es; torrelles@ieec.fcr.es; scuriel@astroscu.unam.mx; akaas@not.iac.es OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 61 TC 22 Z9 22 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2005 VL 130 IS 2 BP 643 EP 651 DI 10.1086/431742 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948NC UT WOS:000230721600021 ER PT J AU Evans, NR Carpenter, KG Robinson, R Kienzle, F Dekas, AE AF Evans, NR Carpenter, KG Robinson, R Kienzle, F Dekas, AE TI High-mass triple systems: The classical Cepheid Y Carinae SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : close; Cepheids; stars : evolution; stars : fundamental parameters ID FF-AQL; ORBIT; COMPANION; CYGNI; LUMINOSITY; TELESCOPE; OPACITIES; STARS AB We have obtained a Hubble Space Telescope STIS ultraviolet high-dispersion echelle-mode spectrum of the binary companion of the double-mode classical Cepheid Y Car. The velocity measured for the hot companion from this spectrum is very different from reasonable predictions for binary motion, implying that the companion is itself a short-period binary. The measured velocity changed by 7 km s(-1) during the 4 days between two segments of the observation, confirming this interpretation. We summarize "binary'' Cepheids that are in fact members of a triple system and find that at least 44% are triples. The summary of information on Cepheids with orbits makes it likely that the fraction is underestimated. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. Harvard Univ, Cambridge, MA 02138 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu; kgc@stargate.gsfc.nasa.gov; robinson@pha.jhu.edu; francesco.kienzle@obs.unige.ch RI Carpenter, Kenneth/D-4740-2012 NR 26 TC 15 Z9 15 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 AUG PY 2005 VL 130 IS 2 BP 789 EP 793 DI 10.1086/430458 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 948NC UT WOS:000230721600034 ER PT J AU Schroedter, M AF Schroedter, M TI Upper limits on the extragalactic background light from the very high energy gamma-ray spectra of blazars SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : general; diffuse radiation; gamma rays : observations; infrared : general ID INTERGALACTIC INFRARED RADIATION; ACTIVE GALACTIC NUCLEI; GALAXY COUNTS; EXPERIMENT SEARCH; POWER SPECTRUM; STRONG FLARES; PKS 2155-304; X-RAY; MU-M; TEV AB The direct measurement of the extragalactic background light (EBL) is difficult at optical to infrared wavelengths because of the strong foreground radiation originating in the solar system. Very high energy (VHE; E > 100 GeV) gamma rays interact with EBL photons of these wavelengths through pair production. In this work, the available VHE spectra from six blazars are used to place upper limits on the EBL. These blazars have been detected over a range of redshifts, and a steepening of the spectral index is observed with increasing source distance. This can be interpreted as absorption by the EBL. In general, knowledge of the intrinsic source spectrum is necessary to determine the density of the intervening EBL. Motivated by the observed spectral steepening with redshift, upper limits on the EBL are derived by assuming that the intrinsic spectra of the six blazars are proportional to E-1.8. Upper limits are then placed on the EBL flux at discrete energies without assuming a specific spectral shape for the EBL. This is an advantage over other methods since the EBL spectrum is uncertain. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Schroedter, M (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM mschroed@cfa.harvard.edu NR 70 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP 617 EP 628 DI 10.1086/431173 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300006 ER PT J AU Nulsen, PEJ McNamara, BR Wise, MW David, LP AF Nulsen, PEJ McNamara, BR Wise, MW David, LP TI The cluster-scale AGN outburst in Hydra A SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : active; galaxies : clusters : individual (Hydra A); intergalactic medium; X-rays : galaxies : clusters ID ACTIVE GALACTIC NUCLEUS; RADIO GALAXY HYDRA; RAY-EMITTING GAS; COOLING FLOWS; HIGH-RESOLUTION; INTRACLUSTER MEDIUM; CHANDRA OBSERVATION; 3C 218; LOBES; CAVITIES AB Deep Chandra observations of the Hydra A Cluster reveal a feature in the X-ray surface brightness that surrounds the 330 MHz radio lobes of the AGN at the cluster center. Surface brightness profiles of this feature and its close association with the radio lobes argue strongly that it is a shock front driven by the expanding radio lobes. The Chandra image also reveals other new structure on smaller scales that is associated with the radio source, including a large cavity and filament. The shock front extends 200-300 kpc from the AGN at the cluster center, and its strength varies along the front, with Mach numbers in the range similar to 1.2-1.4. It is stronger where it is more distant from the cluster center, as expected for a shock driven by expanding radio lobes. Simple modeling gives an age for the shock front of similar to 1.4; 10(8) yr and a total energy driving it of similar to 10(61) ergs. The mean mechanical power driving the shock is comparable to quasar luminosities, well in excess of that needed to regulate the cooling core in Hydra A. This suggests that the feedback regulating cooling cores is inefficient, in that the bulk of the energy is deposited beyond the cooling core. In that case, a significant part of cluster "preheating" is a by-product of the regulation of cooling cores. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio Univ, Clippinger Labs, Inst Astrophys, Athens, OH 45701 USA. Ohio Univ, Clippinger Labs, Dept Phys & Astron, Athens, OH 45701 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Nulsen, PEJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 48 TC 151 Z9 151 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 AUG 1 PY 2005 VL 628 IS 2 BP 629 EP 636 DI 10.1086/430845 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300007 ER PT J AU Vikhlinin, A Markevitch, M Murray, SS Jones, C Forman, W Van Speybroeck, L AF Vikhlinin, A Markevitch, M Murray, SS Jones, C Forman, W Van Speybroeck, L TI Chandra temperature profiles for a sample of nearby relaxed galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; X-rays : galaxies : clusters ID XMM-NEWTON OBSERVATION; X-RAY-CLUSTERS; ROSAT PSPC OBSERVATIONS; DARK-MATTER; ENTROPY PROFILES; INTRACLUSTER MEDIUM; RADIAL TEMPERATURE; CHARGE-TRANSFER; MASS PROFILES; CORE AB We present Chandra gas temperature profiles at large radii for a sample of 13 nearby, relaxed galaxy clusters and groups, which includes A133, A262, A383, A478, A907, A1413, A1795, A1991, A2029, A2390, MKW 4, RX J1159+5531, and USGC S152. The sample covers a range of average temperatures from 1 to 10 keV. The clusters are selected from the archive or observed by us to have sufficient exposures and off-center area coverage to enable accurate background subtraction and reach the temperature accuracy of better than 20%-30% at least to r = (0.4-0.5)r(180) and for the three best clusters to (0.6-0.7)r(180). For all clusters, we find cool gas in the cores, outside of which the temperature reaches a peak at r similar to 0.15r(180) and then declines to similar to 0.5 of its peak value at r similar or equal to 0.5r(180). When the profiles are scaled by the cluster average temperature (excluding cool cores) and the estimated virial radius, they show large scatter at small radii but remarkable similarity at r > (0.1-0.2)r(180) for all but one cluster (A2390). Our results are in good agreement with previous measurements from ASCA by Markevitch et al. and from BeppoSAX by De Grandi & Molendi. Four clusters have recent XMM-Newton temperature profiles, two of which agree with our results, and we discuss reasons for disagreement for the other two. The overall shape of the temperature profiles at large radii is reproduced in recent cosmological simulations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow Space Res Inst, Moscow 117810, Russia. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avikhlinin@cfa.harvard.edu NR 69 TC 338 Z9 339 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 AUG 1 PY 2005 VL 628 IS 2 BP 655 EP 672 DI 10.1086/431142 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300009 ER PT J AU Williams, RM Chu, YH Dickel, JR Gruendl, RA Seward, FD Guerrero, MA Hobbs, G AF Williams, RM Chu, YH Dickel, JR Gruendl, RA Seward, FD Guerrero, MA Hobbs, G TI Supernova remnants in the Magellanic Clouds. V. The complex interior structure of the N206 supernova remnant SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (SNR B0532-71.0); Magellanic Clouds; X-rays : ISM ID X-RAY; BOW SHOCK; LINE SURVEY; NEBULA; PULSAR; IC-443; W44; G359.23-0.82; DISCOVERY; ATLAS AB The N206 supernova remnant (SNR) in the Large Magellanic Cloud has long been considered a prototypical "mixed morphology" SNR. Recent observations, however, have added a new twist to this familiar plot: an elongated, radially oriented radio feature seen in projection against the SNR face. Utilizing the high resolution and sensitivity available with the Hubble Space Telescope, Chandra, and XMM-Newton, we have obtained optical emission line images and spatially resolved X-ray spectral maps for this intriguing SNR. Our findings present the SNR itself as a remnant in the middle to late stages of its evolution. X-ray emission associated with the radio linear feature strongly suggests it to be a pulsar wind nebula (PWN). A small X-ray knot is discovered at the outer tip of this feature. The feature's elongated morphology and the surrounding wedge-shaped X-ray enhancement strongly suggest a bow shock PWN structure. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Williams, RM (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. EM rosanina@astro.uiuc.edu; chu@astro.uiuc.edu; johnd@astro.uiuc.edu; gruendl@astro.uiuc.edu; fds@cfa.harvard.edu; mar@iaa.es; ghobbs@atnf.csiro.au OI Guerrero, Martin/0000-0002-7759-106X NR 33 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP 704 EP 720 DI 10.1086/431349 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300013 ER PT J AU Beuther, H Zhang, Q Sridharan, TK Chen, Y AF Beuther, H Zhang, Q Sridharan, TK Chen, Y TI Testing the massive disk scenario for IRAS 18089-1732 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; astrochemistry; ISM : individual (IRAS 18089-1732); stars : formation; submillimeter; techniques : interferometric ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; MOLECULAR CLOUDS; IRAS 20126+4104; LINE SURVEY; ORION-KL; PROTOSTELLAR CANDIDATES; SUBMILLIMETER ARRAY; ROTATING-DISK; OUTFLOWS AB Investigating in more detail the previously suggested massive disk scenario for the high-mass protostellar object IRAS 18089-1732, we observed the source in the 860 mu m band with the Submillimeter Array in various spectral lines and the submillimeter continuum emission at (sub-)arcsecond spatial resolution. Fifty spectral lines from 18 different species spanning upper-level energy states between 17 and 747 K were detected. One of the assumed best tracers for massive disks, CH3CN, is optically thick and does not allow a further disk investigation. However, the complex molecule HCOOCH3 appears optically thin and exhibits a velocity shift across the central core perpendicular to the emanating outflow. This signature is comparable to well-known low-mass disks and confirms the detection of a massive rotating structure likely associated with the central accretion disk. Assuming equilibrium between centrifugal and gravitational force, the estimated mass for this rotating structure is 16/[sin(2)(i)] M-circle dot (where i is the unknown inclination angle), of the same order as the gas mass derived from the continuum emission. Therefore, in contrast to low-mass disks, a considerable amount of the central gas mass is associated with the rotation, implying that massive disks may not be Keplerian. A temperature estimate based on the CH3CN(19-18) K-ladder results in similar to 350 K; thus, a hot core has already formed in this region. An analysis of the submillimeter continuum emission reveals even at this high spatial resolution only one isolated massive dust core without any detectable companions down to mass limits between 0.2 and 3 M-circle dot (depending on the assumed temperature). Potential implications for the massive cluster formation are discussed. The radial intensity distribution of the core is highly nonsymmetric, outlining the difficulties of density structure investigations based on radial averaging. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 41 TC 37 Z9 37 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP 800 EP 810 DI 10.1086/431277 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300022 ER PT J AU Swartz, DA Drake, JJ Elsner, RF Ghosh, KK Grady, CA Wassell, E Woodgate, BE Kimble, RA AF Swartz, DA Drake, JJ Elsner, RF Ghosh, KK Grady, CA Wassell, E Woodgate, BE Kimble, RA TI The Herbig Ae star HD 163296 in X-rays SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : emission-line, Be; stars : individual (HD 163296); stars : pre-main-sequence; X-rays : stars ID T-TAURI STARS; INTERMEDIATE-MASS STARS; LINE-PROFILE-VARIABILITY; MAIN-SEQUENCE EVOLUTION; ACCRETION SHOCK-WAVE; AE/BE STARS; HIGH-RESOLUTION; MAGNETIC-FIELD; AU MICROSCOPII; DISK ACCRETION AB Chandra X-ray imaging spectroscopy of the nearby Herbig Ae star HD 163296 at 100 AU angular resolution is reported. A pointlike, soft (kT similar to 0.5 keV), emission-line source is detected at the location of the star with an X-ray luminosity of 4 x 10(29) ergs s(-1) (log L-X/L-bol = -5.48). In addition, faint emission along the direction of a previously detected Ly alpha-emitting jet and Herbig-Haro outflow may be present. The relatively low luminosity, lack of a hard spectral component, and absence of strong X-ray variability in HD 163296 can be explained as originating from optically thin shock-heated gas accreting onto the stellar surface along magnetic field lines. This would require a ( dipole) magnetic field strength at the surface of HD 163296 of at least similar to 100 G and perhaps as high as several kG. HD 163296 joins the T Tauri star TW Hya in being the only examples known to date of pre-main-sequence stars whose quiescent X-ray emission appears to be completely dominated by accretion. C1 NASA, Univ Space Res Assoc, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Eureka Sci, Greenbelt, MD 20771 USA. NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Thomas Aquinas Coll, Santa Paula, CA USA. Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Swartz, DA (reprint author), NASA, Univ Space Res Assoc, George C Marshall Space Flight Ctr, SD50, Huntsville, AL 35812 USA. RI Woodgate, Bruce/D-2970-2012 NR 60 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP 811 EP 816 DI 10.1086/429984 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300023 ER PT J AU Hoogerwerf, R Brickhouse, NS Mauche, CW AF Hoogerwerf, R Brickhouse, NS Mauche, CW TI X-ray light curves and accretion disk structure of EX Hydrae SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars : individual (EX Hydrae); X-rays : stars ID CLOSE BINARY-SYSTEM; WHITE-DWARF; EXTREME-ULTRAVIOLET; SPECTROSCOPY; HYA; SIMULATION; PHOTOMETRY; FLOW; MASS AB We present X-ray light curves for the cataclysmic variable EX Hydrae obtained with the Chandra High Energy Transmission Grating Spectrometer and the Extreme Ultraviolet Explorer Deep Survey photometer. We confirm earlier results on the shape and amplitude of the binary light curve and discuss a new feature: the phase of the minimum in the binary light curve, associated with absorption by the bulge on the accretion disk, increases with wavelength. We discuss several scenarios that could account for this trend and conclude that, most likely, the ionization state of the bulge gas is not constant, but rather decreases with binary phase. We also conclude that photoionization of the bulge by radiation originating from the white dwarf is not the main source of ionization, but that it is heated by shocks originating from the interaction between the inflowing material from the companion and the accretion disk. The findings in this paper provide a strong test for accretion disk models in close binary systems. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Hoogerwerf, R (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St,MS 31, Cambridge, MA 02138 USA. EM rhoogerwerf@cfa.harvard.edu; nbrickhouse@cfa.harvard.edu; mauche@cygnus.llnl.gov OI Brickhouse, Nancy/0000-0002-8704-4473 NR 31 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP 946 EP 952 DI 10.1086/431211 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300037 ER PT J AU Frazin, RA Kamalabadi, F Weber, MA AF Frazin, RA Kamalabadi, F Weber, MA TI On the combination of differential emission measure analysis and rotational tomography for three-dimensional solar EUV imaging SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : UV radiation; techniques : image processing ID ELECTRON-DENSITY DISTRIBUTION; WHOLE SUN MONTH; X-RAY CORONA; MEASURE DISTRIBUTIONS; POSITIVE ESTIMATION; RECONSTRUCTION; ROBUST; TEMPERATURES; TELESCOPE; REGIONS AB Conventional differential emission measure (DEM) analysis allows one to determine the amount of plasma as a function of temperature along a given line of sight. A completely different technique called solar rotational tomography (SRT) exploits the view angles provided by solar rotation to determine the spatial distribution of emissivity in three dimensions. These two techniques can be combined in a procedure called differential emission measure tomography (DEMT) to determine the DEM at each point in the corona with the same spatial resolution as can normally be achieved by SRT. In this paper the theory of DEMT is presented, and numerical examples based on the Atmospheric Imaging Assembly (AIA) are given. The results demonstrate promising potential for the methods to be adapted for use with other EUV and X-ray imaging and/or spectroscopy instruments. C1 Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frazin, RA (reprint author), Univ Illinois, Dept Elect & Comp Engn, 1406 W Green St, Urbana, IL 61801 USA. RI Frazin, Richard/J-2625-2012 NR 44 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP 1070 EP 1080 DI 10.1086/431295 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VX UT WOS:000230817300048 ER PT J AU Diaferio, A Geller, MJ Rines, KJ AF Diaferio, A Geller, MJ Rines, KJ TI Caustic and weak-lensing estimators of galaxy cluster masses SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : miscellaneous; cosmology : observations; galaxies : clusters : individual (Abell 2390; Cl 0024+1654, MS 1358.4+6245); gravitational lensing ID FIELD SPECTROSCOPIC SURVEY; REDSHIFT SURVEY CATALOGS; HUBBLE-SPACE-TELESCOPE; X-RAY; ABELL 2390; XMM-NEWTON; PROFILES; DISTANT; REGIONS; MATTER AB There are only two methods for estimating the mass distribution in the outer regions of galaxy clusters, where virial equilibrium does not hold: weak gravitational lensing and identification of caustics in redshift space. For the first time, we apply both methods to three clusters: Abell 2390, MS 1358.4 + 6245, and Cl 0024 + 1654. The two measures are in remarkably good agreement out to similar to 2 h(-1) Mpc from the cluster centers. This result demonstrates that the caustic technique is a valuable complement to weak lensing. With a few tens of redshifts per square comoving megaparsec within the cluster, the caustic method is applicable for any z less than or similar to 0.5. C1 Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. RP Diaferio, A (reprint author), Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Via P Giuria 1, I-10125 Turin, Italy. EM diaferio@ph.unito.it; mjg@cfa.harvard.edu; krines@astro.yale.edu NR 40 TC 47 Z9 47 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 AUG 1 PY 2005 VL 628 IS 2 BP L97 EP L100 DI 10.1086/432880 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VY UT WOS:000230817400004 ER PT J AU Hartmann, L Calvet, N Watson, DM D'Alessio, P Furlan, E Sargent, B Forrest, WJ Uchida, KI Green, JD Sloan, GC Chen, CH Najita, J Kemper, F Herter, TL Morris, P Barry, DJ Hall, P AF Hartmann, L Calvet, N Watson, DM D'Alessio, P Furlan, E Sargent, B Forrest, WJ Uchida, KI Green, JD Sloan, GC Chen, CH Najita, J Kemper, F Herter, TL Morris, P Barry, DJ Hall, P TI The accretion disk of the lithium-depleted young binary ST 34 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared : stars; stars : formation; stars : pre-main-sequence ID T-TAURI-STARS; SPITZER-SPACE-TELESCOPE; AURIGA MOLECULAR CLOUD; ALPHA EMISSION STARS; INFRARED SPECTROGRAPH; HYDRAE ASSOCIATION; MODELS; DUST; OBJECTS; EXTINCTION AB We present the infrared spectrum of the young binary system St 34 obtained with the Infrared Spectrograph (IRS) on the Spitzer Space Telescope. The IRS spectrum clearly shows excess dust emission, consistent with the suggestion of White & Hillenbrand that St 34 is accreting from a circumbinary disk. The disk emission of St 34 is low in comparison with the levels observed in typical T Tauri stars; silicate features at similar to 10 and 20 mu m are much weaker than typically seen in T Tauri stars; and excess emission is nearly absent at the shortest wavelengths observed (similar to 5 mu m). These features of the infrared spectrum suggest substantial grain growth ( to eliminate silicate features) and possible settling of dust to the disk midplane ( to reduce the continuum excess emission levels), along with a relatively evacuated inner disk, as expected due to gravitational perturbations by the binary system. Although the position of St 34 in the H-R diagram suggests an age of 8 +/- 3 Myr, assuming that it lies at the distance of the Taurus-Auriga molecular clouds, White & Hillenbrand could not detect any Li I absorption, which would indicate a Li depletion age of roughly 25 Myr or more. We suggest that St 34 is closer than the Taurus clouds by similar to 30 - 40 pc and has an age roughly consistent with Li depletion models. Such an advanced age would make St 34 the oldest known low-mass pre-main-sequence object with a dusty accretion disk. The persistence of optically thick dust emission well outside the binary orbit may indicate a failure to make giant planets that could effectively remove dust particles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, NASA Herschel Sci Ctr, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hartmann@cfa.harvard.edu RI Kemper, Francisca/D-8688-2011; OI Kemper, Francisca/0000-0003-2743-8240; Furlan, Elise/0000-0001-9800-6248 NR 51 TC 18 Z9 18 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 AUG 1 PY 2005 VL 628 IS 2 BP L147 EP L150 DI 10.1086/432756 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VY UT WOS:000230817400016 ER PT J AU Manchester, RN Gaensler, BM Staveley-Smith, L Kesteven, MJ Tzioumis, AK AF Manchester, RN Gaensler, BM Staveley-Smith, L Kesteven, MJ Tzioumis, AK TI Imaging of the radio remnant of SN 1987A at 12 mm wavelength SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum : ISM; supernova remnants; supernovae : individual (SN 1987A) ID SPACE-TELESCOPE OBSERVATIONS; LARGE-MAGELLANIC-CLOUD; SUPERNOVA REMNANT; EVOLUTION; NEBULA; SHOCK; VIEW AB Observations of the radio remnant of supernova 1987A using the Australia Telescope Compact Array in the 12 mm band on 2003 July 31 ( day 6002.7 after the explosion) give the first fully resolved radio image of the supernova remnant. The diffraction-limited image has a resolution of about 0 ''.45, a factor of 2 better than that of the previously obtained 3 cm images. There is excellent agreement between the 12 mm image and a contemporaneous superresolved 3 cm image. Superresolution of the 12 mm image gives a further factor of 2 improvement in resolution, to 0 ''.25, albeit with limited dynamic range. While the spatial distributions of the radio and X-ray emission are broadly similar, there are significant differences in detail, with no correspondence in the regions of brightest emission. The 12 mm image is well modeled by a thick equatorial ring inclined at 43 degrees to the line of sight. This, together with the common east-west asymmetry and the relatively steady increase in the radio flux density, suggests that the reverse shock is the main site for generation of the radio emission. C1 CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Manchester, RN (reprint author), CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. EM dick.manchester@csiro.au RI Gaensler, Bryan/F-8655-2010; Staveley-Smith, Lister/A-1683-2011; OI Staveley-Smith, Lister/0000-0002-8057-0294; Gaensler, Bryan/0000-0002-3382-9558 NR 23 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2005 VL 628 IS 2 BP L131 EP L134 DI 10.1086/432836 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VY UT WOS:000230817400012 ER PT J AU Udalski, A Jaroszynski, M Paczynski, B Kubiak, M Szymanski, MK Soszynski, I Pietrzynski, G Ulaczyk, K Szewczyk, O Wyrzykowski, L Christie, GW DePoy, DL Dong, S Gal-Yam, A Gaudi, BS Gould, A Han, C Lepine, S McCormick, J Park, BG Pogge, RW Bennett, DP Bond, IA Muraki, Y Tristram, PJ Yock, PCM Beaulieu, JP Bramich, DM Dieters, SW Greenhill, J Hill, K Horne, K Kubas, D AF Udalski, A Jaroszynski, M Paczynski, B Kubiak, M Szymanski, MK Soszynski, I Pietrzynski, G Ulaczyk, K Szewczyk, O Wyrzykowski, L Christie, GW DePoy, DL Dong, S Gal-Yam, A Gaudi, BS Gould, A Han, C Lepine, S McCormick, J Park, BG Pogge, RW Bennett, DP Bond, IA Muraki, Y Tristram, PJ Yock, PCM Beaulieu, JP Bramich, DM Dieters, SW Greenhill, J Hill, K Horne, K Kubas, D CA OGLE Collaborat muFUN Collaborat MOA Collaborat PLANET RoboNet Collaborat TI A jovian-mass planet in microlensing event OGLE-2005-BLG-071 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy : bulge; gravitational lensing; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; EXTRASOLAR PLANETS; HIGH-MAGNIFICATION; GALACTIC BULGE; COMPANIONS; STAR; CONSTRAINTS; PHOTOMETRY; TRANSITS; CAMPAIGN AB We report the discovery of a several-Jupiter - mass planetary companion to the primary lens star in microlensing event OGLE-2005-BLG-071. Precise ( less than or similar to 1%) photometry at the peak of the event yields an extremely high signal-to-noise ratio detection of a deviation from the light curve expected from an isolated lens. The planetary character of this deviation is easily and unambiguously discernible from the gross features of the light curve. Detailed modeling yields a tightly constrained planet-star mass ratio of q = m(p) / M = 0.0071 +/- 0.0003. This is the second robust detection of a planet with microlensing, demonstrating that the technique itself is viable and that planets are not rare in the systems probed by microlensing, which typically lie several kiloparsecs toward the Galactic center. C1 Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Concepcion, Dept Fis, Concepcion, Chile. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Auckland Observ, Auckland 1030, New Zealand. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Cheongju 361763, South Korea. Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. FArm Cove Observ, Ctr Backyard Astrophys, Auckland 1706, New Zealand. Korea Astron & Space Sci Inst, Bohyunsan Opt Astron Observ, Yeongcheon 770820, South Korea. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Massey Univ, Inst Informat & Math Sci, Auckland 1330, New Zealand. Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. Univ Auckland, Dept Phys, Auckland 1001, New Zealand. Inst Astrophys Paris, F-75014 Paris, France. Univ St Andrews, Sch Phys & Astron, Scottish Univ Phys Alliance, St Andrews KY16 9SS, Fife, Scotland. RP Udalski, A (reprint author), Warsaw Univ, Astron Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. EM udalski@astrouw.edu.pl; gould@astronomy.ohio-state.edu; beaulieu@iap.fr RI Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012; Greenhill, John/C-8367-2013; Bennett, David/O-2136-2013 OI Bennett, David/0000-0001-8043-8413 NR 30 TC 145 Z9 146 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 AUG 1 PY 2005 VL 628 IS 2 BP L109 EP L112 DI 10.1086/432795 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VY UT WOS:000230817400007 ER PT J AU Winn, JN Holman, MJ AF Winn, JN Holman, MJ TI Obliquity tides on hot jupiters SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; planetary systems : formation; planets and satellites : formation; stars : individual (HD 209458) ID EXTRASOLAR GIANT PLANETS; GENERALIZED CASSINIS LAWS; B-LIKE PLANETS; TRANSITING PLANET; SOLAR-SYSTEM; HD 209458B; STAR; OBLATENESS; HD-209458; EVOLUTION AB Obliquity tides are a potentially important source of heat for extrasolar planets on close-in orbits. Although tidal dissipation will usually reduce the obliquity to zero, a nonzero obliquity can persist if the planet is in a Cassini state, a resonance between spin precession and orbital precession. Obliquity tides might be the cause of the anomalously large size of the transiting planet HD 209458b. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 TC 65 Z9 66 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 AUG 1 PY 2005 VL 628 IS 2 BP L159 EP L162 DI 10.1086/432834 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VY UT WOS:000230817400019 ER PT J AU Kilgard, RE Cowan, JJ Garcia, MR Kaaret, P Krauss, MI McDowell, JC Prestwich, AH Primini, FA Stockdale, CJ Trinchieri, G Ward, MJ Zezas, A AF Kilgard, RE Cowan, JJ Garcia, MR Kaaret, P Krauss, MI McDowell, JC Prestwich, AH Primini, FA Stockdale, CJ Trinchieri, G Ward, MJ Zezas, A TI A Chandra survey of nearby spiral galaxies. I. Point source catalogs SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies : spiral; surveys; X-rays : galaxies ID X-RAY SOURCES; STAR-FORMATION; STARBURST; EMISSION; DISTANCE; M101; M83; NGC-4314; 1999GI; SOUTH AB Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. We present results from a survey of 11 nearby, nearly face-on spiral galaxies with the Chandra X-ray Observatory. These galaxies span the Hubble sequence for spirals, allowing insights into the X-ray source population of many diverse systems. In this paper, we present source lists for the 11 galaxies along with fluxes, luminosities, X-ray colors, and variability properties. We briefly discuss X-ray luminosity functions and how they relate to star formation of the host galaxies. We also discuss source colors and variability and what these can tell us about the composition of the X-ray source population. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Leicester LE1 7RH, Leics, England. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. USN, Res Lab, Washington, DC 20375 USA. Brera Astron Observ, I-20121 Milan, Italy. RP Kilgard, RE (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; Trinchieri, Ginevra/0000-0002-0227-502X; Primini, Francis/0000-0002-6077-0643 NR 40 TC 36 Z9 36 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 AUG PY 2005 VL 159 IS 2 BP 214 EP 241 DI 10.1086/430443 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VV UT WOS:000230817100002 ER PT J AU Gelfand, JD Lazio, TJW Gaensler, BM AF Gelfand, JD Lazio, TJW Gaensler, BM TI A wide-field, low-frequency radio image of the field of M31. II. Source classification and discussion SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies : individual (M31); radio continuum : galaxies; radio continuum : general ID SUPERNOVA REMNANT CANDIDATES; EXTREME SCATTERING EVENTS; COMPACT STEEP-SPECTRUM; BL LACERTAE OBJECTS; RAY POINT SOURCES; VLA SKY SURVEY; INTERSTELLAR-MEDIUM; SOURCE CATALOG; FLUX-DENSITY; MULTIFREQUENCY OBSERVATIONS AB We have previously presented the results of a 325 MHz radio survey of M31, conducted with the A configuration of the Very Large Array. In this survey, a total of 405 radio sources between less than or similar to 6 '' and 170 '' in extent were mapped with a resolution of 6 '' and a sensitivity of similar to 0.6 mJy beam(-1). Here we compare the resultant source list and image with other radio, IR, optical, and X-ray observations and catalogs of the region. Through this, we were able to identify five supernova remnant candidates and three pulsar wind nebula candidates in M31, as well as three Milky Way radio stars, a possible Milky Way planetary nebula, and a bevy of interesting extragalactic objects: a BL Lac, a giant radio galaxy, a galaxy merger, and several high-z radio galaxy candidates. In addition, a large number of compact (theta less than or similar to 6 '') extremely steep-spectrum sources (alpha <= -1.6; S-nu proportional to nu(alpha)) were detected whose nature is unknown. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Washington, DC 20375 USA. RP Gelfand, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-10, Cambridge, MA 02138 USA. EM jgelfand@cfa.harvard.edu; Joseph.Lazio@nrl.navy.mil; bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 97 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 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2005 VL 159 IS 2 BP 242 EP 276 DI 10.1086/431363 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 949VV UT WOS:000230817100003 ER PT J AU Williams, HE Duckett, CN AF Williams, HE Duckett, CN TI The trimorphic flea-beetle, Alagoasa extrema, not suitable for biocontrol of Lantana camara in Africa SO BIOCONTROL LA English DT Article DE Alticinae; Alagoasa quadrilineata; biological weed control; biology; Chrysomelidae; Coleoptera; host specificity; polymorphism; risk assessment; Verbenaceae; Kushelina petaurista ID TREE SOLANUM-MAURITIANUM; BIOLOGICAL-CONTROL; SOUTH-AFRICA; HOST-SPECIFICITY; RISK-ASSESSMENT; NORTH-AMERICA; CHRYSOMELIDAE; COLEOPTERA; AGENT; VERBENACEAE AB The biology and host range of the flea-beetle, Alagoasa extrema (Harold) (Coleoptera: Chrysomelidae: Galerucinae: Alticini), was studied under quarantine laboratory conditions to evaluate the insect's suitability for release as a biological control agent for the noxious weed, Lantana camara L. (Verbenaceae), in South Africa. Identification of this species proved noteworthy. The adults of A. extrema display three freely interbreeding and very distinct colour morphs, which can be confused with no less than 11 species of Alagoasa found in Mexico and the southwestern U.S. Initially, specimens were identified as two species of the genus Alagoasa Bechyne, i.e. A. quadrilineata (Harold) and A. extrema. Thirteen additional Alagoasa species and Kushelina petaurista (F). that can be confused with A. extremabased on external morphology of adults or larvae are discussed. Favourable biological characteristics included long-lived adults, several overlapping generations per year, and high adult and larval feeding rates. Observations from the insect's native Mexican range and studies in South Africa suggest that A. extrema would probably be more suited to subtropical, rather than temperate areas in Africa. Host-specificity studies showed A. extrema to be an oligophagous species, capable of feeding and developing on several non-target species, especially two indigenous, African Lippia species (Verbenaceae). The host suitability of these indigenous species was only marginally lower than that of L. camara, and the potential risk to them was deemed to be too high to warrant release. It was therefore recommended that A. extrema be rejected as biocontrol agent for lantana in Africa. C1 Agr Res Council, Plant Protect Res Inst, Washington, DC USA. Smithsonian Inst, Washington, DC 20013 USA. RP Williams, HE (reprint author), ARC, Plant Protect Res Inst, Private Bag X134, ZA-0121 Queenswood, South Africa. EM riethes@plant2.agric.za NR 44 TC 6 Z9 7 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1386-6141 J9 BIOCONTROL JI Biocontrol PD AUG PY 2005 VL 50 IS 4 BP 657 EP 683 DI 10.1007/s10526-004-5528-0 PG 27 WC Entomology SC Entomology GA 951AC UT WOS:000230899900009 ER PT J AU Funk, VA Richardson, KS Ferrier, S AF Funk, VA Richardson, KS Ferrier, S TI Survey-gap analysis in expeditionary research: where do we go from here? SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE collecting expeditions; ED complementarity; environmental diversity ID ENVIRONMENTAL DIVERSITY; BIODIVERSITY; CONSERVATION; SURROGATE; INFORMATION; HOTSPOTS; GUYANA AB Research expeditions into remote areas to collect biological specimens provide vital information for understanding biodiversity. However, major expeditions to little-known areas are expensive and time consuming, time is short, and well-trained people are difficult to find. In addition, processing the collections and obtaining accurate identifications takes time and money. In order to get the maximum return for the investment, we need to determine the location of the collecting expeditions carefully. In this study we used environmental variables and information on existing collecting localities to help determine the sites of future expeditions. Results from other studies were used to aid in the selection of the environmental variables, including variables relating to temperature, rainfall, lithology and distance between sites. A survey gap analysis tool based on 'ED complementarity' was employed to select the sites that would most likely contribute the most new taxa. The tool does not evaluate how well collected a previously visited site survey site might be; however, collecting effort was estimated based on species accumulation curves. We used the number of collections and/or number of species at each collecting site to eliminate those we deemed poorly collected. Plants, birds, and insects from Guyana were examined using the survey gap analysis tool, and sites for future collecting expeditions were determined. The south-east section of Guyana had virtually no collecting information available. It has been inaccessible for many years for political reasons and as a result, eight of the first ten sites selected were in that area. In order to evaluate the remainder of the country, and because there are no immediate plans by the Government of Guyana to open that area to exploration, that section of the country was not included in the remainder of the study. The range of the ED complementarity values dropped sharply after the first ten sites were selected. For plants, the group for which we had the most records, areas selected included several localities in the Pakaraima Mountains, the border with the south-east, and one site in the north-west. For birds, a moderately collected group, the strongest need was in the north-west followed by the east. Insects had the smallest data set and the largest range of ED complementarity values; the results gave strong emphasis to the southern parts of the country, but most of the locations appeared to be equidistant from one another, most likely because of insufficient data. Results demonstrate that the use of a survey gap analysis tool designed to solve a locational problem using continuous environmental data can help maximize our resources for gathering new information on biodiversity. (c) 2005 The Linnean Society of London. C1 Smithsonian Inst, US Natl Herbarium, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. Univ Queensland, Dept Zool & Entomol, Cooperat Res Ctr Rainforest Ecol & Management, Brisbane, Qld 4072, Australia. New S Wales Dept Environm & Conservat, Armidale, NSW 2305, Australia. RP Funk, VA (reprint author), Smithsonian Inst, US Natl Herbarium, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. EM funkv@si.edu RI Ferrier, Simon/C-1490-2009 OI Ferrier, Simon/0000-0001-7884-2388 NR 36 TC 47 Z9 52 U1 1 U2 10 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD AUG PY 2005 VL 85 IS 4 BP 549 EP 567 DI 10.1111/j.1095-8312.2005.00520.x PG 19 WC Evolutionary Biology SC Evolutionary Biology GA 953DW UT WOS:000231057700012 ER PT J AU Venzke, E AF Venzke, E 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, v. 29, no. 11, November 2004 (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 AUG PY 2005 VL 67 IS 7 BP 689 EP 690 DI 10.1007/s00445-005-0420-z PG 2 WC Geosciences, Multidisciplinary SC Geology GA 953GQ UT WOS:000231065000007 ER PT J AU Philpott, SM Foster, PF AF Philpott, SM Foster, PF TI Nest-site limitation in coffee agroecosystems: Artificial nests maintain diversity of arboreal ants SO ECOLOGICAL APPLICATIONS LA English DT Article DE biodiversity loss; biological control; Chiapas; Mexico; coffee agroecosystem; nest-site limitation; recruitment limitation; twig-nesting ants ID TROPICAL RAIN-FOREST; SPECIES RICHNESS; SOUTHERN MEXICO; SHADE COFFEE; BIODIVERSITY; COMPETITION; PLANTATIONS; PLANT; COMMUNITIES; HYMENOPTERA AB Nest sites are a limiting resource for arboreal twig-nesting ants, and nest sites may be increasingly limited with habitat modification. One such habitat modification is the conversion of traditional coffee farms, where coffee is cultivated under a dense, diverse shade canopy, to more intensive production systems with reduced canopy cover and lower diversity, height, and density of shade trees. As a result of such management intensification, ant diversity declines. We ask here if: (1) nest sites are a limiting resource for arboreal twig-nesting ants in coffee farms, especially in intensively managed systems and (2) nest-site limitation is a mechanism causing loss of ant diversity,with coffee management intensification. During 2000-2003, we investigated occupancy, species richness, and species composition of arboreal twig-nesting ants using natural (hollow coffee twig) and artificial (bamboo stem) nests in farms either with high or low diversity and density of shade trees. In both high- and low-shade sites ants occupied a majority (>55%) of natural nests and occupied some (>15%) artificial nests, and significantly more artificial nests were occupied in low-shade sites. In both high- and low-shade sites, ant richness was higher in artificial than in natural nests. More species occupied natural nests in low-shade sites, and more species occupied artificial nests in high-shade sites. Furthermore, species composition differed between nest types, with more ant species found more often or only in artificial nests. These results indicate that, although ants are not strongly nest-site limited in coffee agroecosystems, nest limitation increases somewhat with increasing management intensification. Reductions in numbers of nest sites may be a mechanism causing ant diversity loss with coffee management intensification. Interestingly, because relatively fewer species colonized artificial nests in the low-shade site, ants may be recruitment limited in the low-shade sites, possibly maintaining low ant richness in these sites. C1 Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM philpotts@si.edu NR 59 TC 67 Z9 70 U1 0 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD AUG PY 2005 VL 15 IS 4 BP 1478 EP 1485 DI 10.1890/04-1496 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 950SE UT WOS:000230876900034 ER PT J AU Gallegos, CL Jordan, TE Hines, AH Weller, DE AF Gallegos, CL Jordan, TE Hines, AH Weller, DE TI Temporal variability of optical properties in a shallow, eutrophic estuary: Seasonal and interannual variability SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE optical properties; estuary; absorption coefficient; scattering coefficient; suspended solids ID DIFFUSE ATTENUATION COEFFICIENT; MODERATELY TURBID ESTUARY; RHODE RIVER ESTUARY; CHESAPEAKE BAY; WATER-QUALITY; WEIGHT RELATIONSHIPS; SPECTRAL ABSORPTION; PARTICULATE MATTER; BLUE CRABS; IN-SITU AB We monitored inherent optical properties in a turbid, eutrophic estuary to determine the factors affecting the temporal variability in water clarity. Time series of absorption and scattering coefficients were measured at 1-h intervals for nearly 2 years. The seasonal pattern in weekly averaged absorption and scattering coefficients in each year was driven primarily by changes in the particulate matter of both biogenic and mineral origin. Temporal patterns in particulate absorption and scattering resulted from identifiable events that differed in relative magnitude between the 2 years: a spring bloom was followed by a transient "clear-water" phase, followed by increases in non-algal particulate matter to a late-summer maximum, and rapid declines of all parameters in late fall. Interannual variability in the spring bloom was governed by timing and magnitude of nutrient inputs from the watershed, while major patterns in summer variability of both organic and inorganic particulate matter appeared to follow the general cycle of biological activity in the system. (c) 2005 Elsevier Ltd. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegosc@si.edu OI Gallegos, Charles/0000-0001-5112-0166; Weller, Donald/0000-0002-7629-5437 NR 53 TC 49 Z9 49 U1 0 U2 12 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 AUG PY 2005 VL 64 IS 2-3 BP 156 EP 170 DI 10.1016/j.ecss.2005.01.013 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 950QV UT WOS:000230873200002 ER PT J AU Minton, MS Verling, E Miller, AW Ruiz, GM AF Minton, MS Verling, E Miller, AW Ruiz, GM TI Reducing propagule supply and cosateal invasions via ships: effects of emerging strategies SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID BIOLOGICAL INVASIONS; BALLAST-WATER; PATTERNS AB Ships' ballast water is a leading mechanism for the transport and introduction of nonindigenous species to ports worldwide. Two management strategies are being advanced to reduce propagule supply and invasions from overseas shipping. Ballast water exchange (BWE) is now required by several nations and is expected to be replaced by discharge standards (maximum organismal concentrations), negotiated as a treaty within the International Maritime Organization (IMO). Here, we provide the first forecast and comparison of changes to propagule supply at a national scale, resulting from these alternate management strategies. For unmanaged ballast water, sampled ships (n = 354) arriving to the US typically contained zooplankton concentrations < 3000 organisms m(-3), but some ships (1.1%) contained > 50 000 organisms m(-3). Only 3.8% of these arrivals :meet the IMO standards. BWE substantially reduces zooplankton concentrations, but we estimate that <= 17.2% Of BWE ships will meet IMO standards. Although most overseas arrivals discharged < 1500 m(3) of ballast water, discharges are reported as high as 103 +/- 000 m, and total inocula >= 10(6) remain possible, even under the more stringent IMO strategy. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Minton, MS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM mintonm@si.edu OI Ruiz, Gregory/0000-0003-2499-441X; Minton, Mark/0000-0002-9439-4930; Miller, Whitman/0000-0003-0484-182X NR 20 TC 48 Z9 50 U1 0 U2 17 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 AUG PY 2005 VL 3 IS 6 BP 304 EP 308 DI 10.1890/1540-9295(2005)003[0304:RPSACI]2.0.CO;2 PG 5 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 950MH UT WOS:000230860900016 ER EF