FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Turmel, MS Espinosa, J Franco, L Perez, C Hernandez, H Gonzalez, E Fernandez, G Rojas, C Sanchez, D Fernandez, N Barrios, M Whalen, JK Turner, BL AF Turmel, Marie-Soleil Espinosa, Juan Franco, Leon Perez, Candelario Hernandez, Horacio Gonzalez, Eric Fernandez, Guillermo Rojas, Carlos Sanchez, Daniel Fernandez, Nicolas Barrios, Manuel Whalen, Joann K. Turner, Benjamin L. TI On-farm evaluation of a low-input rice production system in Panama SO PADDY AND WATER ENVIRONMENT LA English DT Article DE Low-input agriculture; Panama; Potassium; Rice; Soil fertility; System of Rice Intensification (SRI) AB On-farm trials were conducted to evaluate the potential of the System of Rice Intensification (SRI), a low-input crop management system, to increase rice yields and reduce water consumption on subsistence farms in several regions of Panama and to determine how inherent soil fertility might affect SRI yields and the yield response to SRI management in the first season of SRI management. SRI practices increased yield by 47% on average and showed potential to increase yield by over 90%, while reducing water consumption by as much as 86%. SRI yields were correlated with available soil K and the difference between SRI and the conventional system yields was positively correlated with extractable Ca, Mg and Mn. The results of this study indicate that SRI is a promising rice production system for smallholder farmers in rural Panama farming under Panamanian soil conditions. C1 [Turmel, Marie-Soleil; Whalen, Joann K.] McGill Univ, Dept Nat Resource Sci, Montreal, PQ, Canada. [Turmel, Marie-Soleil; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Espinosa, Juan; Franco, Leon; Perez, Candelario; Hernandez, Horacio; Gonzalez, Eric; Fernandez, Guillermo; Rojas, Carlos; Sanchez, Daniel; Fernandez, Nicolas; Barrios, Manuel] Patronato Nutr, Panama City, Panama. RP Turmel, MS (reprint author), McGill Univ, Dept Nat Resource Sci, Montreal, PQ, Canada. EM msturmel@gmail.com RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU International Development Research Center; National Sciences and Engineering Research Council of Canada FX The funding for this research was provided by the International Development Research Center and the National Sciences and Engineering Research Council of Canada. NR 13 TC 3 Z9 3 U1 0 U2 4 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1611-2490 J9 PADDY WATER ENVIRON JI Paddy Water Environ. PD MAR PY 2011 VL 9 IS 1 SI SI BP 155 EP 161 DI 10.1007/s10333-010-0227-1 PG 7 WC Agricultural Engineering; Agronomy SC Agriculture GA 732HR UT WOS:000288176100018 ER PT J AU Power, ML AF Power, M. L. TI The human obesity epidemic, the mismatch paradigm, and our modern "captive" environment SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Meeting Abstract C1 [Power, M. L.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAR-APR PY 2011 VL 23 IS 2 BP 272 EP 273 PG 2 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 724GN UT WOS:000287564200085 ER PT J AU Aguerri, JAL Girardi, M Boschin, W Barrena, R Mendez-Abreu, J Sanchez-Janssen, R Borgani, S Castro-Rodriguez, N Corsini, EM del Burgo, C D'Onghia, E Iglesias-Paramo, J Napolitano, N Vilchez, JM AF Aguerri, J. A. L. Girardi, M. Boschin, W. Barrena, R. Mendez-Abreu, J. Sanchez-Janssen, R. Borgani, S. Castro-Rodriguez, N. Corsini, E. M. del Burgo, C. D'Onghia, E. Iglesias-Paramo, J. Napolitano, N. Vilchez, J. M. TI Fossil groups origins I. RX J105453.3+552102 a very massive and relaxed system at z similar to 0.5 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: RX J105453.3+552102; galaxies: groups: general; galaxies: kinematics and dynamics; galaxies: luminosity function, mass function; galaxies: elliptical and lenticular, cD; galaxies: evolution ID BRIGHTEST CLUSTER GALAXIES; DIGITAL SKY SURVEY; SURVEY COMMISSIONING DATA; SCALE-INDEPENDENT METHOD; LUMINOSITY FUNCTION; X-RAY; INTRACLUSTER LIGHT; VELOCITY DISPERSIONS; NUMBER COUNTS; RICH CLUSTERS AB Context. The most accepted scenario for the origin of fossil groups is that they are galaxy associations in which the merging rate was fast and efficient. These systems have assembled half of their mass at early epoch of the Universe, subsequently growing by minor mergers, and therefore could contain a fossil record of the galaxy structure formation. Aims. We have started an observational project in order to characterize a large sample of fossil groups. In this paper we present the analysis of the fossil system RX J105453.3+552102. Methods. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members. Results. RX J105453.3+552102 is located at < z > = 0.47, and shows a quite large line-of-sight velocity dispersion sigma(nu) similar to 1000 km s(-1). Assuming the dynamical equilibrium, we estimated a virial mass of M( -3, v(t) = 0 Q branch, and includes 25 E-type and 2 A-type transitions. The 1061 GHz methanol band (observed in HIFI band 4b) is dominated by the Delta J = 0, K = 7 -> 6, v(t) = 0 Q branch transitions which are mostly blended. We have used the isolated E-type vt = 0 methanol transitions to explore the physical conditions in the molecular gas. With HIFI's high velocity resolution, the methanol emission contributed by different spatial components along the line of sight toward Orion KL (hot core, low velocity flow, and compact ridge) can be distinguished and studied separately. The isolated transitions detected in these bands cover a broad energy range (upper state energy ranging from 80 K to 900 K), which provides a unique probe of the thermal structure in each spatial component. The observations further show that the compact ridge is externally heated. These observations demonstrate the power of methanol lines as probes of the physical conditions in warm regions in close proximity to young stars. C1 [Wang, S.; Bergin, E. A.; Crockett, N. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Goldsmith, P. F.; Pearson, J. C.; Gupta, H.; Langer, W. D.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lis, D. C.; Bell, T. A.; Emprechtinger, M.; Phillips, T. G.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Schilke, P.; Comito, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Schilke, P.; Giesen, T. F.; Mueller, H. S. P.; Qin, S-L; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Daniel, F.; Perault, M.] Observ Paris, CNRS, UMR8112, LERMA, F-75231 Paris 05, France. [Daniel, F.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M-L] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M-L; Ossenkopf, V.] Observ Paris, UMR8102, LUTH, Meudon, France. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron & Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. RP Wang, S (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM shiya@umich.edu RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016; OI Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; Maret, Sebastien/0000-0003-1104-4554; Mueller, Holger/0000-0002-0183-8927 FU NASA FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; The Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. The HEXOS team also is grateful to the HIFI instrument team for building a fantastic instrument. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 23 TC 24 Z9 24 U1 0 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2011 VL 527 AR A95 DI 10.1051/0004-6361/201015079 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 723CP UT WOS:000287484100110 ER PT J AU Deichmann, JL Lima, AP Williamson, GB AF Deichmann, Jessica L. Lima, Albertina P. Williamson, G. Bruce TI Effects of Geomorphology and Primary Productivity on Amazonian Leaf Litter Herpetofauna SO BIOTROPICA LA English DT Article DE amphibians; biomass; Brazil; Ecuador; reptiles; soil age; trophic cascade ID SPECIES RICHNESS; CENTRAL-AMERICA; SOUTHEAST-ASIA; FOREST; PATTERNS; BIOMASS; DIVERSITY; ABUNDANCE; FROGS; SCALE AB The Amazon Basin, representing the largest expanse of intact tropical rain forest on the planet, harbors the largest diversity of amphibians and reptiles in the world. Limited elevation and climate differences across the Basin belie one major division of upland forests - geomorphological soil age and induced nutrient levels. We hypothesized that secondary consumers in the leaf litter herpetofauna community on ancient soils of Central Amazonia would exhibit reduced biomass compared with those found on younger soils of Western Amazonia, and that population densities on ancient soils could be driven below viable thresholds, reducing species richness. We found overall herpetofauna abundance, biomass and richness on young soils in Ecuador were significantly greater than those on ancient soils in the Brazilian Amazon. Separately, amphibians were only slightly more abundant, but their biomass on younger soils was twice that on ancient soils. Even more impressive was the variation exhibited by lizards: abundance was not significantly different, but biomass was five times greater on younger soils. Diversity of both taxa was greater on young soils. The most important driver of differences in herpetofauna biomass, abundance and possibly diversity across Amazonia may be the underlying geomorphologic differences. Reduced primary productivity on ancient soils appears to reverberate up the food chain, leaving fewer resources for higher trophic levels. We suggest that conservation initiatives must compensate for reduced biomass on ancient soils through increased reserve size, especially as forest fragmentation escalates. This study highlights the importance of including biomass as a standard measure in herpetofauna sampling. C1 [Deichmann, Jessica L.; Williamson, G. Bruce] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Deichmann, Jessica L.; Williamson, G. Bruce] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, AM, Brazil. [Deichmann, Jessica L.; Williamson, G. Bruce] Smithsonian Trop Res Inst, BR-69011970 Manaus, AM, Brazil. [Lima, Albertina P.] Inst Nacl de Pesquisas da Amazonia, BR-69060001 Manaus, AM, Brazil. RP Deichmann, JL (reprint author), Louisiana State Univ, Dept Biol Sci, 107 Life Sci Bldg, Baton Rouge, LA 70803 USA. EM jessiedeichmann@gmail.com RI Habe, Neusa/D-6316-2011 FU Conservation, Food and Health Foundation; Louisiana Governor's Office of Environmental Education; Louisiana State University Biograds FX We thank the staff at Tiputini, Yasuni and the BDFFP for their help with logistics and M. Rodrigues, A. Enomenga, I. Nenquimo, H. Ahua and J. Fragata for assistance in the field. This work was supported by grants from the Conservation, Food and Health Foundation, Louisiana Governor's Office of Environmental Education and the Louisiana State University Biograds. We are also grateful to W. E. Duellman, R. K. Colwell, J. Heinen, D. Bickford and one anonymous reviewer for providing valuable comments on the manuscript. Herpetofauna sampling procedures were approved by the Louisiana State University Animal Care and Use Committee (Protocol 04-132). Fieldwork was conducted in Ecuador with permission of the Ministerio del Ambiente (004-IC-FA-PNY-RSO) and in Brazil with permits from CNPq (EXC 006-06-C) and IB-AMA (no 222/2006). This is publication #555 in the BDFFP technical series. NR 54 TC 3 Z9 3 U1 5 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2011 VL 43 IS 2 BP 149 EP 156 DI 10.1111/j.1744-7429.2010.00683.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 728CM UT WOS:000287851700003 ER PT J AU Poltz, K Zotz, G AF Poltz, Kerstin Zotz, Gerhard TI Vascular Epiphytes on Isolated Pasture Trees Along a Rainfall Gradient in the Lowlands of Panama SO BIOTROPICA LA English DT Article DE crassulacean acid metabolism; land-use change; mistletoes; plant diversity; rain forest; secondary vegetation ID CRASSULACEAN ACID METABOLISM; TROPICAL FOREST; PHYSIOLOGICAL ECOLOGY; DIVERSITY; MEXICO; CONSERVATION; VEGETATION; VERACRUZ; ORCHIDS; BROMELIACEAE AB Secondary habitats are increasing in importance in tropical countries due to ongoing destruction of pristine vegetation. In spite of the magnitude of current changes, our understanding of their effects on nontrees (e.g., nonvascular or vascular epiphytes) is still very patchy, particularly in lowland habitats. Here, we report a study with isolated pasture trees in southwest Panama. The > 800 studied trees, which belonged to > 100 different species, harbored almost 27,000 epiphytes of 83 species. Orchidaceae was the most species-rich family, with almost 60 percent of all species, while Bromeliaceae were most abundant. A rainfall gradient in the study region from ca 1000 to > 3000 mm explained more of the variation in species abundance and richness than host characteristics (e.g., species identity, tree size). The unexpectedly large number of epiphytes in these pastures still represents a substantial change relative to a natural setting, which is suggested by a comparison with a forest inventory under similar climatic conditions. In pastures, species richness was lower as deduced from individual-based rarefaction curves, a larger proportion of species and individuals showed crassulacean acid metabolism, and the relationship of epiphyte abundance/species richness and tree diameter was much less steep. Even the already reduced diversity, however, may be only transient in secondary habitats-the long-term persistence of epiphyte populations in pastures is an open question and has to be addressed by repeated monitoring to fully evaluate the significance of pasture trees for the conservation of vascular epiphytes in tropical lowlands. Abstract in Spanish is available at http://www.blackwell-synergy.com/loi/btp C1 [Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, Inst Biol & Environm Sci, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. [Poltz, Kerstin] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, Inst Biol & Environm Sci, Box 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 51 TC 7 Z9 8 U1 2 U2 15 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2011 VL 43 IS 2 BP 165 EP 172 DI 10.1111/j.1744-7429.2010.00669.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 728CM UT WOS:000287851700005 ER PT J AU Rivera, JHV Ortega-Huerta, MA Sarkar, S Rappole, JH AF Vega Rivera, Jorge H. Ortega-Huerta, Miguel A. Sarkar, Sahotra Rappole, John H. TI Modelling the potential winter distribution of the endangered Black-capped Vireo (Vireo atricapilla) SO BIRD CONSERVATION INTERNATIONAL LA English DT Article ID TROPICAL DECIDUOUS FOREST; SPECIES DISTRIBUTIONS; MEXICO; BIODIVERSITY; PREDICTION; ECOLOGY; SEASON; LIFE AB We applied the ecological niche/habitat modelling approach to predict the potential winter distribution of the endangered Black-capped Vireo Vireo atricapilla. We used historical and current field records along with climatic and topographic variables to generate three different models (Biomapper, Maxent, and GARP). Using field data on species occurrence, a model was selected based on the accuracy of assessment results. A final model was obtained by eliminating those areas mapped as known unsuitable habitat, using high resolution land use/land cover data. The GARP model obtained the best accuracy values. It showed the winter distribution of the Black-capped Vireo to cover an area in western Mexico of about 141,000 km(2) that runs along the Pacific coast from southern Sonora (Rio Yaqui, Alvaro Obregon Dam) to the southern state of Oaxaca (Salina Cruz on the Pacific coast and Matias Romero, and inland). One third of the proposed model's area was located at elevations of 0-500 m, while 83% occurred at elevations < 1,250 m; however, a significant area (17%) consists of sites > 1,250 m in elevation. For the most part, the distribution model proposed closely followed the tropical dry forest boundaries and clearly avoided temperate areas at higher elevations. This situation seems to be critical for the species, since the dry forest is one of most endangered Neotropical ecosystems, both nationally and internationally. Furthermore, the array of areas under protection regimes included only about 7.1% of the predicted wintering area. However, this figure could be misleading when it is considered that some protected areas are just "paper reserves" without significant conservation programmes developed in situ. C1 [Vega Rivera, Jorge H.; Ortega-Huerta, Miguel A.] UNAM, Inst Biol, Estn Biol Chamela, Chamela, Jalisco, Mexico. [Sarkar, Sahotra] Univ Texas Austin, Sect Integrat Biol, Biodivers & Biocultural Conservat Lab, Austin, TX 78712 USA. [Rappole, John H.] Smithsonian Conservat & Res Ctr, Front Royal, VA USA. RP Rivera, JHV (reprint author), UNAM, Inst Biol, Estn Biol Chamela, Km 59,200 Barra Navidad Puerto Vallarta, Chamela, Jalisco, Mexico. EM jhvga@ibiologia.unam.mx FU UNAM though the Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica [PAPIIT IN218803] FX We thank Rocio Guerrero and Andres Garcia for his help in the field. Logistical support (vehicles, equipment and office space) was provided by Estacion de Biologia Chamela, Instituto de Biologia, UNAM. We thank Simon Gilling, Tomislav Hengl, and two anonymous reviewers for insightful comments that greatly improved the manuscript. Funding for fieldwork was provided by UNAM though the Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica, (PAPIIT IN218803) to JV and MO. NR 61 TC 2 Z9 3 U1 0 U2 17 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0959-2709 J9 BIRD CONSERV INT JI Bird Conserv. Int. PD MAR PY 2011 VL 21 IS 1 BP 92 EP 106 DI 10.1017/S0959270910000365 PG 15 WC Ornithology SC Zoology GA 731CZ UT WOS:000288085200010 ER PT J AU Risaliti, G Salvati, M Marconi, A AF Risaliti, G. Salvati, M. Marconi, A. TI [O iii] equivalent width and orientation effects in quasars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: general ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; 5TH DATA RELEASE; X-RAY; BLACK-HOLES; EMISSION; GALAXIES; DISKS; LUMINOSITY; SCATTERING AB The flux of the [O iii] lambda 5007-A line is considered to be a good indicator of the bolometric emission of quasars. The observed continuum emission from the accretion disc should instead be strongly dependent on the inclination angle theta between the disc axis and the line of sight. Based on this, the equivalent width (EW) of [O iii] should provide a direct measure of theta. Here we analyse the distribution of EW([O iii]) in a sample of similar to 6000 Sloan Digital Sky Survey quasars, and find that it can be accurately reproduced assuming a relatively small intrinsic scatter and a random distribution of inclination angles. This result has several implications: (1) it is a direct proof of the disc-like emission of the optical continuum of quasars; (2) the value of EW([O iii]) can be used as a proxy of the inclination, to correct the measured continuum emission and then estimate the bolometric luminosity of quasars and (3) the presence of almost edge-on discs among broad-line quasars implies that the accretion disc is not aligned with the circumnuclear absorber, and/or that the covering fraction of the latter is rather small. Finally, we show that a similar analysis of EW distributions of broad lines (H beta, Mg ii and C iv) provides no evidence of inclination effects, suggesting a disc-like geometry of the broad emission line region. C1 [Risaliti, G.; Salvati, M.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marconi, A.] Univ Florence, Dipartimento Fis & Astron, Florence, Italy. RP Risaliti, G (reprint author), INAF Osservatorio Astrofis Arcetri, Lgo E Fermi 5, Florence, Italy. EM grisaliti@cfa.harvard.edu RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti, Guido/0000-0002-3556-977X FU NASA [NNX10AF50G] FX We are grateful to the referee for his/her careful reading and constructive comments. This work has been partly supported by NASA grants NNX10AF50G. NR 30 TC 23 Z9 23 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2011 VL 411 IS 4 BP 2223 EP 2229 DI 10.1111/j.1365-2966.2010.17843.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 728FF UT WOS:000287859200009 ER PT J AU Domenech-Carbo, MT Silva, MF Aura-Castro, E Fuster-Lopez, L Kroner, S Martinez-Bazan, ML Mas-Barbera, X Mecklenburg, MF Osete-Cortina, L Domenech, A Gimeno-Adelantado, JV Yusa-Marco, DJ AF Teresa Domenech-Carbo, Maria Silva, Miguel F. Aura-Castro, Elvira Fuster-Lopez, Laura Kroener, Stephan Luisa Martinez-Bazan, Maria Mas-Barbera, Xavier Mecklenburg, Marion F. Osete-Cortina, Laura Domenech, Antonio Vicente Gimeno-Adelantado, Jose Julia Yusa-Marco, Dolores TI Study of behaviour on simulated daylight ageing of artists' acrylic and poly(vinyl acetate) paint films SO ANALYTICAL AND BIOANALYTICAL CHEMISTRY LA English DT Article; Proceedings Paper CT 8th Polish Conference on Analytical Chemistry CY JUL 04-09, 2010 CL Krakow, POLAND DE Surfactant; Acrylic artists' paint; PVAc paint; FTIR spectroscopy; AFM; Tensile tests ID POLY(ETHYLENE GLYCOL) ADDITIVES; LATEX FILMS; MASS-SPECTROMETRY; MALDI-MS; ESI-MS; IDENTIFICATION; POLYMERS; MEDIA AB This work proposes a multi-method approach that combines advanced microscopy (SEM/EDX, AFM) and spectroscopy (UV-vis and FTIR) techniques. This approach not only characterises the behaviour of the additives of two commercial poly(vinyl acetate) (PVAc) and acrylic emulsion paints but also simultaneously characterises the changes in chemical composition and morphology observed in the paint films as a result of ageing due to the paints being exposed to an intense source of simulated daylight. In parallel, a series of mechanical tests were performed that correlate the chemical changes in composition and the changes observed in the films' mechanical properties. This work was a comparative study between both types of acrylic and PVAc paints. The results obtained are of great interest for the modern paint conservation field as they provide valuable information on the mid- and long-term behaviours of these synthetic paints. C1 [Teresa Domenech-Carbo, Maria; Silva, Miguel F.; Aura-Castro, Elvira; Fuster-Lopez, Laura; Kroener, Stephan; Luisa Martinez-Bazan, Maria; Mas-Barbera, Xavier; Osete-Cortina, Laura; Julia Yusa-Marco, Dolores] Univ Politecn Valencia, Inst Restaurac Patrimonio, Valencia 46022, Spain. [Mecklenburg, Marion F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Domenech, Antonio; Vicente Gimeno-Adelantado, Jose] Univ Valencia, Fac Quim, E-46100 Burjassot, Spain. RP Domenech-Carbo, MT (reprint author), Univ Politecn Valencia, Inst Restaurac Patrimonio, Camino Vera S-N, Valencia 46022, Spain. EM tdomenec@crbc.upv.es RI FUSTER-LOPEZ, Laura/F-5503-2016 FU Spanish "I+D+I MICINN" [CTQ2008-06727-C03-01/BQU]; Universitary Researchers in Spanish Universities and Research Centres from the Spanish Ministry of Science and Innovation (MICINN) [ACOMP/2009/171, AP2006-3223] FX Financial support is gratefully acknowledged from the Spanish "I+D+I MICINN" project CTQ2008-06727-C03-01/BQU supported by ERDEF funds and from the "Generalitat Valenciana" I+D project ACOMP/2009/171 and the AP2006-3223 project ascribed to the Predoctoral Stages Programme of Universitary Researchers in Spanish Universities and Research Centres from the Spanish Ministry of Science and Innovation (MICINN). The authors wish to thank Mr. Manuel Planes i Insausti and Dr. Jose Luis Moya Lopez, the technical supervisors responsible for the Electron Microscopy Service at the Polytechnic University of Valencia. NR 32 TC 10 Z9 10 U1 0 U2 19 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1618-2642 EI 1618-2650 J9 ANAL BIOANAL CHEM JI Anal. Bioanal. Chem. PD MAR PY 2011 VL 399 IS 9 BP 2921 EP 2937 DI 10.1007/s00216-010-4294-3 PG 17 WC Biochemical Research Methods; Chemistry, Analytical SC Biochemistry & Molecular Biology; Chemistry GA 726EW UT WOS:000287703000005 PM 20981537 ER PT J AU Kawashima, T Thorington, RW AF Kawashima, Tomokazu Thorington, Richard W., Jr. TI Comparative Morphological Configuration of the Cardiac Nervous System in Lorises and Galagos (Infraorder Lorisiformes, Strepsirrhini, Primates) with Evolutionary Perspective SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE Loris; Galago; Lorisiformes; cardiac nerve; cardiac branch; heart; comparative anatomy; primate evolution ID RHESUS-MONKEY; WORLD MONKEYS; ANATOMY AB The detailed systematic morphology and comparative anatomy of the autonomic cardiac nervous system (ACNS) with its surrounding structures were examined in 14 sides of 7 Lorisiformes species (lorises and galagos) to consider its evolutionary differences and similarities to others in the primate lineage. Our detailed descriptions clarified that (1) a family-dependent morphology of the ACNS does not exist although several variations are recognized as common variation in Lorisiformes, (2) the morphology of the ACNS in Lorisiformes is almost consistent regardless of the number of presacral vertebrae and cardiac positions, and (3) the ACNS morphology in Lorisiformes is extremely different from that in New and Old World monkeys, gibbons, and human, specifically in a narrower contribution of the superior cervical ganglion to the spinal cervical nerves, the caudal position and organization of the cervicothoracic ganglion, and the narrower origins of the sympathetic cardiac nerves, although all parasympathetic vagal cardiac branches are consistently present among the primates. Based on these detailed findings, the systematic and evolutionary morphologies of the ACNS are discussed and compared with our previous works. These results suggest the primate ACNS preserves its evolutionary history without modification and specialization by its functional adaptation as seen in the somatic system. Anat Rec, 294:412-426, 2011. (C) 2011 Wiley-Liss, Inc. C1 [Kawashima, Tomokazu; Thorington, Richard W., Jr.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, Washington, DC 20560 USA. RP Kawashima, T (reprint author), Tokyo Womens Med Univ, Sch Med, Dept Anat, Shinjuku Ku, 8-1 Kawada Cho, Tokyo 1628666, Japan. EM kawa@research.twmu.ac.jp FU Japanese Ministry of Education, Culture, Sports, Science, and Technology [16790804, 19790985, 2008TWMU001] FX Grant sponsor: Scientific Research from the Japanese Ministry of Education, Culture, Sports, Science, and Technology (2004-2006 and 2007-2009); Grant numbers: 16790804, 19790985; Grant sponsor: International Research Program by the Japanese Ministry of Education, Culture, Sports, Science, and Technology (2008-2009); Grant number: 2008TWMU001. NR 57 TC 6 Z9 6 U1 0 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1932-8486 J9 ANAT REC JI Anat. Rec. PD MAR PY 2011 VL 294 IS 3 BP 412 EP 426 DI 10.1002/ar.21334 PG 15 WC Anatomy & Morphology SC Anatomy & Morphology GA 725UN UT WOS:000287671700007 PM 21284093 ER PT J AU Fernandez-Lopez, M Curiel, S Girart, JM Ho, PTP Patel, N Gomez, Y AF Fernandez-Lopez, M. Curiel, S. Girart, J. M. Ho, P. T. P. Patel, N. Gomez, Y. TI MILLIMETER AND SUBMILLIMETER HIGH ANGULAR RESOLUTION INTERFEROMETRIC OBSERVATIONS: DUST IN THE HEART OF IRAS 18162-2048 SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: individual objects (GGD27, HH 80-81, IRAS 18162-2048); stars: early-type; stars: formation; submillimeter: ISM ID HERBIG-HARO OBJECTS; MASSIVE STAR-FORMATION; ULTRACOMPACT HII-REGIONS; YOUNG STELLAR OBJECTS; THERMAL RADIO JET; HH 80-81; CONTINUUM OBSERVATIONS; FORMING REGIONS; H2O MASERS; VLA OBSERVATIONS AB The GGD27 complex includes the HH 80-81-80N system, which is one of the most powerful molecular outflows associated with a high-mass star-forming region observed to date. This outflow is powered by the star associated with the source IRAS 18162-2048. Here, we report on the detection of continuum emission at subarcsec/arcsec resolution with the Submillimeter Array (SMA) at 1.36 mm and 456 mu m, respectively. We detected dust emission arising from two compact cores, MM1 and MM2, separated by about 7 '' (similar to 12,000 AU in projected distance). MM1 spatially coincides with the powerful thermal radio continuum jet that powers the very extended molecular outflow, while MM2 is associated with the protostar that drives the compact molecular outflow recently found in this region. High angular resolution observations at 1.36 mm show that MM1 is unresolved and that MM2 splits into two subcomponents separated by similar to 1 ''. The mass of MM1 is about 4M(circle dot) and it has a size of less than or similar to 300 AU. This is consistent with MM1 being associated with a massive and dense (n(H-2) greater than or similar to 10(9) cm(-3)) circumstellar dusty disk surrounding a high-mass protostar, which has not yet developed a compact H II region. On the other hand, the masses of the two separate components of MM2 are about 2 M-circle dot each. One of these components is a compact core with an intermediate-mass young protostar inside and the other component is probably a prestellar core. MM1 is the brightest source at 1.36 mm, while MM2 dominates the emission at 456 mu m. These are the only (sub) millimeter sources detected in the SMA observations. Hence, it seems that both sources may contribute significantly to the bolometric luminosity of the region. Finally, we argue that the characteristics of these two sources indicate that MM2 is probably in an earlier evolutionary stage than MM1. C1 [Fernandez-Lopez, M.; Curiel, S.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Girart, J. M.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Bellaterra 08193, Catalunya, Spain. [Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, P. T. P.; Patel, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gomez, Y.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Fernandez-Lopez, M (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. EM manferna@gmail.com; scuriel@astroscu.unam.mx; girart@ieec.cat; y.gomez@astrosmo.unam.mx RI Girart, Josep/O-1638-2014 OI Girart, Josep/0000-0002-3829-5591 NR 76 TC 14 Z9 14 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 MAR PY 2011 VL 141 IS 3 AR 72 DI 10.1088/0004-6256/141/3/72 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 719TC UT WOS:000287231000003 ER PT J AU Acciari, VA Arlen, T Aune, T Beilicke, M Benbow, W Bottcher, M Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Cannon, A Cesarini, A Ciupik, L Cui, W Dickherber, R Duke, C Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Huang, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Madhavan, AS Maier, G McArthur, S McCann, A Moriarty, P Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Steele, D Swordy, SP Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wood, M Zitzer, B Aleksic, J Antonelli, LA Antoranz, P Backes, M Barrio, JA Bastieri, D Gonzalez, JB Bednarek, W Berdyugin, A Berger, K Bernardini, E Biland, A Blanch, O Bock, RK Boller, A Bonnoli, G Bordas, P Tridon, DB Bosch-Ramon, V Bose, D Braun, I Bretz, T Camara, M Carmona, E Carosi, A Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Dazzi, F De Angelis, A Del Pozo, ED De Lotto, B De Maria, M De Sabata, F Mendez, CD Ortega, AD Doert, M Dominguez, A Prester, DD Dorner, D Doro, M Elsaesser, D Errando, M Ferenc, D Fonseca, MV Font, L Lopez, RJG Garczarczyk, M Gaug, M Giavitto, G Godinovic, N Hadasch, D Herrero, A Hildebrand, D Hohne-Monch, D Hose, J Hrupec, D Jogler, T Klepser, S Krahenbuhl, T Kranich, D Krause, J La Barbera, A Leonardo, E Lindfors, E Lombardi, S Longo, F Lopez, M Lorenz, E Majumdar, P Makariev, M Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Mariotti, M Martinez, M Mazin, D Meucci, M Miranda, JM Mirzoyan, R Miyamoto, H Moldon, J Moralejo, A Nieto, D Nilsson, K Orito, R Oya, I Paoletti, R Paredes, JM Partini, S Pasanen, M Pauss, F Pegna, RG Perez-Torres, MA Persic, M Peruzzo, L Pochon, J Prada, F Moroni, PGP Prandini, E Puchades, N Puljak, I Reichardt, I Reinthal, R Rhode, W Ribo, M Rico, J Rissi, M Rugamer, S Saggion, A Saito, K Saito, TY Salvati, M Sanchez-Conde, M Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shayduk, M Shore, SN Sierpowska-Bartosik, A Sillanpaa, A Sitarek, J Sobczynska, D Spanier, F Spiro, S Stamerra, A Steinke, B Storz, J Strah, N Struebig, JC Suric, T Takalo, L Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Torres, DF Vankov, H Wagner, RM Weitzel, Q Zabalza, V Zandanel, F Zanin, R Paneque, D Hayashida, M AF Acciari, V. A. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boettcher, M. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Cannon, A. Cesarini, A. Ciupik, L. Cui, W. Dickherber, R. Duke, C. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Huang, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Madhavan, A. S. Maier, G. McArthur, S. McCann, A. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Steele, D. Swordy, S. P. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wood, M. Zitzer, B. Aleksic, J. Antonelli, L. A. Antoranz, P. Backes, M. Barrio, J. A. Bastieri, D. Becerra Gonzalez, J. Bednarek, W. Berdyugin, A. Berger, K. Bernardini, E. Biland, A. Blanch, O. Bock, R. K. Boller, A. Bonnoli, G. Bordas, P. Tridon, D. Borla Bosch-Ramon, V. Bose, D. Braun, I. Bretz, T. Camara, M. Carmona, E. Carosi, A. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Dazzi, F. De Angelis, A. De Cea Del Pozo, E. De Lotto, B. De Maria, M. De Sabata, F. Delgado Mendez, C. Diago Ortega, A. Doert, M. Dominguez, A. Prester, D. Dominis Dorner, D. Doro, M. Elsaesser, D. Errando, M. Ferenc, D. Fonseca, M. V. Font, L. Garcia Lopez, R. J. Garczarczyk, M. Gaug, M. Giavitto, G. Godinovic, N. Hadasch, D. Herrero, A. Hildebrand, D. Hoehne-Moench, D. Hose, J. Hrupec, D. Jogler, T. Klepser, S. Kraehenbuehl, T. Kranich, D. Krause, J. La Barbera, A. Leonardo, E. Lindfors, E. Lombardi, S. Longo, F. Lopez, M. Lorenz, E. Majumdar, P. Makariev, M. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Mariotti, M. Martinez, M. Mazin, D. Meucci, M. Miranda, J. M. Mirzoyan, R. Miyamoto, H. Moldon, J. Moralejo, A. Nieto, D. Nilsson, K. Orito, R. Oya, I. Paoletti, R. Paredes, J. M. Partini, S. Pasanen, M. Pauss, F. Pegna, R. G. Perez-Torres, M. A. Persic, M. Peruzzo, L. Pochon, J. Prada, F. Moroni, P. G. Prada Prandini, E. Puchades, N. Puljak, I. Reichardt, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Rissi, M. Ruegamer, S. Saggion, A. Saito, K. Saito, T. Y. Salvati, M. Sanchez-Conde, M. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Shayduk, M. Shore, S. N. Sierpowska-Bartosik, A. Sillanpaa, A. Sitarek, J. Sobczynska, D. Spanier, F. Spiro, S. Stamerra, A. Steinke, B. Storz, J. Strah, N. Struebig, J. C. Suric, T. Takalo, L. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Torres, D. F. Vankov, H. Wagner, R. M. Weitzel, Q. Zabalza, V. Zandanel, F. Zanin, R. Paneque, D. Hayashida, M. CA VERITAS Collaboration MAGIC Collaboration TI SPECTRAL ENERGY DISTRIBUTION OF MARKARIAN 501: QUIESCENT STATE VERSUS EXTREME OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (Markarian 501=VER J1653+397); galaxies: active; gamma rays: galaxies; radiation mechanisms: non-thermal; X-rays: galaxies ID GAMMA-RAY EMISSION; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; X-RAY; MULTIWAVELENGTH OBSERVATIONS; RADIATION; BLAZAR; PERFORMANCE; EVOLUTION; ASTRONOMY AB The very high energy (VHE; E > 100 GeV) blazar Markarian 501 (Mrk 501) has a well-studied history of extreme spectral variability and is an excellent laboratory for studying the physical processes within the jets of active galactic nuclei. However, there are few detailed multiwavelength studies of Mrk 501 during its quiescent state, due to its low luminosity. A short-term multiwavelength study of Mrk 501 was coordinated in 2009 March, focusing around a multi-day observation with the Suzaku X-ray satellite and including gamma-ray data from VERITAS, MAGIC, and the Fermi Gamma-ray Space Telescope with the goal of providing a well-sampled multiwavelength baseline measurement of Mrk 501 in the quiescent state. The results of these quiescent-state observations are compared to the historically extreme outburst of 1997 April 16, with the goal of examining variability of the spectral energy distribution (SED) between the two states. The derived broadband SED shows the characteristic double-peaked profile. We find that the X-ray peak shifts by over two orders of magnitude in photon energy between the two flux states while the VHE peak varies little. The limited shift in the VHE peak can be explained by the transition to the Klein-Nishina (KN) regime. Synchrotron self-Compton models are matched to the data and the implied KN effects are explored. C1 [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Cannon, A.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Errando, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Huang, D.; Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Madhavan, A. S.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Aleksic, J.; Blanch, O.; Cortina, J.; Errando, M.; Giavitto, G.; Klepser, S.; Martinez, M.; Mazin, D.; Moralejo, A.; Puchades, N.; Reichardt, I.; Rico, J.; Tescaro, D.; Zanin, R.] IFAE, E-08193 Bellaterra, Spain. [Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Maraschi, L.; Salvati, M.; Spiro, S.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy. [Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Pegna, R. G.; Moroni, P. G. Prada; Stamerra, A.] Univ Siena, Dipartimento Fis, I-53100 Siena, Italy. [Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Pegna, R. G.; Moroni, P. G. Prada; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy. [Backes, M.; Doert, M.; Rhode, W.; Strah, N.] Tech Univ Dortmund, Fak Phys, D-44221 Dortmund, Germany. [Barrio, J. A.; Bose, D.; Camara, M.; Contreras, J. L.; Fonseca, M. V.; Nieto, D.; Oya, I.] Univ Complutense, Dept Atom Phys, E-28040 Madrid, Spain. [Bastieri, D.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Peruzzo, L.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Univ Padua, Dipartimento Fis, I-35131 Padua, Italy. [Bastieri, D.; Berdyugin, A.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Peruzzo, L.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] INFN, I-35131 Padua, Italy. [Becerra Gonzalez, J.; Berger, K.; Colombo, E.; Delgado Mendez, C.; Diago Ortega, A.; Garcia Lopez, R. J.; Garczarczyk, M.; Gaug, M.; Herrero, A.; Pochon, J.; Sanchez-Conde, M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Becerra Gonzalez, J.; Diago Ortega, A.; Garcia Lopez, R. J.; Herrero, A.; Sanchez-Conde, M.] Depto Astrofis, E-38206 Tenerife, Spain. [Bednarek, W.; Sierpowska-Bartosik, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, Dept Expt Phys, PL-90236 Lodz, Poland. [Berdyugin, A.; Lindfors, E.; Nilsson, K.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, FI-51500 Piikkio, Finland. [Bernardini, E.; Majumdar, P.; Satalecka, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Biland, A.; Boller, A.; Braun, I.; Dorner, D.; Hildebrand, D.; Kraehenbuehl, T.; Kranich, D.; Lorenz, E.; Pauss, F.; Rissi, M.; Weitzel, Q.] ETH, CH-8093 Zurich, Switzerland. [Bock, R. K.; Tridon, D. Borla; Carmona, E.; Colin, P.; Hose, J.; Jogler, T.; Krause, J.; Lorenz, E.; Mirzoyan, R.; Miyamoto, H.; Orito, R.; Saito, K.; Saito, T. Y.; Schweizer, T.; Shayduk, M.; Sitarek, J.; Steinke, B.; Teshima, M.; Wagner, R. M.; Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Bordas, P.; Bosch-Ramon, V.; Moldon, J.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona, Dept Astron & Meteorol, ICC IEEC, E-08028 Barcelona, Spain. [Bretz, T.; Elsaesser, D.; Hoehne-Moench, D.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Storz, J.; Struebig, J. C.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Dazzi, F.; De Angelis, A.; De Lotto, B.; De Maria, M.; De Sabata, F.; Longo, F.; Mankuzhiyil, N.; Persic, M.; Scapin, V.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [Dazzi, F.; De Angelis, A.; De Lotto, B.; De Maria, M.; De Sabata, F.; Longo, F.; Mankuzhiyil, N.; Persic, M.; Scapin, V.] INFN Trieste, I-33100 Udine, Italy. [De Cea Del Pozo, E.; Hadasch, D.; Torres, D. F.] IEEC CSIC, Inst Ciencies Espai, E-08193 Barcelona, Spain. [Dominguez, A.; Perez-Torres, M. A.; Prada, F.; Zandanel, F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Rijeka, Croatian MAGIC Consortium, Inst R Boskovic, HR-10000 Zagreb, Croatia. [Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Split, HR-10000 Zagreb, Croatia. [Dazzi, F.; Font, L.] Univ Autonoma Barcelona, Dept Appl Phys, E-08193 Barcelona, Spain. [Makariev, M.; Maneva, G.; Temnikov, P.; Vankov, H.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria. [Persic, M.] INAF Osservatorio Astron, I-34143 Trieste, Italy. [Persic, M.] INFN, I-34143 Trieste, Italy. [Rico, J.; Torres, D. F.] ICREA, E-08010 Barcelona, Spain. [Shore, S. N.] Univ Pisa, Dipartimento Fis, I-56126 Pisa, Italy. [Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy. [Paneque, D.; Hayashida, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Paneque, D.; Hayashida, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM cui@purdue.edu; daniel-d-gall@uiowa.edu RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; XRAY, SUZAKU/A-1808-2009; Miranda, Jose Miguel/F-2913-2013; Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Maneva, Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Backes, Michael/N-5126-2016; Torres, Diego/O-9422-2016; Reichardt, Ignasi/P-7478-2016; Temnikov, Petar/L-6999-2016; Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017; Prada Moroni, Pier Giorgio/G-5565-2011; Braun, Isabel/C-9373-2012; Mannheim, Karl/F-6705-2012; Doro, Michele/F-9458-2012; Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Lopez Moya, Marcos/L-2304-2014; GAug, Markus/L-2340-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Antoranz, Pedro/H-5095-2015; Delgado, Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; OI Bastieri, Denis/0000-0002-6954-8862; Ribo, Marc/0000-0002-9931-4557; Pandel, Dirk/0000-0003-2085-5586; Covino, Stefano/0000-0001-9078-5507; Bordas, Pol/0000-0002-0266-8536; Paredes, Josep M./0000-0002-1566-9044; Oya, Igor/0000-0002-3881-9324; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; De Angelis, Alessandro/0000-0002-3288-2517; LA BARBERA, ANTONINO/0000-0002-5880-8913; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; leonardo, elvira/0000-0003-0271-7673; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480; Ward, John E/0000-0003-1973-0794; Spanier, Felix/0000-0001-6802-4744; Dominguez, Alberto/0000-0002-3433-4610; Miranda, Jose Miguel/0000-0002-1472-9690; Font, Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Backes, Michael/0000-0002-9326-6400; Torres, Diego/0000-0002-1522-9065; Reichardt, Ignasi/0000-0003-3694-3820; Temnikov, Petar/0000-0002-9559-3384; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Braun, Isabel/0000-0002-9389-0502; Doro, Michele/0000-0001-9104-3214; Rico, Javier/0000-0003-4137-1134; Lopez Moya, Marcos/0000-0002-8791-7908; GAug, Markus/0000-0001-8442-7877; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Antoranz, Pedro/0000-0002-3015-3601; Delgado, Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755; Bonnoli, Giacomo/0000-0003-2464-9077; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022 FU INFN Padova; German BMBF and MPG; Italian INFN; Swiss National Fund SNF; Spanish MICINN; NASA [NNX08AZ98G, NNX08AX53G]; U.S. Department of Energy; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK FX Supported by INFN Padova.; We thank Elena Pian for providing the BeppoSAX data. This work was supported in part by NASA through grants NNX08AZ98G and NNX08AX53G. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and USA (NASA). The VERITAS research is supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and the collaborating institutions in the construction and operation of the instrument.; The MAGIC Collaboration thanks the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 program, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the DFG Cluster of Excellence "Origin and Structure of the Universe," and by the Polish MNiSzW Grant N N203 390834. NR 48 TC 21 Z9 21 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 2 DI 10.1088/0004-637X/729/1/2 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300002 ER PT J AU Chakraborti, S Ray, A AF Chakraborti, Sayan Ray, Alak TI BARYON LOADED RELATIVISTIC BLAST WAVES IN SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; radiation mechanisms: non-thermal; shock waves; supernovae: individual (SN 2009bb); techniques: interferometric ID GAMMA-RAY-BURST; FLUID-DYNAMICS; RADIO-EMISSION; FIREBALL MODEL; LIGHT CURVES; SN 1993J; AFTERGLOW; SYNCHROTRON; HYDRODYNAMICS; RADIATION AB We provide a new analytic blast wave solution which generalizes the Blandford-McKee solution to arbitrary ejecta masses and Lorentz factors. Until recently relativistic supernovae have been discovered only through their association with long-duration gamma-ray bursts (GRBs). The blast waves of such explosions are well described by the Blandford-McKee (in the ultra-relativistic regime) and Sedov-Taylor (in the non-relativistic regime) solutions during their afterglows, as the ejecta mass is negligible in comparison to the swept-up mass. The recent discovery of the relativistic supernova SN 2009bb, without a detected GRB, opens up the possibility of highly baryon loaded, mildly relativistic outflows which remains in nearly free-expansion phase during the radio afterglow. In this work, we consider a massive, relativistic shell, launched by a Central Engine Driven EXplosion (CEDEX), decelerating adiabatically due to its collision with the pre-explosion circumstellar wind profile of the progenitor. We compute the synchrotron emission from relativistic electrons in the shock amplified magnetic field. This models the radio emission from the circumstellar interaction of a CEDEX. We show that this model explains the observed radio evolution of the prototypical SN 2009bb and demonstrate that SN 2009bb had a highly baryon loaded, mildly relativistic outflow. We discuss the effect of baryon loading on the dynamics and observational manifestations of a CEDEX. In particular, our predicted angular size of SN 2009bb is consistent with very long baseline interferometric (VLBI) upper limits on day 85, but is presently resolvable on VLBI angular scales, since the relativistic ejecta is still in the nearly free-expansion phase. C1 [Chakraborti, Sayan; Ray, Alak] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Chakraborti, Sayan; Ray, Alak] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Chakraborti, S (reprint author), Tata Inst Fundamental Res, Dept Astron & Astrophys, 1 Homi Bhabha Rd, Bombay 400005, Maharashtra, India. EM sayan@tifr.res.in; akr@tifr.res.in FU TIFR 11th Five Year Plan Project [11P-409] FX We thank Alicia Soderberg, Abraham Loeb, and Poonam Chandra for discussions on mildly relativistic supernovae. We thank Naveen Yadav for checking the manuscript and Swastik Bhattacharya for help with mathematics. This work has made use of the Wolfram Mathematica computer algebra system. This research was supported by the TIFR 11th Five Year Plan Project No. 11P-409. We thank the Institute for Theory and Computation, Harvard University for its hospitality. We thank an anonymous referee for detailed comments which significantly extended this work, in particular for pointing out to us the Chiang and Dermer papers, which we were unaware of. We thank Charles Dermer for sharing their numerical results in these papers. We thank Tsvi Piran and Charles Dermer for discussions at the Annapolis GRB2010 meeting. NR 48 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 MAR 1 PY 2011 VL 729 IS 1 AR 57 DI 10.1088/0004-637X/729/1/57 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300057 ER PT J AU Das, S Marriage, TA Ade, PAR Aguirre, P Amiri, M Appel, JW Barrientos, LF Battistelli, ES Bond, JR Brown, B Burger, B Chervenak, J Devlin, MJ Dicker, SR Doriese, WB Dunkley, J Dunner, R Essinger-Hileman, T Fisher, RP Fowler, JW Hajian, A Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hilton, GC Hilton, M Hincks, AD Hlozek, R Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Juin, JB Kaul, M Klein, J Kosowsky, A Lau, JM Limon, M Lin, YT Lupton, RH Marsden, D Martocci, K Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Nolta, MR Page, LA Parker, L Partridge, B Reid, B Sehgal, N Sherwin, BD Sievers, J Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Trac, H Tucker, C Warne, R Wollack, E Zhao, Y AF Das, Sudeep Marriage, Tobias A. Ade, Peter A. R. Aguirre, Paula Amiri, Mandana Appel, John W. Barrientos, L. Felipe Battistelli, Elia S. Bond, John R. Brown, Ben Burger, Bryce Chervenak, Jay Devlin, Mark J. Dicker, Simon R. Doriese, W. Bertrand Dunkley, Joanna Duenner, Rolando Essinger-Hileman, Thomas Fisher, Ryan P. Fowler, Joseph W. Hajian, Amir Halpern, Mark Hasselfield, Matthew Hernandez-Monteagudo, Carlos Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin M. Hughes, David H. Hughes, John P. Infante, Leopoldo Irwin, Kent D. Juin, Jean Baptiste Kaul, Madhuri Klein, Jeff Kosowsky, Arthur Lau, Judy M. Limon, Michele Lin, Yen-Ting Lupton, Robert H. Marsden, Danica Martocci, Krista Mauskopf, Phil Menanteau, Felipe Moodley, Kavilan Moseley, Harvey Netterfield, Calvin B. Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Parker, Lucas Partridge, Bruce Reid, Beth Sehgal, Neelima Sherwin, Blake D. Sievers, Jon Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Trac, Hy Tucker, Carole Warne, Ryan Wollack, Ed Zhao, Yue TI THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 AND 218 GHz FROM THE 2008 SOUTHERN SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations ID PROBE WMAP OBSERVATIONS; POLE TELESCOPE; BEAM PROFILES; SOURCE COUNTS; ANISOTROPY; SKY; TEMPERATURE; RADIATION; SIMULATIONS; CONSTRAINTS AB We present measurements of the cosmic microwave background (CMB) power spectrum made by the Atacama Cosmology Telescope at 148 GHz and 218 GHz, as well as the cross-frequency spectrum between the two channels. Our results clearly show the second through the seventh acoustic peaks in the CMB power spectrum. The measurements of these higher-order peaks provide an additional test of the Lambda CDM cosmological model. At l > 3000, we detect power in excess of the primary anisotropy spectrum of the CMB. At lower multipoles 500 < l < 3000, we find evidence for gravitational lensing of the CMB in the power spectrum at the 2.8 sigma level. We also detect a low level of Galactic dust in our maps, which demonstrates that we can recover known faint, diffuse signals. C1 [Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Das, Sudeep; Appel, John W.; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Kosowsky, Arthur; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Das, Sudeep; Marriage, Tobias A.; Dunkley, Joanna; Hajian, Amir; Lin, Yen-Ting; Lupton, Robert H.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aguirre, Paula; Barrientos, L. Felipe; Duenner, Rolando; Infante, Leopoldo; Juin, Jean Baptiste; Lin, Yen-Ting] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Bond, John R.; Hajian, Amir; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Brown, Ben] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Marsden, Danica; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Doriese, W. Bertrand; Fowler, Joseph W.; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa. [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Hughes, David H.] INAOE, Puebla, Mexico. [Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Kosowsky, Arthur; Martocci, Krista; Switzer, Eric R.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. [Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Das, S (reprint author), Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698 FU US National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation under Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; Berkeley Center for Cosmological Physics Fellowship; NASA [NNX08AH30G]; RCUK Fellowship; Rhodes Trust; Natural Science and Engineering Research Council of Canada (NSERC); NSF [AST-0546035, AST-0606975, PHY-0114422]; FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion Andes; South African National Research Foundation (NRF); Meraka Institute; South African Square Kilometer Array (SKA) Project; World Premier International Research Center Initiative, MEXT, Japan; US Department of Energy [DE-AC3-76SF00515]; NASA Office of Space Science FX ACT is on the Chajnantor Science preserve, which was made possible by the Chilean Comision Nacional de Investigacion Cientifica y Tecnologica. We are grateful for the assistance we received at various times from the ALMA, APEX, ASTE, CBI/QUIET, and NANTEN2 groups. The PWV data come from the public APEX weather Web site. Field operations were based at the Don Esteban facility run by Astro-Norte. Reed Plimpton and David Jacobson worked at the telescope during the 2008 season. We thank Norm Jarosik for support throughout the project. This work was supported by the US National Science Foundation through awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731, and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. The PIRE program made possible exchanges between Chile, South Africa, Spain, and the US that enabled this research program. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund-Research Excellence, and the University of Toronto. We thank the referee for useful comments. S. D. acknowledges support from the Berkeley Center for Cosmological Physics Fellowship. S. D. thanks Christian Reichardt and Oliver Zahn for useful discussions. We thank Bruce Bassett for suggestions on testing lensing in the power spectrum. S. D., A. H., and T. M. were supported through NASA grant NNX08AH30G. J. D. acknowledges support from an RCUK Fellowship. R. H. received funding from the Rhodes Trust. A. D. H. received additional support from a Natural Science and Engineering Research Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially supported through NSF AST-0546035 and AST-0606975, respectively, for work on ACT. L. I. acknowledges partial support from FONDAP Centro de Astrofisica. R. D. was supported by CONICYT, MECESUP, and Fundacion Andes. E. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. K. M., M. Hilton, and R. W. received financial support from the South African National Research Foundation (NRF), the Meraka Institute via funding for the South African Centre for High Performance Computing (CHPC), and the South African Square Kilometer Array (SKA) Project. Y.-T.L. acknowledges support from the World Premier International Research Center Initiative, MEXT, Japan. N.S. is supported by the US Department of Energy contract to SLAC no. DE-AC3-76SF00515. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. The data will be made public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web site (http://www.physics.princeton.edu/act/). NR 57 TC 117 Z9 117 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 MAR 1 PY 2011 VL 729 IS 1 AR 62 DI 10.1088/0004-637X/729/1/62 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300062 ER PT J AU Fallscheer, C Beuther, H Sauter, J Wolf, S Zhang, Q AF Fallscheer, C. Beuther, H. Sauter, J. Wolf, S. Zhang, Q. TI A HIGH-MASS DUSTY DISK CANDIDATE: THE CASE OF IRAS 18151-1208 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: early type; stars: formation; stars: individual (IRAS 18151-1208) ID PROTOSTELLAR CANDIDATES; RADIATIVE-TRANSFER; CIRCUMSTELLAR DISK; ACCRETION DISKS; SPACE-TELESCOPE; BUTTERFLY STAR; IRAS-18151-1208; EVOLUTION; CLOUD; EXTINCTION AB Many questions remain regarding the properties of disks around massive prototstars. Here, we present the observations of a high-mass protostellar object including an elongated dust continuum structure perpendicular to the outflow. Submillimeter Array 230 GHz line and continuum observations of the high-mass protostellar object IRAS 18151-1208 along with single-dish IRAM 30 m observations afford us high spatial resolution (0 ''.8) as well as recovery of the extended emission that gets filtered out by the interferometer. The observations of (CO)-C-12 confirm the outflow direction to be in the southeast-northwest direction, and the 1.3 mm continuum exhibits an elongation in the direction perpendicular to the outflow. We model the physical parameters of the elongated structure by simultaneously fitting the observed spectral energy distribution and the brightness profile along the major axis using the 3D Radiative Transfer code MC3D. Assuming a density profile similar to that of a low-mass disk, we can also reproduce the observations of this high-mass protostellar object. This is achieved by using the same density distribution and flaring parameters as were used in the low-mass case, and scaling up the size parameters that successfully modeled the circumstellar disk of several T Tauri stars. We also calculate that a region within the inner 30 AU of such a high-mass disk is stable under the Toomre criterion. While we do not rule out other scenarios, we show here that the observations in the high-mass regime are consistent with a scaled-up version of a low-mass disk. Implications on high-mass star formation are discussed. C1 [Fallscheer, C.; Beuther, H.; Sauter, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Sauter, J.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fallscheer, C (reprint author), Herzberg Inst Astrophys, Natl Res Council, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. EM Cassandra.Fallscheer@nrc-cnrc.gc.ca OI Zhang, Qizhou/0000-0003-2384-6589 FU Deutsche Forschungsgemeinschaft, DFG [BE 2578]; International Max Planck Research School for Astronomy & Cosmic Physics at the University of Heidelberg; DFG-Forschergruppe [759] FX C. F. and H. B. acknowledge support by the Deutsche Forschungsgemeinschaft, DFG project number BE 2578. C. F. also acknowledges support from the International Max Planck Research School for Astronomy & Cosmic Physics at the University of Heidelberg. J.S. acknowledges support by the DFG-Forschergruppe 759 "The Formation of Planets: The Critical First Growth Phase." It is our pleasure to thank the anonymous referee for his/her comments leading to improvement of our manuscript. NR 34 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 66 DI 10.1088/0004-637X/729/1/66 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300066 ER PT J AU Fish, VL Muehlbrad, TC Pratap, P Sjouwerman, LO Strelnitski, V Pihlstrom, YM Bourke, TL AF Fish, Vincent L. Muehlbrad, Talitha C. Pratap, Preethi Sjouwerman, Lorant O. Strelnitski, Vladimir Pihlstroem, Ylva M. Bourke, Tyler L. TI FIRST INTERFEROMETRIC IMAGES OF THE 36 GHz METHANOL MASERS IN THE DR21 COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; magnetic fields; masers; radio lines: ISM; stars: formation ID STAR-FORMING-REGIONS; MOLECULAR CLOUDS; MAGNETIC-FIELDS; OH MASERS; POLARIZATION; EMISSION; OMC-1; SAGITTARIUS; MILLIMETERS; DR-21(OH) AB Class I methanol masers are believed to be produced in the shock-excited environment around star-forming regions. Many authors have argued that the appearance of various subsets of class I masers may be indicative of specific evolutionary stages of star formation or excitation conditions. Until recently, however, no major interferometer was capable of imaging the important 36 GHz transition. We report on Expanded Very Large Array observations of the 36 GHz methanol masers and Submillimeter Array observations of the 229 GHz methanol masers in DR21(OH), DR21N, and DR21W. The distribution of 36 GHz masers in the outflow of DR21(OH) is similar to that of the other class I methanol transitions, with numerous multitransition spatial overlaps. At the site of the main continuum source in DR21(OH), class I masers at 36 and 229 GHz are found in virtual overlap with class II 6.7 GHz masers. To the south of the outflow, the 36 GHz masers are scattered over a large region but usually do not appear coincident with 44 GHz masers. In DR21W, we detect an "S-curve" signature in Stokes V that implies a large value of the magnetic field strength if interpreted as due to Zeeman splitting, suggesting either that class I masers may exist at higher densities than previously believed or that the direct Zeeman interpretation of S-curve Stokes V profiles in class I masers may be incorrect. We find a diverse variety of different maser phenomena in these sources, suggestive of differing physical conditions among them. C1 [Fish, Vincent L.; Muehlbrad, Talitha C.; Pratap, Preethi] MIT, Haystack Observ, Westford, MA 01886 USA. [Sjouwerman, Lorant O.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Strelnitski, Vladimir] Maria Mitchell Observ, Nantucket, MA 02554 USA. [Pihlstroem, Ylva M.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fish, VL (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM vfish@haystack.mit.edu; ppratap2002@gmail.com FU National Science Foundation; Smithsonian Institution; Academia Sinica FX T.C.M. acknowledges support from the National Science Foundation's Research Experiences for Undergraduates program. The National Radio Astronomy Observatory is a facility of the National Science Foundation (NSF) operated under cooperative agreement by Associated Universities, Inc. The Sub-millimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank W.H.T. Vlemmings and A. Sarma for helpful discussions regarding methanol Zeeman splitting coefficients. NR 41 TC 18 Z9 18 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 14 DI 10.1088/0004-637X/729/1/14 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300014 ER PT J AU Mocz, P Lee, JC Iwasawa, K Canizares, CR AF Mocz, Philip Lee, Julia C. Iwasawa, Kazushi Canizares, Claude R. TI A DETECTION OF AN X-RAY WIND AND AN IONIZED DISK IN THE CHANDRA HETGS OBSERVATION OF THE SEYFERT 2 GALAXY IRAS 18325-5926 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (IRAS 18325-5925); galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; IRON K EMISSION; BLACK-HOLE SYSTEMS; WARM ABSORBERS; LINE; REFLECTION; RESOLUTION; SPECTRA; MODELS; MASS AB We analyze the Chandra High Energy Transmission Grating Spectrometer observation of the Seyfert 2 AGN IRAS 18325-5926. We detect a upsilon = -360(-66)(+41) km s(-1) blueshifted ionized absorber in the X-ray spectrum, with photoionization parameter log xi = 2.0(-0.1)(+0.1) and hydrogen column density N-H = 1.55(-0.38)(+0.75) x10(21) cm(-2). The absorber may be a photoionized wind originating in the obscuring torus/global covering around the black hole or outer edge of the accretion disk. The estimated mass outflow rate suggests that the supermassive black hole in IRAS 18325-5926 may significantly affect the large-scale environment of the host galaxy, unless the solid angle subtended by the outflow or the gas filling factor is small. A second warm absorber may be needed to explain the absorption features in the vicinity of the iron K edge, although insufficient counts in the data beyond 7.0 keV make it difficult to assess the nature of the second absorber. Most plausible is a high ionization (log xi similar to 2.3 to 2.6), high column density (N-H similar to 10(23) cm(-2)) absorber with upsilon similar to -3000 to 0 km s(-1), although these parameters are not well constrained. We also examine the broad Fe K emission line in the spectrum, which is likely due to Fe xxv in a highly ionized accretion disk inclined at 25 degrees, consistent with the XMM-Newton EPIC observations of the emission line. Because we are able to view both the obscuring gas and the accretion disk of IRAS 18325-5926, the surrounding gas of IRAS 18325-5926 may be patchy or we are viewing the system at an angle just grazing the obscuring torus. C1 [Mocz, Philip; Lee, Julia C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Mocz, Philip; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Iwasawa, Kazushi] Univ Barcelona, Inst Ciencies Cosmos, ICREA, E-08028 Barcelona, Spain. [Canizares, Claude R.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Mocz, P (reprint author), Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. EM jclee@cfa.harvard.edu; kazushi.iwasawa@icc.ub.edu; crc@mit.edu RI Lee, Julia/G-2381-2015; OI Lee, Julia/0000-0002-7336-3588; Mocz, Philip/0000-0001-6631-2566 FU Harvard University FX We thank Andrew Fabian for useful discussions and the referee for valuable comments. P.M. acknowledges Harvard University for the award of funding through the Harvard College Program for Research in Science and Engineering. J.C.L. thanks the Harvard Faculty of Arts and Sciences and the Harvard College Observatory. NR 32 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 30 DI 10.1088/0004-637X/729/1/30 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300030 ER PT J AU Otsuka, M Meixner, M Riebel, D Hyung, S Tajitsu, A Izumiura, H AF Otsuka, Masaaki Meixner, Margaret Riebel, David Hyung, Siek Tajitsu, Akito Izumiura, Hideyuki TI DUST AND CHEMICAL ABUNDANCES OF THE SAGITTARIUS DWARF GALAXY PLANETARY NEBULA Hen2-436 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: abundances; planetary nebulae: individual (Hen2-436); stars: AGB and post-AGB ID ASYMPTOTIC GIANT BRANCH; OPTICAL RECOMBINATION LINES; INTERMEDIATE-MASS STARS; CARBON STARS; INFRARED SPECTROGRAPH; ELEMENTAL ABUNDANCES; FLUORINE ABUNDANCES; COLLISION STRENGTHS; SPHEROIDAL GALAXY; MAGELLANIC CLOUDS AB We have estimated elemental abundances of the planetary nebula (PN) Hen2-436 in the Sagittarius (Sgr) spheroidal dwarf galaxy using ESO/VLT FORS2, Magellan/MMIRS, and Spitzer/IRS spectra. We have detected candidates of fluorine [F II] lambda 4790, krypton [Kr III] lambda 6826, and phosphorus [P II] lambda 7875 lines and successfully estimated the abundances of these elements ([F/H] = +1.23, [Kr/H] = +0.26, [P/H] = +0.26) for the first time. These elements are known to be synthesized by the neutron capture process in the He-rich intershell during the thermally pulsing asymptotic giant branch (AGB) phase. We present a relation between C, F, P, and Kr abundances among PNe and C-rich stars. The detections of these elements in Hen2-436 support the idea that F, P, Kr together with C are synthesized in the same layer and brought to the surface by the third dredge-up. We have detected N II and O II optical recombination lines (ORLs) and derived the N2+ and O2+ abundances. The discrepancy between the abundance derived from the oxygen ORL and that derived from the collisionally excited line is > 1 dex. To investigate the status of the central star of the PN, nebula condition, and dust properties, we construct a theoretical spectral energy distribution (SED) model to match the observed SED with Cloudy. By comparing the derived luminosity and temperature of the central star with theoretical evolutionary tracks, we conclude that the initial mass of the progenitor is likely to be similar to 1.5-2.0M(circle dot) and the age is similar to 3000 yr after the AGB phase. The observed elemental abundances of Hen2-436 can be explained by a theoretical nucleosynthesis model with a star of initial mass 2.25 M-circle dot, Z = 0.008, and LMC compositions. We have estimated the dust mass to be 2.9x10(-4) M-circle dot (amorphous carbon only) or 4.0x10(-4) M-circle dot (amorphous carbon and polycyclic aromatic hydrocarbon). Based on the assumption that most of the observed dust is formed during the last two thermal pulses and the dust-to-gas mass ratio is 5.58 x 10(-3), the dust mass-loss rate and the total mass-loss rate are < 3.1x10(-8) M-circle dot yr(-1) and < 5.5x10(-6) M-circle dot yr(-1), respectively. Our estimated dust mass-loss rate is comparable to a Sgr dwarf galaxy AGB star with similar metallicity and luminosity. C1 [Otsuka, Masaaki; Meixner, Margaret] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Meixner, Margaret] Harvard Smithsonian Astrophys, Radio & Geoastron Div, Cambridge, MA 02138 USA. [Riebel, David] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hyung, Siek] Chungbuk Natl Univ, Sch Sci Educ Astron, Cheongju 361763, Chungbuk, South Korea. [Tajitsu, Akito] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Izumiura, Hideyuki] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan. RP Otsuka, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM otsuka@stsci.edu FU STScI [GO-1129.01-A]; NASA [NAO-50-12595]; STScI DDRF [D0101.90128]; Harvard-Smithsonian Center for Astrophysics; Ministry of Education, Science and Technology [NRF-2010-0011454]; JPL/Caltech FX The authors express their thanks to Amanda Karakas for a fruitful discussion of AGB nucleosynthesis and a critical reading of the manuscript. They wish to thank the anonymous referee for valuable comments. M.O. and M. M. acknowledge funding support from STScI GO-1129.01-A and NASA NAO-50-12595. M.O. acknowledges funding support form STScI DDRF D0101.90128. M. M. appreciates support from Harvard-Smithsonian Center for Astrophysics during this work. S. H. acknowledges the support by Basic Science Research Program through the National Research Foundation of Korea funded by the Ministry of Education, Science and Technology (NRF-2010-0011454). We thank the Magellan Telescope staffs for supporting MMIRS observations. This work is in part based on ESO archive data obtained by ESO Telescopes at the Paranal Observatory. This work is in part based on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. This work is in part based on HST archive data downloaded from the Canadian Astronomy Data Centre. NR 72 TC 17 Z9 17 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 39 DI 10.1088/0004-637X/729/1/39 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300039 ER PT J AU Wang, JF Fabbiano, G Risaliti, G Elvis, M Karovska, M Zezas, A Mundell, CG Dumas, G Schinnerer, E AF Wang, Junfeng Fabbiano, Giuseppina Risaliti, Guido Elvis, Martin Karovska, Margarita Zezas, Andreas Mundell, Carole G. Dumas, Gaelle Schinnerer, Eva TI A DEEP CHANDRA ACIS STUDY OF NGC 4151. I. THE X-RAY MORPHOLOGY OF THE 3 kpc DIAMETER CIRCUM-NUCLEAR REGION AND RELATION TO THE COLD INTERSTELLAR MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4151); galaxies: ISM; galaxies: Seyfert; ISM: jets and outflows; X-rays: galaxies ID NARROW-LINE REGION; SEYFERT-GALAXY NGC-4151; ACTIVE GALACTIC NUCLEI; SPLIT-PIXEL EVENTS; H-I; MOLECULAR GAS; GEMINI NIFS; SPATIAL-RESOLUTION; IMAGE-RESTORATION; NEUTRAL HYDROGEN AB We report on the imaging analysis of similar to 200 ks sub-arcsecond resolution Chandra Advanced CCD Imaging Spectrometer (ACIS-S) observations of the nearby Seyfert 1 galaxy NGC 4151. Bright, structured soft X-ray emission is observed to extend from 30 pc to 1.3 kpc in the southwest from the nucleus, much farther than seen in earlier X-ray studies. The terminus of the northeastern X-ray emission is spatially coincident with a CO gas lane, where the outflow likely encounters dense gas in the host galactic disk. X-ray emission is also detected outside the boundaries of the ionization cone, which indicates that the gas there is not completely shielded from the nuclear continuum, as would be the case for a molecular torus collimating the bicone. In the central r < 200 pc region, the subpixel processing of the ACIS data recovers the morphological details on scales of <30 pc (<0 ''.5) first discovered in Chandra High Resolution Camera images. The X-ray emission is more absorbed toward the boundaries of the ionization cone, as well as perpendicular to the bicone along the direction of a putative torus in NGC 4151. The innermost region where X-ray emission shows the highest hardness ratio is spatially coincident with the near-infrared-resolved H-2 emission and dusty spirals we find in an Hubble Space Telescope V-H color image. The agreement between the observed H-2 line flux and the value predicted from X-ray-irradiated molecular cloud models supports photo-excitation by X-rays from the active nucleus as the origin of the H-2 line, although contribution from UV fluorescence or collisional excitation cannot be ruled out with current data. The discrepancy between the mass of cold molecular gas inferred from recent CO and near-infrared H-2 observations may be explained by the anomalous CO abundance in this X-ray-dominated region. The total H-2 mass derived from the X-ray observation agrees with the recent measurement by Storchi-Bergmann et al. C1 [Wang, Junfeng; Fabbiano, Giuseppina; Risaliti, Guido; Elvis, Martin; Karovska, Margarita; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, Guido] INAF Arcetri Observ, I-50125 Florence, Italy. [Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Mundell, Carole G.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Dumas, Gaelle; Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM juwang@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X; Schinnerer, Eva/0000-0002-3933-7677 FU NASA [GO8-9101X, NAS8-03060]; CXC; Royal Society and Research Councils UK; DFG [SCH 536/4-1, SCH 536/4-2, SPP 1177] FX We thank the anonymous referee for helpful comments on the H2 excitation mechanisms. This work is supported by NASA grant GO8-9101X. We acknowledge support from the CXC, which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060. C. G. M. acknowledges financial support from the Royal Society and Research Councils UK. G. D. was supported by DFG grants SCH 536/4-1 and SCH 536/4-2 as part of SPP 1177. We thank Eckhard Sturm for providing the FIR line ratios prior to the publication of their work, Dan Harris and Dan Schwartz for advice on subpixel binning. J.W. thanks T. Storchi-Bergmann and R. Riffel for providing the Gemini NIFS maps, M. McCollough, E. Galle, M. Juda, and T. Gaetz (CXC) for technical discussion on Chandra PSF, ACIS readout streaks and HRC data reduction. This research has made use of data obtained from the Chandra Data Archive, and software provided by the CXC in the application packages CIAO and Sherpa. This research used observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). NR 85 TC 12 Z9 12 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 MAR 1 PY 2011 VL 729 IS 1 AR 75 DI 10.1088/0004-637X/729/1/75 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300075 ER PT J AU Williams, BJ Borkowski, KJ Reynolds, SP Ghavamian, P Raymond, JC Long, KS Blair, WP Sankrit, R Smith, RC Points, S Winkler, PF Hendrick, SP AF Williams, Brian J. Borkowski, Kazimierz J. Reynolds, Stephen P. Ghavamian, Parviz Raymond, John C. Long, Knox S. Blair, William P. Sankrit, Ravi Smith, R. Chris Points, Sean Winkler, P. Frank Hendrick, Sean P. TI DUSTY BLAST WAVES OF TWO YOUNG LARGE MAGELLANIC CLOUD SUPERNOVA REMNANTS: CONSTRAINTS ON POST-SHOCK COMPRESSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: supernova remnants; Magellanic Clouds ID GRAIN-SIZE DISTRIBUTIONS; SPITZER OBSERVATIONS; RED CLUMP; EMISSION; DESTRUCTION; PHYSICS; ACCELERATION; SPECTRA; PLASMA; LINES AB We present results from mid-IR spectroscopic observations of two young supernova remnants (SNRs) in the Large Magellanic Cloud made with the Spitzer Space Telescope. We imaged SNRs B0509-67.5 and B0519-69.0 with Spitzer in 2005, and follow-up spectroscopy presented here confirms the presence of warm, shock-heated dust, with no lines present in the spectrum. We use model fits to Spitzer Infrared Spectrograph (IRS) data to estimate the density of the post-shock gas. Both remnants show asymmetries in the infrared images, and we interpret bright spots as places where the forward shock is running into material that is several times denser than elsewhere. The densities we infer for these objects depend on the grain composition assumed, and we explore the effects of differing grain porosity on the model fits. We also analyze archival XMM-Newton RGS spectroscopic data, where both SNRs show strong lines of both Fe and Si, coming from ejecta, as well as strong O lines, which may come from ejecta or shocked ambient medium. We use model fits to IRS spectra to predict X-ray O line strengths for various grain models and values of the shock compression ratio. For 0509-67.5, we find that compact (solid) grain models require nearly all O lines in X-ray spectra to originate in reverse-shocked ejecta. Porous dust grains would lower the strength of ejecta lines relative to those arising in the shocked ambient medium. In 0519-69.0, we find significant evidence for a higher than standard compression ratio of 12, implying efficient cosmic-ray acceleration by the blast wave. A compact grain model is favored over porous grain models. We find that the dust-to-gas mass ratio of the ambient medium is significantly lower than what is expected in the interstellar medium. C1 [Williams, Brian J.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Ghavamian, Parviz; Long, Knox S.] STScI, Baltimore, MD 21218 USA. [Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Smith, R. Chris; Points, Sean] CTIO, La Serena, Chile. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Hendrick, Sean P.] Millersville Univ Pennsylvania, Dept Phys, Millersville, PA 17551 USA. RP Williams, BJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. EM bjwilli2@ncsu.edu FU Spitzer Guest Observer Grant [RSA 1328682] FX We thank John Blondin for providing the VH-1 hydrodynamics code and for useful discussions on interpretation, and the anonymous referee for many useful comments which improved the paper. We acknowledge support from Spitzer Guest Observer Grant RSA 1328682. NR 52 TC 21 Z9 21 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 65 DI 10.1088/0004-637X/729/1/65 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300065 ER PT J AU Fowler, AE Gerner, NV Sewell, MA AF Fowler, Amy E. Gerner, Nadine V. Sewell, Mary A. TI Temperature and salinity tolerances of Stage 1 zoeae predict possible range expansion of an introduced portunid crab, Charybdis japonica, in New Zealand SO BIOLOGICAL INVASIONS LA English DT Article DE Charybdis japonica; Invasive; Stage 1 zoeae; New Zealand; Temperature; Salinity ID DECAPOD CRUSTACEAN LARVAE; CHASMAGNATHUS-GRANULATA; CARCINUS-MAENAS; ESTUARINE CRAB; ONTOGENY; SURVIVAL; LIFE; OSMOREGULATION; MORTALITY; GRAPSIDAE AB The successful invasion of a non-native species depends on several factors, including initial colonization and establishment of a self-sustaining population. Populations of the non-native paddle crab Charybdis japonica were first recognized in the Waitemata Harbour, Auckland, New Zealand in 2000, most likely arriving in ballast waters of an Asian merchant vessel. A survey completed in 2003 found C. japonica throughout the Waitemata Harbour, and further sampling in 2009 has revealed several well established populations in estuaries up to 70 km from the putative invasion point. As the potential for further establishment of C. japonica beyond this area may depend on the temperature and salinity tolerances of their free swimming larvae, we quantified the survival of newly-hatched Stage 1 C. japonica zoeae subjected to temperatures ranging from 11 to 43A degrees C or salinities from 5 to 45aEuro degrees in the laboratory. Upon hatching, replicate C. japonica zoeae were directly transferred from 21A degrees C and 34.6aEuro degrees seawater to either an experimental temperature or salinity level. Behaviour and death rates of the larvae were monitored over a 24 h period in the absence of food. Comparisons of zoeal survival rates to historical sea surface temperatures and salinities show that C. japonica Stage 1 zoeae tolerate a broad range of temperatures and salinities and could survive natural conditions throughout New Zealand. This gives C. japonica the potential to invade many other New Zealand estuaries and harbours. C1 [Fowler, Amy E.] Univ Auckland, Leigh Marine Lab, Warkworth 0941, New Zealand. [Gerner, Nadine V.] Goethe Univ Frankfurt, Inst Okol Evolut & Diversitat, Frankfurt, Germany. [Sewell, Mary A.] Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand. RP Fowler, AE (reprint author), Smithsonian Environm Res Ctr, Marine Invas Lab, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM afow014@aucklanduni.ac.nz RI Sewell, Mary/C-9017-2009; OI Sewell, Mary A./0000-0002-1595-7951 FU Fulbright New Zealand; University of Auckland; Mercator Stiftung, Universitatsstiftung Kiel and Vereinigung von Freunden und Forderern der Goethe-Universitat Frankfurt am Main FX This research was supported by a Fulbright New Zealand Graduate scholarship and University of Auckland Fulbright scholarship to A.E.F. N.V.G was supported by the IFM-Geomar in Kiel, Germany with the financial support from the Mercator Stiftung, Universitatsstiftung Kiel and Vereinigung von Freunden und Forderern der Goethe-Universitat Frankfurt am Main. M. Birch assisted with project development, and A. Fukunaga provided statistical and editorial advice. Thank you to the various governmental councils and research organizations for providing us with the historical temperature and salinity data. We gratefully acknowledge D. Simberloff and an anonymous reviewer for comments which significantly improved the manuscript. NR 41 TC 13 Z9 13 U1 4 U2 29 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD MAR PY 2011 VL 13 IS 3 BP 691 EP 699 DI 10.1007/s10530-010-9860-2 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 719JT UT WOS:000287201700013 ER PT J AU Carvalho, JC Cardoso, P Crespo, LC Henriques, S Carvalho, R Gomes, P AF Carvalho, Jose C. Cardoso, Pedro Crespo, Luis C. Henriques, Sergio Carvalho, Rui Gomes, Pedro TI Determinants of beta diversity of spiders in coastal dunes along a gradient of mediterraneity SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Araneae; beta diversity; coastal dunes; latitudinal gradients; Mediterranean; Portugal ID SPECIES RICHNESS; LATITUDINAL GRADIENT; NEIGHBOR MATRICES; IBERIAN PENINSULA; TEMPERATE FOREST; ECOLOGICAL DATA; NORTH-AMERICA; ARANEAE; SCALE; PATTERNS AB Aim The Mediterranean Basin is recognized for its high levels of species richness, rarity and endemicity. Our main aim was to evaluate the relative effects of environmental and spatial variables and their scale-specific importance on beta diversity patterns along a gradient of mediterraneity, using spiders as a model group. Location This study was carried out in 18 coastal dune sites along the Portuguese Atlantic coast. This area encompasses 445 km and comprises two distinct biogeographic regions, Eurosiberian (northern coast) and Mediterranean (centre and south). Methods A forward selection procedure was carried out to select environmental and spatial variables responsible for determining beta diversity patterns. Variation partitioning and principal coordinates of neighbour matrices (PCNM) were used to estimate the contribution of pure environmental and pure spatial effects and their shared influence on beta diversity patterns and to estimate the relative importance of environmental structured variation and pure spatial variation at multiple spatial scales. Results Climate, ground vegetation dune cover and area were selected by a forward selection procedure. The same procedure identified three PCNM variables, all corresponding to large and medium spatial scales. Variation partitioning revealed that 46.1% of the variation of beta diversity patterns was explained by a combination of environmental and PCNM variables. Most of this variation (42.5%) corresponded to spatial variation (environmental spatially structured and pure spatial). Climate and vegetation structure influences were predominant at the PCNM1 and PCNM3 scales, while area was more important at the intermediate PCNM2 scale. Main conclusions Our study revealed that beta diversity of spiders was primarily controlled by a broad-scale gradient of mediterraneity. The relative importance of environmental variables on the spider assemblage composition varied with spatial scale. This study highlights the need of considering the scale-specific influence of niche and neutral processes on beta diversity patterns. C1 [Carvalho, Jose C.; Gomes, Pedro] Univ Minho, Dept Biol, CBMA Mol & Environm Ctr, P-4710057 Braga, Portugal. [Cardoso, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Cardoso, Pedro] Univ Azores, Azorean Biodivers Grp CITA A, P-9700851 Angra Do Heroismo, Portugal. [Crespo, Luis C.] Univ Coimbra, Dept Life Sci, IMAR Marine & Environm Res Ctr, P-3004517 Coimbra, Portugal. [Henriques, Sergio; Carvalho, Rui] Univ Evora, Dept Biol, P-7002554 Evora, Portugal. RP Carvalho, JC (reprint author), Univ Minho, Dept Biol, CBMA Mol & Environm Ctr, Gualtar Campus, P-4710057 Braga, Portugal. EM josecarvalho@bio.uminho.pt RI Cardoso, Pedro/A-8820-2008; Gomes, Pedro/I-8348-2015; CBMA, CBMA/J-1937-2016 OI Cardoso, Pedro/0000-0001-8119-9960; Gomes, Pedro/0000-0002-5595-6988; CBMA, CBMA/0000-0002-2841-2678 FU Luso-American Foundation; Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007] FX We thank Oliver Schweiger, Chris Thomas and two anonymous reviewers for providing helpful suggestions on an earlier version of the manuscript. We acknowledge Jose Antonio Barrientos, Carmen Urones and Stano Pekar for their help with the taxonomic identification of some spider specimens. J.C.C expresses his gratitude to the Luso-American Foundation for its support (FLAD C&T Links 2010 grant). P.C. is supported by the Portuguese Foundation for Science and Technology (SFRH/BPD/40688/2007). NR 68 TC 19 Z9 19 U1 3 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD MAR PY 2011 VL 17 IS 2 BP 225 EP 234 DI 10.1111/j.1472-4642.2010.00731.x PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 722PZ UT WOS:000287448100004 ER PT J AU Jung, K Kalko, EKV AF Jung, Kirsten Kalko, Elisabeth K. V. TI Adaptability and vulnerability of high flying Neotropical aerial insectivorous bats to urbanization SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Acoustic monitoring; adaptability; anthropogenic influence; chiroptera; conservation; Panama ID FREE-TAILED BATS; ECHOLOCATION CALLS; COMMUNITY STRUCTURE; PHYLLOSTOMID BATS; URBAN LANDSCAPE; TROPICAL FOREST; MATING SYSTEM; DIVERSITY; HABITAT; BIODIVERSITY AB Aim Urbanization is a dominant demographic trend throughout the world that involves massive habitat alterations. Understanding how urbanization affects biota is a crucial prerequisite for development and application of effective species conservation programmes. Our study focuses on Neotropical high flying aerial insectivorous bats, an ecologically important, but so far seriously understudied group of vertebrates. Location Panama. Methods Using acoustic monitoring, we assessed and compared species occurrence, composition and activity of aerial insectivorous bats at three site categories located on the isthmus in Panama: forest, urban areas and a forest-town interface. Results In 2 years of field work, we recorded 44,744 bat passes over the microphone and identified a total of 25 aerial insectivorous bat species. Species richness was highest in the forest, decreased towards the forest-town interface and was lowest at the urban sites, while dominance (Berger-Parker-Index) increased from the forest to the urban sites. Overall, general bat activity (passes min-1) was highest at the forest-town interface and lowest at the urban sites. Multivariate analysis suggests compositional differences in species occurrence and activity among site categories with mainly molossid species occurring in urban areas. Main conclusions Our results clearly demonstrate species-specific differences between high flying aerial insectivorous bats concerning their adaptability and vulnerability to urban areas. Our results suggest that a suite of morphological traits including species mobility determine persistence of aerial insectivorous species in cities. Our results underline the necessity for detailed assessments of species-specific habitat requirements and dynamics of species occurrence and activity over time to develop meaningful conservation tools targeted at aerial insectivorous bats. C1 [Jung, Kirsten; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Jung, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM kirsten.jung@uni-ulm.de FU German Academic Exchange Program (DAAD) FX We cordially thank Y. Basset, N. Gomez, R. Arias (Canopy Tower Hotel) and the Gamboa Resort Hotel; all who provided excellent acoustic monitoring sites. We thank the Environmental Sciences Program of the Smithsonian Tropical Research Institute (STRI); C. Meyer for all the discussions and statistical advice; we kindly thank K. Rex and T. Czaczkes for revising our English. We acknowledge the valuable input of four anonymous reviewers. We thank STRI in Panama, especially O. Acevedo, for excellent logistic support and the German Academic Exchange Program (DAAD) for financial support to the first author. NR 78 TC 38 Z9 39 U1 10 U2 48 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 EI 1472-4642 J9 DIVERS DISTRIB JI Divers. Distrib. PD MAR PY 2011 VL 17 IS 2 BP 262 EP 274 DI 10.1111/j.1472-4642.2010.00738.x PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 722PZ UT WOS:000287448100008 ER PT J AU Muirhead, JR Lewis, MA MacIsaac, HJ AF Muirhead, Jim R. Lewis, Mark A. MacIsaac, Hugh J. TI Prediction and error in multi-stage models for spread of aquatic non-indigenous species SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Biological invasions; Cercopagis pengoi; gravity model; invasion sequence; spread; stochasticity ID CLADOCERAN CERCOPAGIS-PENGOI; HUMAN-MEDIATED DISPERSAL; BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; LAKE-ONTARIO; BYTHOTREPHES-LONGIMANUS; PLANT INVASIONS; INLAND LAKES; BALTIC SEA; RECONCILING PATTERN AB Aim Predictions of spread of non-indigenous species allow for greater efficiency in managing invasions by targeting areas for preventative measures. The invasion sequence is a useful concept in predictions of spread, as it allows us to test hypotheses about the transport and establishment of propagules in novel habitats. Our aims are twofold: (1) to develop and validate multi-stage invasion models for the introduced fishhook waterflea, Cercopagis pengoi, and (2) to assess how variability in the transport patterns of the propagules influences the accuracy and spatial extent for predictions of spread. Location New York State, USA. Methods We developed a two-stage model for the spread of C. pengoi. First, we developed a stochastic gravity model for dispersal based on surveys of recreational boat traffic in New York State as a proxy for propagule pressure. We then modelled the probability of establishment based on predicted levels of propagule pressure and measures of lakes' physicochemistry. In addition, we used Monte Carlo simulations based on the gravity model to propagate variability in boater traffic through the establishment model to assess how uncertainty in dispersal influenced predictions of spread. Results The amount recreationalists were willing to spend, lake area and population size of the city nearest to the destination lake were significant factors affecting boater traffic. In turn, boater traffic, lake area, specific conductance and turbidity were significant predictors of establishment. The inclusion of stochastic dispersal reduced the rate of false positives (i.e. incorrect prediction of an invasion) in detecting invasions at the upper 95% prediction interval for the probability of establishment. Main conclusions Combinations of measures of propagule pressure, habitat suitability and stochastic dispersal allow for the most accurate predictions of spread. Further, multi-stage spread models may overestimate the extent of spread if stochasticity in early stages of the models is not considered. C1 [Muirhead, Jim R.; Lewis, Mark A.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Muirhead, Jim R.; Lewis, Mark A.] Univ Alberta, Ctr Math Biol, Edmonton, AB T6G 2G1, Canada. [Lewis, Mark A.] Univ Alberta, Dept Math & Stat Sci, Edmonton, AB T6G 2G1, Canada. [Muirhead, Jim R.; MacIsaac, Hugh J.] Univ Windsor, Great Lakes Inst Environm Res, Windsor, ON N9B 3P4, Canada. RP Muirhead, JR (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM muirheadj@si.edu RI Lewis, Mark/C-5015-2008 FU Canadian Aquatic Invasive Species Network (CAISN); NSERC; Ontario Graduate Scholarship; Department of Fisheries and Oceans Invasive Species Research Chair; Canada Research Chair FX We thank Alexei Potapov, Subhash Lele and Norman Yan for helpful discussions during this project. We are grateful for financial support from the Canadian Aquatic Invasive Species Network (CAISN), NSERC Discovery program (H.J.M. and M.A.L.), an Ontario Graduate Scholarship and NSERC postdoctoral fellowship to J.R.M., a Department of Fisheries and Oceans Invasive Species Research Chair to H.J.M., and Canada Research Chair to M.A.L. NR 68 TC 2 Z9 2 U1 1 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 EI 1472-4642 J9 DIVERS DISTRIB JI Divers. Distrib. PD MAR PY 2011 VL 17 IS 2 BP 323 EP 337 DI 10.1111/j.1472-4642.2011.00745.x PG 15 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 722PZ UT WOS:000287448100013 ER PT J AU Ruiz, GM Fofonoff, PW Steves, B Foss, SF Shiba, SN AF Ruiz, Gregory M. Fofonoff, Paul W. Steves, Brian Foss, Stephen F. Shiba, Sharon N. TI Marine invasion history and vector analysis of California: a hotspot for western North America SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Biological invasions; California; marine invasions; non-native species; ships; vector strength ID BIOLOGICAL INVASIONS; AQUATIC ORGANISMS; CARCINUS-MAENAS; COMMUNITIES; PACIFIC; ESTUARY; SHIPS; RISK; INTRODUCTIONS; AQUACULTURE AB Aim We examine the regional dominance of California as a beachhead for marine biological invasions in western North America and assess the relative contribution of different transfer mechanisms to invasions over time. Location Western North America (California to Alaska, excluding Mexico). Methods We undertook extensive analysis of literature and collections records to characterize the invasion history of non-native species (invertebrates, microalgae and microorganisms) with established populations in coastal marine (tidal) waters of western North America through 2006. Using these data, we estimated (1) the proportion of first regional records of non-native species that occurred in California and (2) the relative contribution of transfer mechanisms to California invasions (or vector strength) over time. Results Excluding vascular plants and vertebrates, we identified 290 non-native marine species with established populations in western North America, and 79% had first regional records from California. Many (40-64%) of the non-native species in adjacent states and provinces were first reported in California, suggesting northward spread. California also drives the increasing regional rate of detected invasions. Of 257 non-native species established in California, 59% had first regional records in San Francisco Bay; 57% are known from multiple estuaries, suggesting secondary spread; and a majority were attributed to vessels (ballast water or hull fouling) or oysters, in some combination, but their relative contributions are not clear. For California, more than one vector was possible for 56% of species, and the potential contribution of ballast water, hull fouling and live trade increased over time, unlike other vectors. Main conclusions California, especially San Francisco Bay, plays a pivotal role for marine invasion dynamics for western North America, providing an entry point from which many species spread. This pattern is associated historically with high propagule supply and salinity. Any effective strategies to minimize new invasions throughout this region must (1) focus attention on California and (2) address current uncertainty and future shifts in vector strength. C1 [Ruiz, Gregory M.; Fofonoff, Paul W.; Steves, Brian] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ruiz, Gregory M.; Steves, Brian] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA. [Foss, Stephen F.; Shiba, Sharon N.] Calif Dept Fish & Game, Marine Invas Species Program, Off Spill Prevent & Response, Sacramento, CA 95811 USA. RP Ruiz, GM (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM ruizg@si.edu OI Ruiz, Gregory/0000-0003-2499-441X FU California Department of Fish and Game; Department of Defense; National Sea Grant Program; Smithsonian Institution FX We thank D. Cadien, J. Carlton, J. Chapman, L. Harris, G. Lambert, K. Miller, P. Slattery, and T. Therriault for insights into the occurrence records, identifications and invasion status of species in western North America. S. Havard assisted in data proofing and analyses. Our research on invasions in California and western North America was supported by funding from the California Department of Fish and Game, Department of Defense Legacy Program, National Sea Grant Program, and Smithsonian Institution. NR 62 TC 33 Z9 34 U1 2 U2 42 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD MAR PY 2011 VL 17 IS 2 BP 362 EP 373 DI 10.1111/j.1472-4642.2011.00742.x PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 722PZ UT WOS:000287448100016 ER PT J AU Maloney, KO Weller, DE AF Maloney, Kelly O. Weller, Donald E. TI Anthropogenic disturbance and streams: land use and land-use change affect stream ecosystems via multiple pathways SO FRESHWATER BIOLOGY LA English DT Article DE benthic macroinvertebrates; land use legacy; past land use; stream water chemistry; structural equation modelling (SEM) ID LARGE WOODY DEBRIS; COMMUNITY STRUCTURE; HEADWATER STREAMS; ECOLOGICAL THEORY; CURRENT KNOWLEDGE; RIPARIAN BUFFERS; SOIL PROPERTIES; UNITED-STATES; RIVER; CATCHMENT AB 1. Ecosystems are strongly influenced by land use practices. However, identifying the mechanisms behind these influences is complicated by the many potential pathways (often indirect) between land use and ecosystems and by the long-lasting effects of past land use. To support ecosystem restoration and conservation efforts, we need to better understand these indirect and lasting effects. 2. We constructed structural equation models (SEM) to evaluate the direct and indirect effects of contemporary (2002) land use (agriculture and development) and change in land use from 1952 to 2002 on present-day streams (n = 190) in Maryland, U.S.A. Additional variables examined included site location, system size, altitude, per cent sand in soils, riparian condition, habitat quality, stream water NO(3)-N and benthic macroinvertebrate and fish measures of stream condition. Our first SEM (2002 Land Use) included the proportions of contemporary agriculture and development in catchments in the model. The second SEM (Land Use Change) included five measures of land use change (proportion agricultural in both times, developed in both times, agricultural in 1952 and developed in 2002, forested in 1952 and developed in 2002 and agricultural in 1952 and forested in 2002). 3. The data set fit both SEMs well. The 2002 Land Use model explained 71% of variation in NO(3)-N and 55%, 42% and 38% of variation in riffle quality, macroinvertebrate condition and fish condition, respectively. The Land Use Change model explained similar amounts of variation in NO(3)-N (R2 = 0.72), riffle quality (R2 = 0.57) and macroinvertebrate condition (R2 = 0.44) but slightly more variation in fish condition (R2 = 0.43). 4. Both models identified pathways through which landscape variables affect stream responses, including negative direct effects of latitude on macroinvertebrate and fish conditions and positive direct and indirect effects of altitude on NO(3)-N, riffle quality and macroinvertebrate and fish conditions. The 2002 Land Use model showed contemporary development and agriculture had positive total effects on NO(3)-N (both through direct pathways); contemporary development had negative effects on macroinvertebrate condition. The Land Use Change model showed that contemporary developed land that was forested in 1952 had no effects on NO(3)-N; current developed land that was developed or agricultural in 1952 showed positive effects on NO(3)-N. Forests that were agricultural in 1952 had negative effects on NO(3)-N, suggesting reduced NO(3)-N export with reforestation. The Land Use Change model also showed negative total effects of all types of contemporary developed land (developed, agricultural or forested in 1952) on benthic condition. Developed land that was forested in 1952 had negative effects on fish condition. Forest sites that were agricultural in 1952 had negative effects on fish and macroinvertebrate conditions, suggesting a long-term imprint of abandoned agriculture in stream communities. 5. Our analyses (i) identified multiple indirect effects of contemporary land use on streams, (ii) showed that current land uses with different land use histories can exhibit different effects on streams and (iii) demonstrated an imprint of land use lasting > 50 years. Knowledge of these indirect and long-term effects of land use will help to conserve and restore streams. C1 [Maloney, Kelly O.; Weller, Donald E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Maloney, KO (reprint author), US Geol Survey, Leetown Sci Ctr, No Appalachian Res Lab, 176 Straight Run Rd, Wellsboro, PA 16901 USA. EM kmaloney@usgs.gov OI Weller, Donald/0000-0002-7629-5437 FU Smithsonian Post-Doctoral Research Fellowship FX We thank the Maryland Department of Natural Resources for providing the MBSS data, the Maryland Department of Transportation for providing the 2002 land use data, Matt Baker for catchment boundaries and Eric Lind, Darryl Hondorp, Lori Davias, John Parker, Ariana Sutton-Grier and two anonymous reviewers for constructive comments on the manuscript. The project was funded by a Smithsonian Post-Doctoral Research Fellowship awarded to KOM. NR 77 TC 25 Z9 26 U1 8 U2 94 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0046-5070 J9 FRESHWATER BIOL JI Freshw. Biol. PD MAR PY 2011 VL 56 IS 3 BP 611 EP 626 DI 10.1111/j.1365-2427.2010.02522.x PG 16 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 718AV UT WOS:000287092900016 ER PT J AU Mishchenko, MI Menguc, MP Rothman, LS AF Mishchenko, Michael I. Menguec, M. Pinar Rothman, Laurence S. TI Van de Hulst Light-Scattering Award SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Menguec, M. Pinar] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM crmim2@gmail.com RI Menguc, Pinar/O-3114-2013; Mishchenko, Michael/D-4426-2012; OI Rothman, Laurence/0000-0002-3837-4847 NR 0 TC 0 Z9 0 U1 0 U2 4 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 MAR PY 2011 VL 112 IS 4 SI SI BP 559 EP 559 DI 10.1016/j.jqsrt.2010.11.018 PG 1 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 725VO UT WOS:000287675000001 ER PT J AU Dimichele, WA Falcon-Lang, HJ AF Dimichele, William A. Falcon-Lang, Howard J. TI Pennsylvanian 'fossil forests' in growth position (T-0 assemblages): origin, taphonomic bias and palaeoecological insights SO JOURNAL OF THE GEOLOGICAL SOCIETY LA English DT Article ID SYDNEY-MINES-FORMATION; VOLCANIC ASH-FALL; NOVA-SCOTIA; JOGGINS FORMATION; NEW-BRUNSWICK; IN-SITU; PLANT TAPHONOMY; ALLUVIAL-PLAIN; SEA-LEVEL; ATLANTIC CANADA AB Fossil forests, buried in growth position in a geological instant (T-0 assemblages) are far more abundant in Pennsylvanian successions than in any other part of the geological record. In this review paper, we evaluate the fundamental controls on the origin of these phenomena, investigate the taphonomic biases that influence their composition, and summarize their palaeoecological significance. Following earlier workers, we highlight that high rates of burial and accommodation are essential for the formation and preservation of T-0 assemblages. Contexts especially favourable for their origin include ashfalls proximal to volcanic centres, coastal plains drowned by relative sea-level rise, and fluvial environments such as channel bars, crevasse splays, and distributary lobes. Long-term preservation requires high rates of subsidence. Consequently, the vast majority of Palaeozoic T-0 assemblages are confined to wetland settings at, or close to, sea level, whereas drylands are poorly represented and uplands rarely sampled, if ever. However, this is not the only major bias in the fossil record; taphonomic processes selectively preserve plants dependent on their anatomy and stature, and on groundwater chemistry. Thus, although T-0 assemblages offer unrivalled insights into the nature of ancient forests (whole-plant reconstructions, tree density, canopy height, productivity, plant hydraulics, cohort dynamics, spatial heterogeneity, ecological gradients, tree-sediment interactions, and animal-plant interactions, to name but a few), it is naive to believe they provide 'photographic snapshots' of palaeoecosystems. None the less, careful taphonomic analysis of T-0 assemblages offers the potential for a nuanced understanding of these evocative phenomena, and much remains to be learned from these important palaeoecological resources. C1 [Dimichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. RP Dimichele, WA (reprint author), NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM dimichel@si.edu RI Falcon-Lang, Howard/D-8465-2011; DiMichele, William/K-4301-2012 FU National Museum of Natural History; Smithsonian Institution; NERC FX We thank C. Cleal and J. Hilton, the organizers of the Lyell Symposium (2009), for their generous invitation to contribute to this special volume. W.D.'s original research that contributed to this paper was supported by endowment and small grant funds of National Museum of Natural History and the Smithsonian Institution. H. F. L. acknowledges receipt of an NERC Advanced Fellowship. We thank S. Oplustil, R. Gastaldo, M. Gibling and S. Greb for permission to use their figures and photographs in this paper (Figs 3, 4, 8 and 14). The reviews of S. Oplustil, R. Gastaldo and C. Cleal greatly improved an earlier version of this paper. NR 194 TC 42 Z9 43 U1 4 U2 26 PU GEOLOGICAL SOC PUBL HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CENTRE, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0016-7649 EI 2041-479X J9 J GEOL SOC LONDON JI J. Geol. Soc. PD MAR PY 2011 VL 168 IS 2 BP 585 EP 605 DI 10.1144/0016-76492010-103 PG 21 WC Geosciences, Multidisciplinary SC Geology GA 726CE UT WOS:000287695200023 ER PT J AU Woods, PM Oliveira, JM Kemper, F van Loon, JT Sargent, BA Matsuura, M Szczerba, R Volk, K Zijlstra, AA Sloan, GC Lagadec, E McDonald, I Jones, O Gorjian, V Kraemer, KE Gielen, C Meixner, M Blum, RD Sewilo, M Riebel, D Shiao, B Chen, CHR Boyer, ML Indebetouw, R Antoniou, V Bernard, JP Cohen, M Dijkstra, C Galametz, M Galliano, F Gordon, KD Harris, J Hony, S Hora, JL Kawamura, A Lawton, B Leisenring, JM Madden, S Marengo, M McGuire, C Mulia, AJ O'Halloran, B Olsen, K Paladini, R Paradis, D Reach, WT Rubin, D Sandstrom, K Soszynski, I Speck, AK Srinivasan, S Tielens, AGGM van Aarle, E Van Dyk, SD Van Winckel, H Vijh, UP Whitney, B Wilkins, AN AF Woods, Paul M. Oliveira, J. M. Kemper, F. van Loon, J. Th. Sargent, B. A. Matsuura, M. Szczerba, R. Volk, K. Zijlstra, A. A. Sloan, G. C. Lagadec, E. McDonald, I. Jones, O. Gorjian, V. Kraemer, K. E. Gielen, C. Meixner, M. Blum, R. D. Sewilo, M. Riebel, D. Shiao, B. Chen, C. -H. R. Boyer, M. L. Indebetouw, R. Antoniou, V. Bernard, J. -P. Cohen, M. Dijkstra, C. Galametz, M. Galliano, F. Gordon, Karl D. Harris, J. Hony, S. Hora, J. L. Kawamura, A. Lawton, B. Leisenring, J. M. Madden, S. Marengo, M. McGuire, C. Mulia, A. J. O'Halloran, B. Olsen, K. Paladini, R. Paradis, D. Reach, W. T. Rubin, D. Sandstrom, K. Soszynski, I. Speck, A. K. Srinivasan, S. Tielens, A. G. G. M. van Aarle, E. Van Dyk, S. D. Van Winckel, H. Vijh, Uma P. Whitney, B. Wilkins, A. N. TI The SAGE-Spec Spitzer Legacy programme: the life-cycle of dust and gas in the Large Magellanic Cloud - Point source classification I SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; surveys; galaxies: individual: LMC; Magellanic Clouds; infrared: galaxies; infrared: stars ID ASYMPTOTIC GIANT BRANCH; YOUNG STELLAR OBJECTS; LONG-PERIOD VARIABLES; POST-AGB STARS; GRAVITATIONAL LENSING EXPERIMENT.; CORONAE-BOREALIS STARS; OGLE-III CATALOG; MU-M SOURCES; EXTREME CARBON STARS; WOLF-RAYET STARS AB We present the classification of 197 point sources observed with the Infrared Spectrograph in the SAGE-Spec Legacy programme on the Spitzer Space Telescope. We introduce a decision-tree method of object classification based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information, which is used to classify the SAGE-Spec sample of point sources. The decision tree has a broad application to mid-infrared spectroscopic surveys, where supporting photometry and variability information are available. We use these classifications to make deductions about the stellar populations of the Large Magellanic Cloud and the success of photometric classification methods. We find 90 asymptotic giant branch (AGB) stars, 29 young stellar objects, 23 post-AGB objects, 19 red supergiants, eight stellar photospheres, seven background galaxies, seven planetary nebulae, two H II regions and 12 other objects, seven of which remain unclassified. C1 [Woods, Paul M.; Kemper, F.; Zijlstra, A. A.; Lagadec, E.; McDonald, I.; Jones, O.; McGuire, C.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Oliveira, J. M.; van Loon, J. Th.] Univ Keele, Sch Phys & Geog Sci, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Sargent, B. A.; Volk, K.; Meixner, M.; Sewilo, M.; Shiao, B.; Boyer, M. L.; Gordon, Karl D.; Lawton, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Matsuura, M.] Univ London Univ Coll, Dept Phys & Astron, Inst Origins, London WC1E 6BT, England. [Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, Inst Origins, Dorking RH5 6NT, Surrey, England. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Sloan, G. C.; Wilkins, A. N.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Lagadec, E.] European So Observ, D-85748 Garching, Germany. [Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kraemer, K. E.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. [Gielen, C.; van Aarle, E.; Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Blum, R. D.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Riebel, D.; Srinivasan, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Chen, C. -H. R.; Indebetouw, R.; Leisenring, J. M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Antoniou, V.; Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Bernard, J. -P.; Olsen, K.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Cohen, M.; Sandstrom, K.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Galametz, M.; Galliano, F.; Harris, J.; Hony, S.; Madden, S.; Rubin, D.] Univ Paris Diderot DAPNIA, CNRS, CEA DSM, Lab AIM, F-91191 Gif Sur Yvette, France. [Galametz, M.; Galliano, F.; Harris, J.; Hony, S.; Madden, S.; Rubin, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hora, J. L.; Marengo, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kawamura, A.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 46401, Japan. [Mulia, A. J.; Speck, A. K.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [O'Halloran, B.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Paladini, R.; Paradis, D.; Reach, W. T.; Van Dyk, S. D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Sandstrom, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Srinivasan, S.] Inst Astrophys, F-75014 Paris, France. [Tielens, A. G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Vijh, Uma P.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. [Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA. RP Woods, PM (reprint author), Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM woods@manchester.ac.uk RI Woods, Paul/E-6926-2011; Van Winckel, Hans/I-7863-2013; Kemper, Francisca/D-8688-2011; Antoniou, Vallia/E-3837-2013; OI Reach, William/0000-0001-8362-4094; Woods, Paul/0000-0003-4340-3590; Van Winckel, Hans/0000-0001-5158-9327; Kemper, Francisca/0000-0003-2743-8240; Antoniou, Vallia/0000-0001-7539-1593; Hora, Joseph/0000-0002-5599-4650; Jones, Olivia/0000-0003-4870-5547; Kraemer, Kathleen/0000-0002-2626-7155; Van Dyk, Schuyler/0000-0001-9038-9950 FU US Department of Energy through the University of California, Lawrence Livermore National Laboratory [W-7405-Eng-48]; National Science Foundation through the Center for Particle Astrophysics of the University of California [AST-8809616]; Mount Stromlo and Siding Spring Observatory, Australian National University; National Aeronautics and Space Administration; National Science Foundation; [N203 511838 (MNiSW)] FX RSz acknowledges support from grant N203 511838 (MNiSW). This paper utilizes public domain data obtained by the MACHO project, jointly funded by the US Department of Energy through the University of California, Lawrence Livermore National Laboratory under contract no. W-7405-Eng-48, by the National Science Foundation through the Center for Particle Astrophysics of the University of California under cooperative agreement AST-8809616, and by the Mount Stromlo and Siding Spring Observatory, part of the Australian National University. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Optical Gravitational Lensing Experiment OGLE-III online catalogue of variable stars. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 213 TC 55 Z9 55 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 MAR PY 2011 VL 411 IS 3 BP 1597 EP 1627 DI 10.1111/j.1365-2966.2010.17794.x PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 723DL UT WOS:000287486400016 ER PT J AU O'Sullivan, E Giacintucci, S David, LP Vrtilek, JM Raychaudhury, S AF O'Sullivan, Ewan Giacintucci, Simona David, Laurence P. Vrtilek, Jan M. Raychaudhury, Somak TI A deep Chandra observation of the poor cluster AWM 4-II. The role of the radio jets in enriching the intracluster medium SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: individual: AWM 4; galaxies: clusters: intracluster medium; galaxies: individual: NGC 6051; X-rays: galaxies: clusters ID RELAXED GALAXY CLUSTERS; COOLING FLOW CLUSTERS; ABUNDANCE PROFILES; XMM-NEWTON; STAR-FORMATION; METAL TRANSPORT; MOLECULAR GAS; COLD FRONTS; HOT GAS; CORE AB We use a Chandra observation of the poor cluster AWM 4 to map the temperature and abundance of the intracluster medium, so as to examine the influence of the central radio galaxy on its environment. While the cluster core is generally enriched to near-solar abundances, we find evidence of supersolar abundances correlated with the radio jets, extending similar to 35 kpc from the core of the central dominant galaxy NGC 6051 along its minor-axis. We conclude that the enriched gas has been transported out of the central galaxy through the action of the radio source. We estimate the excess mass of iron in the entrained gas to be similar to 1.4 x 10(6)M(circle dot) and find that this can be produced in the core of NGC 6051 within the time-scale of the active galactic nucleus (AGN) outburst. The energy required to transport this gas to its current location is similar to 4.5 x 10(57) erg, a significant fraction of the estimated total mechanical energy output of the AGN, though this estimate is dependent on the degree of enrichment of the uplifted gas. The larger near-solar abundance region is also compatible with enrichment by metals mixed outwards from NGC 6051 over a much longer time-scale. C1 [O'Sullivan, Ewan; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Edgbaston B15 2TT, England. [O'Sullivan, Ewan; Giacintucci, Simona; David, Laurence P.; Vrtilek, Jan M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giacintucci, Simona] INAF Inst Radioastron, I-40129 Bologna, Italy. RP O'Sullivan, E (reprint author), Univ Birmingham, Sch Phys & Astron, Edgbaston B15 2TT, England. EM ejos@star.sr.bham.ac.uk OI O'Sullivan, Ewan/0000-0002-5671-6900 FU National Aeronautics and Space Administration [GO8-9127X-R]; NASA [NAS8-03060]; European Community FX The authors thank the anonymous referee for a number of comments, which have materially improved this paper. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO8-9127X-R issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. EO'S acknowledges the support of the European Community under the Marie Curie Research Training Network. We thank the staff of the GMRT for their help during the observations. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr). NR 51 TC 17 Z9 17 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2011 VL 411 IS 3 BP 1833 EP 1842 DI 10.1111/j.1365-2966.2010.17812.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 723DL UT WOS:000287486400035 ER PT J AU Dow, TL Roudebush, W Parker, FN Brown, JL AF Dow, T. L. Roudebush, W. Parker, F. N. Brown, J. L. TI Influence of age and gender on secretion of anti-Mullerian hormone in Asian (Elephas maximus) and African (Loxodonta africana) elephants SO THERIOGENOLOGY LA English DT Article DE Anti-Mullerian hormone; Ovary; Granulosa cell; Spermatogenesis; Elephant ID INHIBITING SUBSTANCE; COMPARATIVE ENDOCRINOLOGY; ANTIMULLERIAN HORMONE; FOLLICLE RECRUITMENT; OVARIAN RESERVE; ESTROUS-CYCLE; SERUM; FEMALE; SEMEN; ULTRASONOGRAPHY AB Anti-Mullerian hormone (AMH) secretion was studied in Asian and African elephants varying in age and reproductive status. Overall mean concentrations did not differ (P > 0.05) between species, but were markedly higher in male than female Asian elephants (31.01 +/- 4.22 ng/mL and 0.19 +/- 0.02 ng/mL, mean +/- SEM) and African elephants (40.27 +/- 3.18 ng/mL, 0.17 +/- 0.04 ng/mL), respectively. Anti-Mullerian hormone secretion was not significantly affected by ovarian cyclicity status (cycling vs noncycling), but was higher (P < 0.05) in prepubertal (0.40 +/- 0.10 ng/mL) than reproductive age (8-35 y; 0.18 +/- 0.04 ng/mL) and aged (>= 36 y; 0.16 +/- 0.03 ng/mL) females. In males, AMH secretion was not significantly affected by musth status, but was age-related, with higher concentrations (P > 0.05) in prepubertal (49.08 +/- 6.11 ng/mL) as compared to aged (>= 36 y; 22.27 +/- 5.82 ng/mL) bulls; concentrations in mature bulls (8-35 y; 37.01 +/- 3.17 ng/mL) were similar to prepubertal and older bulls. We concluded that circulating AMH concentrations in elephants were similar between species and not affected by reproductive status; however, concentrations were significantly higher in males than females, and in younger animals. The diagnostic value of AMH to assess fertility status of individual elephants remains to be determined. (C) 2011 Elsevier Inc. All rights reserved. C1 [Dow, T. L.; Parker, F. N.; Brown, J. L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22623 USA. [Roudebush, W.] Charleston So Univ, Charleston, SC 29406 USA. [Dow, T. L.] W Virginia Univ, Dept Anim & Nutr Sci, Morgantown, WV 26505 USA. RP Brown, JL (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, Natl Zool Pk, Front Royal, VA 22623 USA. EM brownjan@si.edu NR 52 TC 3 Z9 4 U1 2 U2 8 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X EI 1879-3231 J9 THERIOGENOLOGY JI Theriogenology PD MAR 1 PY 2011 VL 75 IS 4 BP 620 EP 627 DI 10.1016/j.theriogenology.2010.10.002 PG 8 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 725FE UT WOS:000287629800004 PM 21111473 ER PT J AU Dumbauld, BR Chapman, JW Torchin, ME Kuris, AM AF Dumbauld, Brett R. Chapman, John W. Torchin, Mark E. Kuris, Armand M. TI Is the Collapse of Mud Shrimp (Upogebia pugettensis) Populations Along the Pacific Coast of North America Caused by Outbreaks of a Previously Unknown Bopyrid Isopod Parasite (Orthione griffenis)? SO ESTUARIES AND COASTS LA English DT Article DE Parasitic castrator; Local extinctions; Introduced species; Neotrypaea californiensis; Thalassinidea ID PROBOPYRUS-PANDALICOLA; BIOLOGICAL INVASIONS; INFECTIOUS-DISEASES; BENTHIC COMMUNITY; WILLAPA BAY; DYNAMICS; HOST; EXTINCTION; CASTRATION; EPIDEMIOLOGY AB A dramatic increase in prevalence of the recently discovered bopyrid isopod parasite, Orthione griffenis, likely introduced in the 1980s from Asia to the Pacific coast of North America, coincided with the 2002 collapse of a population of its burrowing mud shrimp host, Upogebia pugettensis, in Willapa Bay, Washington that had been stable since monitoring began in 1988. An examination of whether O. griffenis infections were sufficient to cause this decline and other recently noted U. pugettensis population collapses in Pacific Coast estuaries was conducted. O. griffenis prevalence was the highest in large reproductive-sized female shrimp and caused an estimated average 68% loss of U. pugettensis reproduction in Yaquina Bay, Oregon over a 5-year period. O. griffenis prevalence fluctuated from year to year, but trends were similar in all estuaries sampled. Uninfected shrimp transplanted back into locations from which they had disappeared acquired the parasite, suggesting that O. griffenis is extremely effective at finding its host even in estuaries with very low host density. Since both U. pugettensis and O. griffenis have pelagic larval stages, their population dynamics are also influenced by coastal nearshore oceanography and estuarine recruitment success. Coastwide lack of estuarine recruitment appears to coincide with declines in density of a co-occurring thalassinid shrimp, Neotrypaea californiensis, but cannot alone explain U. pugettensis population collapses. Although patterns observed to date could be explained by the presence of either a native or introduced parasitic castrator, assumptions of a resilient co-evolved host-parasite relationship do not apply for introduced species, so continued efforts to follow the spatial extent and consequences of the O. griffenis-U. pugettensis host-parasite relationship are warranted. C1 [Dumbauld, Brett R.] ARS, USDA, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Chapman, John W.] Oregon State Univ, Hatfield Marine Sci Ctr, Dept Fisheries & Wildlife, Newport, OR 97365 USA. [Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa 08433092, Ancon, Panama. [Kuris, Armand M.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. [Kuris, Armand M.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP Dumbauld, BR (reprint author), ARS, USDA, Hatfield Marine Sci Ctr, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. EM brett.dumbauld@ars.usda.gov FU US Department of Agriculture, Agricultural Research Service; Washington State Legislature; USFWS through the Coastal Resources Alliance; NSF at Hatfield Marine Science Center; Washington Department of Fish and Wildlife; Western Regional Aquaculture Center FX This research was funded in part by the US Department of Agriculture, Agricultural Research Service, the Washington State Legislature via a grant to JWC to examine biological control of shrimp, a grant to AMK from the USFWS through the Coastal Resources Alliance, funding from NSF for the REU program at Hatfield Marine Science Center, and in-kind field assistance from the LCCSC-OYCC field crews. Historical monitoring was funded by the Washington Department of Fish and Wildlife and several grants to David Armstrong and BRD from the Western Regional Aquaculture Center. We especially thank Lee McCoy and Cara Fritz for their help in the field and with data analysis. Katelyn Cassidy, Roy Hildenbrand, Roxanna Hintzman, Kristine Feldman, Bruce Kauffman, Michael Herrle, Andy Smith, Lauren Woods, Caitlin White, Xeronimo Castaneda, Erin Ashley, Sara Heerhartz, and numerous others assisted with shrimp sampling. Finally, we thank Melanie Frazier, Vladlina Gerteseva, and two anonymous reviewers for their comments on the manuscript. NR 88 TC 21 Z9 23 U1 5 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAR PY 2011 VL 34 IS 2 BP 336 EP 350 DI 10.1007/s12237-010-9316-z PG 15 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 718SQ UT WOS:000287146900011 ER PT J AU Zhou, X Robinson, JL Geraci, CJ Parker, CR Flint, OS Etnier, DA Ruiter, D DeWalt, RE Jacobus, LM Hebert, PDN AF Zhou, Xin Robinson, Jason L. Geraci, Christy J. Parker, Charles R. Flint, Oliver S., Jr. Etnier, David A. Ruiter, David DeWalt, R. Edward Jacobus, Luke M. Hebert, Paul D. N. TI Accelerated construction of a regional DNA-barcode reference library: caddisflies (Trichoptera) in the Great Smoky Mountains National Park SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE DNA barcoding; mitochondrial DNA; COI; aquatic insects; molecular identification; biomonitoring; biodiversity; ATBI ID PARASITOID FLIES DIPTERA; POPULATION-STRUCTURE; NORTHERN CALIFORNIA; MITOCHONDRIAL-DNA; CRYPTIC DIVERSITY; GENETIC-STRUCTURE; DRUSUS-DISCOLOR; EPHEMEROPTERA; GENUS; IDENTIFICATION AB Deoxyribonucleic acid (DNA) barcoding is an effective tool for species identification and life-stage association in a wide range of animal taxa. We developed a strategy for rapid construction of a regional DNA-barcode reference library and used the caddisflies (Trichoptera) of the Great Smoky Mountains National Park (GSMNP) as a model. Nearly 1000 cytochrome c oxidase subunit I (COI) sequences, representing 209 caddisfly species previously recorded from GSMNP, were obtained from the global Trichoptera Barcode of Life campaign. Most of these sequences were collected from outside the GSMNP area. Another 645 COI sequences, representing 80 species, were obtained from specimens collected in a 3-d bioblitz (short-term, intense sampling program) in GSMNP. The joint collections provided barcode coverage for 212 species, 91% of the GSMNP fauna. Inclusion of samples from other localities greatly expedited construction of the regional DNA-barcode reference library. This strategy increased intraspecific divergence and decreased average distances to nearest neighboring species, but the DNA-barcode library was able to differentiate 93% of the GSMNP Trichoptera species examined. Global barcoding projects will aid construction of regional DNA-barcode libraries, but local surveys make crucial contributions to progress by contributing rare or endemic species and full-length barcodes generated from high-quality DNA. DNA taxonomy is not a goal of our present work, but the investigation of COI divergence patterns in caddisflies is providing new insights into broader biodiversity patterns in this group and has directed attention to various issues, ranging from the need to re-evaluate species taxonomy with integrated morphological and molecular evidence to the necessity of an appropriate interpretation of barcode analyses and its implications in understanding species diversity (in contrast to a simple claim for barcoding failure). C1 [Zhou, Xin; Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Robinson, Jason L.; Etnier, David A.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Geraci, Christy J.; Flint, Oliver S., Jr.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Parker, Charles R.] US Geol Survey, Biol Resources Discipline, Gatlinburg, TN 37738 USA. [DeWalt, R. Edward] Illinois Nat Hist Survey, Champaign, IL 61820 USA. [Jacobus, Luke M.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. RP Zhou, X (reprint author), Univ Guelph, Biodivers Inst Ontario, 50 Stone Rd E, Guelph, ON N1G 2W1, Canada. EM xinzhou@uoguelph.ca; jrobin30@utk.edu; geracic@si.edu; chuck_parker@usgs.gov; flinto@si.edu; dipnet@utk.edu; druiter@msn.com; edewalt@inhs.uiuc.edu; luke.jacobus@gmail.com; phebert@uoguelph.ca RI Zhou, Xin/D-4025-2009; Hebert, Paul/C-4161-2013 OI Zhou, Xin/0000-0002-1407-7952; Hebert, Paul/0000-0002-3081-6700 FU Discover Life in America [DLIA2007-08]; GSMNP; Natural Sciences and Engineering Research Council of Canada; Genome Canada; US Geological Survey; Environment Canada's Water Science and Technology program FX The 2007 bioblitz was supported by Discover Life in America (DLIA2007-08) and by the GSMNP. Sequencing costs and informatics support were provided by grants from the Natural Sciences and Engineering Research Council of Canada and by Genome Canada to PDNH. The US Geological Survey provided funding from the Natural Resources Protection Program to CRP. Funding from Environment Canada's Water Science and Technology program enabled surveys in New Brunswick. Parks Canada supported collecting efforts across Canada under permit number NAP-2008-1636. We thank other members of the bioblitz team including Ian Stocks, Lauren Harvey, Katy Hind, John Wilson, and Anne Timm, for aid with collections and identifications. We thank the following organizations for contributing crucial specimens to this study and hosting voucher specimens: National Museum of Natural History, University of Minnesota Insect Collection, Royal Ontario Museum, Florida A&M University, Illinois Natural History Survey, Environment Canada, and Rutgers University. Numerous collaborators have helped to collect specimens, maintain vouchers, and provide taxonomic advice. We particularly thank Ralph Holzenthal, Karl Kjer, Roger Blahnik, Donald Baird, Kristie Heard, Boris Kondratieff, John Morse, Luke Myers, and Andrew Rasmussen. Sheng Li of Peking University provided help in generating the sample distribution map. Last, we thank colleagues at the Canadian Centre for DNA Barcoding, and the Biodiversity Institute of Ontario, for their assistance in the laboratory and field. NR 60 TC 31 Z9 37 U1 4 U2 26 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD MAR PY 2011 VL 30 IS 1 BP 131 EP 162 DI 10.1899/10-010.1 PG 32 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 718IP UT WOS:000287114800012 ER PT J AU Geraci, CJ Al-Saffar, MA Zhou, X AF Geraci, Christy Jo Al-Saffar, Mohammed A. Zhou, Xin TI DNA barcoding facilitates description of unknown faunas: a case study on Trichoptera in the headwaters of the Tigris River, Iraq SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE Middle East; systematics; Hydropsyche; mitochondrial DNA; COI; biodiversity; biomonitoring ID HYDROPSYCHIDAE; QUALITY; LARVAE; INSECTA AB Monitoring water quality with aquatic insects as sentinels requires taxonomic knowledge of adult and immature life stages that is not available in many parts of the world. We used deoxyribonucleic acid (DNA) barcoding to expedite identification of larval caddisflies from 20 sites in the headwaters of the Tigris River in northern Iraq by comparing their mitochondrial cytochrome c oxidase subunit I (COI) sequences to a global reference library (the Trichoptera Barcode of Life). We obtained full-length DNA barcodes for 16 COI haplogroups from 11 genera in 9 Trichoptera families. The most haplogroups and genera were recorded from Sulaimani Province. Two distinct COI haplogroups were found for the genus Psychomyia, and 5 haplogroups were found for Hydropsyche. The Hydropsyche COI haplogroups do not form a monophyletic clade with reference to the world fauna, but 4 out of 5 haplogroups are related to other Palearctic species. Three larval Rhyacophila specimens in a single COI haplogroup are closely related to specimens of Rhyacophila nubila Zetterstedt and Rhyacophila dorsalis (Curtis) from Europe, but adults from Iraq are needed to confirm their species identity. C1 [Geraci, Christy Jo] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC USA. [Al-Saffar, Mohammed A.] Amer Univ Iraq Sulaimani, Twin Rivers Inst Sci Res, Sulaimani, Kurdistan, Iraq. [Zhou, Xin] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. RP Geraci, CJ (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC USA. EM geracic@si.edu; moalsaffar@gmail.com; xinzhou@uoguelph.ca RI Zhou, Xin/D-4025-2009 OI Zhou, Xin/0000-0002-1407-7952 FU Italian Ministry for the Environment, Land and Sea (IMELS); Natural Sciences and Engineering Research Council of Canada (NSERC); Genome Canada through the Ontario Genomics Institute; University of Guelph FX Field work was conducted by the benthic macroinvertebrates team in Nature Iraq (Ali Sadeq Al-Zubaidi and Ghazwan Al-Waili) during the Key Biodiversity Areas of Iraq Project, funded by the Italian Ministry for the Environment, Land and Sea (IMELS). Sequencing cost was supported by a grant from the Natural Sciences and Engineering Research Council of Canada (NSERC) and by grants from Genome Canada through the Ontario Genomics Institute to Paul Hebert, University of Guelph. The following institutions and individuals contributed specimens to our study or are currently housing voucher specimens: National Museum of Natural History, University of Minnesota Insect Collection, Nanjing Agricultural University, Rutgers University, and Hans Malicky. CJG thanks John C. Morse, M. Lourdes Chamorro, and Oliver S. Flint for taxonomic consultations; Terry L. Erwin for valuable editorial comments on the manuscript; and Maggie Barrett and Mackenzie Flight for imaging voucher specimens. MAA thanks Azzam Alwash, Adel Hillawi, Anna Bachmann, Giorgio Galli, Andrea Cattarossi, and Mauro Randone. Last, we thank colleagues at the Canadian Centre for DNA Barcoding for their assistance with laboratory work. NR 35 TC 11 Z9 12 U1 2 U2 11 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD MAR PY 2011 VL 30 IS 1 BP 163 EP 173 DI 10.1899/10-011.1 PG 11 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 718IP UT WOS:000287114800013 ER PT J AU Pilgrim, EM Jackson, SA Swenson, S Turcsanyi, I Friedman, E Weigt, L Bagley, MJ AF Pilgrim, Erik M. Jackson, Suzanne A. Swenson, Stephanie Turcsanyi, Istvan Friedman, Ellen Weigt, Lee Bagley, Mark J. TI Incorporation of DNA barcoding into a large-scale biomonitoring program: opportunities and pitfalls SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE DNA barcoding; taxonomic resolution; bioassessment; benthic macroinvertebrate; EPT; water quality; streams; environmental sensitivity ID TAXONOMIC RESOLUTION; BIOLOGICAL IDENTIFICATIONS; DATA QUALITY; EPHEMEROPTERA; ASSESSMENTS; TRICHOPTERA; LIFE; MACROINVERTEBRATES; BIOASSESSMENTS; COMMUNITIES AB Taxonomic identification of benthic macroinvertebrates is critical to protocols used to assess the biological integrity of aquatic ecosystems. The time, expense, and inherent error rate of species-level morphological identifications has necessitated use of genus- or family-level identifications in most large, statewide bioassessment programs. Use of coarse-scale taxonomy can obscure signal about biological condition, particularly if the range of species tolerances is large within genera or families. We hypothesized that integration of deoxyribonucleic acid (DNA) barcodes (partial cytochrome c oxidase subunit I sequences) into bioassessment protocols would provide greater discriminatory ability than genus-level identifications and that this increased specificity could lead to more sensitive assessments of water quality and habitat. Analysis of DNA barcodes from larval specimens of Ephemeroptera, Plecoptera, and Trichoptera (EPT) taxa collected as part of Maryland's Biological Stream Survey (MBSS) revealed similar to 2 to 3x as many DNA-barcode groups or molecular operational taxonomic units (mOTUs) as morphologically identified genera. As expected, geographic distributions for several mOTUs were tighter than for the parent genus, but few mOTUs showed closer associations with water-quality variables or physical-habitat features than did the genus in which they belonged. The need for improved protocols for the consistent generation of DNA barcodes is discussed. C1 [Pilgrim, Erik M.; Jackson, Suzanne A.; Bagley, Mark J.] US EPA, Ecol Exposure Res Div, Natl Exposure Res Lab, Cincinnati, OH 45268 USA. [Swenson, Stephanie] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Turcsanyi, Istvan] Dynamac Corp, Annapolis, MD 21401 USA. [Friedman, Ellen] Maryland Dept Nat Resources, Monitoring & Nontidal Assessment Div, Annapolis, MD 21401 USA. [Weigt, Lee] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA. RP Pilgrim, EM (reprint author), US EPA, Ecol Exposure Res Div, Natl Exposure Res Lab, 26 W Martin Luther King Dr, Cincinnati, OH 45268 USA. EM pilgrim.erik@epa.gov; jackson.suzanne@epa.gov; swensons@si.edu; iturcsanyi@yahoo.com; efriedman@dnr.state.md.us; weigtl@si.edu; bagley.mark@epa.gov FU US EPA Advanced Monitoring Initiative [D-06-096] FX This work was funded in part under the US EPA Advanced Monitoring Initiative and was partially completed under US EPA contract number EP-D-06-096 to Dynamac Corporation. We thank Amy Driskell, at Smithsonian Institution's Laboratory of Analytical Biology, for her in-kind contributions to this work. Ana Braam, Carrie Drake, Nancy Schable, and Ian Struewing of Dynamac Corporation, and Annette Roth, US EPA, provided technical support. Pia Marquardt from the Canadian Barcoding Network assisted with data management in the Barcode of Life Database. Ron Klauda, Dan Boward, and Michael Kashiwagi of the Maryland Department of Natural Resources provided MBSS water-quality and habitat data. David Schindel, Consortium for the Barcode of Life, and Charles Spooner, US EPA Office of Water, were collaborators in this project and provided valuable insight. Joseph Flotemersch provided valuable comments about the manuscript. NR 53 TC 21 Z9 22 U1 3 U2 40 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD MAR PY 2011 VL 30 IS 1 BP 217 EP 231 DI 10.1899/10-012.1 PG 15 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 718IP UT WOS:000287114800017 ER PT J AU Maloney, K Munguia, P Mitchell, RM AF Maloney, Kelly O. Munguia, Pablo Mitchell, Richard M. TI Anthropogenic disturbance and landscape patterns affect diversity patterns of aquatic benthic macroinvertebrates SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE beta diversity; alpha diversity; multivariate dispersion; nonmetric multidimensional scaling; ecoregion; scale ID BETA-DIVERSITY; SPECIES TRAITS; LAND-COVER; HEADWATER STREAMS; FISH ASSEMBLAGES; HABITAT QUALITY; URBAN LANDSCAPE; UNITED-STATES; HOMOGENIZATION; COMMUNITIES AB Measures of species diversity are valuable tools for assessing ecosystem health. However, most assessments have addressed individual sites or regional taxon pools, with few comparisons of differences in assemblage composition within or among regions. We examined the effects of anthropogenic disturbance on local richness (alpha diversity) and species turnover (beta diversity) of benthic macroinvertebrates in small streams within and between 2 ecoregions (Northern Piedmont vs Southeastern Plains ecoregions) of the Patuxent River basin (Maryland, USA). Regional species pools did not differ between ecoregions (Piedmont = 166 taxa, Plains = 162 taxa); however, local richness was lower in the Plains (mean = 17.4 taxa/stream) compared to the Piedmont (mean = 22.2 taxa/stream). When streams were categorized into disturbance classes (low, medium, high), local richness did not differ among categories for either region. However, at the entire Patuxent scale, local richness tended to decrease with % impervious cover in a watershed. Variation in species composition, analyzed with nonmetric multidimensional scaling (nMDS), differed significantly between Piedmont and Plains streams, and Plains streams had higher beta diversity than Piedmont streams. When partitioned by disturbance category and region, beta diversity differed only between the low-disturbance sites (Plains > Piedmont). Relationships between beta diversity and environmental variables varied by region. beta diversity was weakly negatively related to % row-crop cover in a watershed at the entire Patuxent scale. For the Piedmont region, beta diversity tended to decrease with % forest, % pasture, and % row-crop cover in a watershed. Such negative relationships between beta diversity and landuse variables indicate a possible homogenization of the assemblage. The incongruence between diversity measures and composition measures, together with differing effects of anthropogenic land use on beta diversity in the 2 regions, emphasizes the need to incorporate both alpha and beta diversity and regional environmental factors in conservation/land management studies. C1 [Maloney, Kelly O.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Munguia, Pablo] Univ Texas Austin, Inst Marine Sci, Port Aransas, TX 78373 USA. [Mitchell, Richard M.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. RP Maloney, KO (reprint author), US Geol Survey, Leetown Sci Ctr, No Appalachian Res Lab, Wellsboro, PA 16901 USA. EM kmaloney@usgs.gov; munguia@mail.utexas.edu; mitchrm@auburn.edu RI Munguia, Pablo/D-8653-2012; OI Munguia, Pablo/0000-0002-9900-2123 FU US Environmental Protection Agency National Center for Environmental Research (NCER) [R831369] FX We thank the Maryland Department of Natural Resources and Ryan King (Baylor University) for providing data on benthic macroinvertebrates, and Stephen Prince (University of Maryland) and Scott Goetz (Woods Hole Research Center) for providing land-cover data. We also thank Kathy Bailey-Boomer and Donald Weller of the Ecological Modeling lab at the Smithsonian Environmental Research Center, Chris Swan, and 2 anonymous referees for instructive comments on the manuscript. Funding for our work was provided by the US Environmental Protection Agency National Center for Environmental Research (NCER) Science to Achieve Results (STAR) grant R831369. The research described in this article was funded by the US Environmental Protection Agency, but it has not been subjected to the Agency's required peer and policy review and, therefore, does not necessarily reflect the views of the Agency, and no official endorsement should be inferred. NR 68 TC 18 Z9 18 U1 10 U2 67 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD MAR PY 2011 VL 30 IS 1 BP 284 EP 295 DI 10.1899/09-112.1 PG 12 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 718IP UT WOS:000287114800023 ER PT J AU Price, JP Wagner, WL AF Price, Jonathan P. Wagner, Warren L. TI A PHYLOGENETIC BASIS FOR SPECIES-AREA RELATIONSHIPS AMONG THREE PACIFIC ISLAND FLORAS SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE biodiversity; flora; Hawaiian Islands; Marquesas Islands; phylogeny; Society Islands; species-area relations ID NORTH-AMERICAN ORIGIN; ADAPTIVE RADIATION; TRIBE SPERMACOCEAE; HAWAIIAN-ISLANDS; FRENCH-POLYNESIA; DNA EVIDENCE; BIOGEOGRAPHY; SPECIATION; EVOLUTION; DIVERSIFICATION AB Premise of the study : The angiosperm floras of the Hawaiian, Society, and Marquesas archipelagoes are remarkably comparable ecologically and evolutionarily, a result of similar geologic history, climate, and isolation. Methods : We characterized variation in species richness among islands and whole archipelagoes by analyzing species-area relationships (SARs). By partitioning each flora into putative phylogenetic lineages each derived from a given colonization event, we explored several ways in which speciation contributes to SARs. Key results : Specifically, these groups exhibit expected island SARs and a whole archipelago SAR characterized by a steep slope. The number of species added by net cladogenesis increases with area much more quickly than the number contributed by net colonization from outside. In each of the three archipelagoes, most colonists do not speciate, while many species occur in a few diverse colonist lineages. Colonization events that are unique to a given archipelago are in more prone to speciation than lineages with close relatives in the other archipelagoes. Most lineages with relatives in all three archipelagoes have one species in each, suggesting a similar tendency not to diversify. On the other hand, a correlation between lineage size in one archipelago and that of related lineages in other archipelagoes suggests a consistent tendency among diverse groups to speciate extensively. Lineages with multiple species in each archipelago also tend to have far more species in the largest archipelago, the Hawaiian Islands. Conclusions : The most diverse lineages exhibit a strong response to archipelago area. These diverse, area-sensitive lineages contribute substantially to the slope of the inter-archipelago SAR. Regional species pools elsewhere may exhibit similar steep-sloped SARs; thus, these findings may inform how the behavior of lineages with different responses to increasing shapes these patterns. C1 [Price, Jonathan P.] Univ Hawaii, Dept Geog & Environm Sci, Hilo, HI 96720 USA. [Wagner, Warren L.] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Price, JP (reprint author), Univ Hawaii, Dept Geog & Environm Sci, 200 W Kawili St, Hilo, HI 96720 USA. EM jpprice@hawaii.edu NR 95 TC 12 Z9 12 U1 1 U2 21 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 EI 1537-2197 J9 AM J BOT JI Am. J. Bot. PD MAR PY 2011 VL 98 IS 3 BP 449 EP 459 DI 10.3732/ajb.1000388 PG 11 WC Plant Sciences SC Plant Sciences GA 734FU UT WOS:000288320600018 PM 21613138 ER PT J AU Harris, AW Mommert, M Hora, JL Mueller, M Trilling, DE Bhattacharya, B Bottke, WF Chesley, S Delbo, M Emery, JP Fazio, G Mainzer, A Penprase, B Smith, HA Spahr, TB Stansberry, JA Thomas, CA AF Harris, A. W. Mommert, M. Hora, J. L. Mueller, M. Trilling, D. E. Bhattacharya, B. Bottke, W. F. Chesley, S. Delbo, M. Emery, J. P. Fazio, G. Mainzer, A. Penprase, B. Smith, H. A. Spahr, T. B. Stansberry, J. A. Thomas, C. A. TI ExploreNEOs. II. THE ACCURACY OF THE WARM SPITZER NEAR-EARTH OBJECT SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: planetary systems; minor planets, asteroids: general; surveys ID THERMAL INFRARED OBSERVATIONS; SPACE-TELESCOPE; RADIOMETRIC DIAMETER; ARRAY CAMERA; ASTEROIDS; ALBEDO; SIZE; MISSION; MODEL; EROS AB We report on results of observations of near-Earth objects (NEOs) performed with the NASA Spitzer Space Telescope as part of our ongoing (2009-2011) Warm Spitzer NEO survey ("ExploreNEOs"), the primary aim of which is to provide sizes and albedos of some 700 NEOs. The emphasis of the work described here is an assessment of the overall accuracy of our survey results, which are based on a semi-empirical generalized model of asteroid thermal emission. The NASA Spitzer Space Telescope has been operated in the so-called Warm Spitzer mission phase since the cryogen was depleted in 2009 May, with the two shortest-wavelength channels, centered at 3.6 mu m and 4.5 mu m, of the Infrared Array Camera continuing to provide valuable data. The set of some 170 NEOs in our current Warm Spitzer results catalog contains 28 for which published taxonomic classifications are available, and 14 for which relatively reliable published diameters and albedos are available. A comparison of the Warm Spitzer results with previously published results ("ground truth"), complemented by a Monte Carlo error analysis, indicates that the rms Warm Spitzer diameter and albedo errors are +/- 20% and +/- 50%, respectively. Cases in which agreement with results from the literature is worse than expected are highlighted and discussed; these include the potential spacecraft target 138911 2001 AE(2). We confirm that 1.4 appears to be an appropriate overall default value for the relative reflectance between the V band and the Warm Spitzer wavelengths, for use in correction of the Warm Spitzer fluxes for reflected solar radiation. C1 [Harris, A. W.; Mommert, M.] DLR Inst Planetary Res, D-12489 Berlin, Germany. [Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mueller, M.; Delbo, M.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA. [Bhattacharya, B.] NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA. [Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Harris, AW (reprint author), DLR Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM alan.harris@dlr.de OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650; Thomas, Cristina/0000-0003-3091-5757 FU NASA; DFG [SPP 1385] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Liberal use was made of the excellent JPL Horizons System for generating ephemerides. We acknowledge support by DFG through SPP 1385: The first ten million years of the solar system-a planetary materials approach. We thank the anonymous referee for comments that led to significant improvements in the paper. NR 50 TC 13 Z9 13 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2011 VL 141 IS 3 AR 75 DI 10.1088/0004-6256/141/3/75 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 719TC UT WOS:000287231000006 ER PT J AU Martin, S Krips, M Martin-Pintado, J Aalto, S Zhao, JH Peck, AB Petitpas, GR Monje, R Greve, TR An, T AF Martin, S. Krips, M. Martin-Pintado, J. Aalto, S. Zhao, J. -H. Peck, A. B. Petitpas, G. R. Monje, R. Greve, T. R. An, T. TI The Submillimeter Array 1.3 mm line survey of Arp 220 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; galaxies: abundances; galaxies: active; galaxies: individual: Arp 220; galaxies: ISM; galaxies: starburst ID ULTRALUMINOUS INFRARED GALAXIES; STARBURST GALAXIES; MOLECULAR CLOUD; STAR-FORMATION; DENSE GAS; NGC 253; INTERACTING GALAXIES; CHANDRA OBSERVATIONS; INTERSTELLAR-MEDIUM; SUPERNOVA-REMNANTS AB Context. Though Arp 220 is the closest and by far the most studied ULIRG, a discussion is still ongoing on the main power source driving its huge infrared luminosity. Aims. To study the molecular composition of Arp 220 in order to find chemical fingerprints associated with the main heating mechanisms within its nuclear region. Methods. We present the first aperture synthesis unbiased spectral line survey toward an extragalactic object. The survey covered the 40 GHz frequency range between 202 and 242 GHz of the 1.3 mm atmospheric window. Results. We find that 80% of the observed band shows molecular emission, with 73 features identified from 15 molecular species and 6 isotopologues. The C-13 isotopic substitutions of HC3N and transitions from (H2O)-O-18, (SiO)-Si-29, and CH2CO are detected for the first time outside the Galaxy. No hydrogen recombination lines have been detected in the 40 GHz window covered. The emission feature at the transition frequency of H31 alpha line is identified to be an HC3N molecular line, challenging the previous detections reported at this frequency. Within the broad observed band, we estimate that 28% of the total measured flux is due to the molecular line contribution, with CO only contributing 9% to the overall flux. We present maps of the CO emission at a resolution of 2.9 '' x 1.9 '' which, though not enough to resolve the two nuclei, recover all the single-dish flux. The 40 GHz spectral scan has been modelled assuming LTE conditions and abundances are derived for all identified species. Conclusions. The chemical composition of Arp 220 shows no clear evidence of an AGN impact on the molecular emission but seems indicative of a purely starburst-heated ISM. The overabundance of H2S and the low isotopic ratios observed suggest a chemically enriched environment by consecutive bursts of star formation, with an ongoing burst at an early evolutionary stage. The large abundance of water (similar to 10(-5)), derived from the isotopologue (H2O)-O-18, as well as the vibrationally excited emission from HC3N and CH3CN are claimed to be evidence of massive star forming regions within Arp 220. Moreover, the observations put strong constraints on the compactness of the starburst event in Arp 220. We estimate that such emission would require similar to 2-8 x 10(6) hot cores, similar to those found in the Sgr B2 region in the Galactic center, concentrated within the central 700 pc of Arp 220. C1 [Martin, S.] European So Observ, Santiago 19, Chile. [Krips, M.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [Martin-Pintado, J.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Aalto, S.] Chalmers, Onsala Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Zhao, J. -H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peck, A. B.] Joint ALMA Observ, Santiago 19, Chile. [Petitpas, G. R.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Monje, R.] CALTECH, Pasadena, CA 91125 USA. [Greve, T. R.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [An, T.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. RP Martin, S (reprint author), European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago 19, Chile. EM smartin@eso.org RI he, shuyi/K-2082-2014; Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU Smithsonian Institution; Academia Sinica FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 99 TC 31 Z9 31 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2011 VL 527 AR A36 DI 10.1051/0004-6361/201015855 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 723CP UT WOS:000287484100051 ER PT J AU Batalha, NM Borucki, WJ Bryson, ST Buchhave, LA Caldwell, DA Christensen-Dalsgaard, J Ciardi, D Dunham, EW Fressin, F Gautier, TN Gilliland, RL Haas, MR Howell, SB Jenkins, JM Kjeldsen, H Koch, DG Latham, DW Lissauer, JJ Marcy, GW Rowe, JF Sasselov, DD Seager, S Steffen, JH Torres, G Basri, GS Brown, TM Charbonneau, D Christiansen, J Clarke, B Cochran, WD Dupree, A Fabrycky, DC Fischer, D Ford, EB Fortney, J Girouard, FR Holman, MJ Johnson, J Isaacson, H Klaus, TC Machalek, P Moorehead, AV Morehead, RC Ragozzine, D Tenenbaum, P Twicken, J Quinn, S VanCleve, J Walkowicz, LM Welsh, WF Devore, E Gould, A AF Batalha, Natalie M. Borucki, William J. Bryson, Stephen T. Buchhave, Lars A. Caldwell, Douglas A. Christensen-Dalsgaard, Jorgen Ciardi, David Dunham, Edward W. Fressin, Francois Gautier, Thomas N., III Gilliland, Ronald L. Haas, Michael R. Howell, Steve B. Jenkins, Jon M. Kjeldsen, Hans Koch, David G. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Rowe, Jason F. Sasselov, Dimitar D. Seager, Sara Steffen, Jason H. Torres, Guillermo Basri, Gibor S. Brown, Timothy M. Charbonneau, David Christiansen, Jessie Clarke, Bruce Cochran, William D. Dupree, Andrea Fabrycky, Daniel C. Fischer, Debra Ford, Eric B. Fortney, Jonathan Girouard, Forrest R. Holman, Matthew J. Johnson, John Isaacson, Howard Klaus, Todd C. Machalek, Pavel Moorehead, Althea V. Morehead, Robert C. Ragozzine, Darin Tenenbaum, Peter Twicken, Joseph Quinn, Samuel VanCleve, Jeffrey Walkowicz, Lucianne M. Welsh, William F. Devore, Edna Gould, Alan TI KEPLER'S FIRST ROCKY PLANET: KEPLER-10b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (Kepler-10 KIC 11904151, 2MASS 19024305+5014286); techniques: photometric; techniques: spectroscopic ID MASS-RADIUS RELATIONSHIPS; TESTING BLEND SCENARIOS; LIGHT CURVES; INITIAL CHARACTERISTICS; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS; SUPER-EARTHS; CADENCE DATA; EXOPLANET; STARS AB NASA's Kepler Mission uses transit photometry to determine the frequency of Earth-size planets in or near the habitable zone of Sun-like stars. The mission reached a milestone toward meeting that goal: the discovery of its first rocky planet, Kepler-10b. Two distinct sets of transit events were detected: (1) a 152 +/- 4 ppm dimming lasting 1.811 +/- 0.024 hr with ephemeris T [BJD] = 2454964.57375(-0.00082)(+0.00060) + N * 0.837495(-0.000005)(+0.000004) days and (2) a 376 +/- 9 ppm dimming lasting 6.86 +/- 0.07 hr with ephemeris T [BJD] = 2454971.6761(-0.0023)(+0.0020) + N * 45.29485(-0.00076)(+0.00065) days. Statistical tests on the photometric and pixel flux time series established the viability of the planet candidates triggering ground-based follow-up observations. Forty precision Doppler measurements were used to confirm that the short-period transit event is due to a planetary companion. The parent star is bright enough for asteroseismic analysis. Photometry was collected at 1 minute cadence for > 4 months from which we detected 19 distinct pulsation frequencies. Modeling the frequencies resulted in precise knowledge of the fundamental stellar properties. Kepler-10 is a relatively old (11.9 +/- 4.5 Gyr) but otherwise Sun-like main-sequence star with T-eff = 5627 +/- 44 K, M-star = 0.895 +/- 0.060M(circle dot), and R-star = 1.056 +/- 0.021R(circle dot). Physical models simultaneously fit to the transit light curves and the precision Doppler measurements yielded tight constraints on the properties of Kepler-10b that speak to its rocky composition: M-P = 4.56(-1.29)(+1.17) M-circle plus, R-P = 1.416(-0.036)(+0.033) R-circle plus, and rho P = 8.8(-2.9)(+2.1) g cm(-3). Kepler-10b is the smallest transiting exoplanet discovered to date. C1 [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Caldwell, Douglas A.; Jenkins, Jon M.; Clarke, Bruce; Machalek, Pavel; Tenenbaum, Peter; Twicken, Joseph; VanCleve, Jeffrey; Devore, Edna] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Buchhave, Lars A.; Fressin, Francois; Latham, David W.; Sasselov, Dimitar D.; Torres, Guillermo; Charbonneau, David; Dupree, Andrea; Fabrycky, Daniel C.; Holman, Matthew J.; Ragozzine, Darin; Quinn, Samuel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Ciardi, David] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Marcy, Geoffrey W.; Basri, Gibor S.; Isaacson, Howard; Walkowicz, Lucianne M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Seager, Sara] MIT, Cambridge, MA 02139 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Ford, Eric B.; Moorehead, Althea V.; Morehead, Robert C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Girouard, Forrest R.; Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. RP Batalha, NM (reprint author), San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. EM Natalie.Batalha@sjsu.edu RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183 FU National Science Foundation; NASA's Science Mission Directorate FX The authors thank Carly Chubak for computing the barycentric radial velocity of Kepler-10. J.C.D. acknowledges support from The National Center for Atmospheric Research which is sponsored by the National Science Foundation. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. NR 81 TC 282 Z9 283 U1 29 U2 115 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 27 DI 10.1088/0004-637X/729/1/27 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300027 ER PT J AU Boroson, B Kim, DW Fabbiano, G AF Boroson, Bram Kim, Dong-Woo Fabbiano, Giuseppina TI REVISITING WITH CHANDRA THE SCALING RELATIONS OF THE X-RAY EMISSION COMPONENTS (BINARIES, NUCLEI, AND HOT GAS) OF EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; X-rays: galaxies ID ELLIPTIC GALAXIES; STELLAR POPULATION; GLOBULAR-CLUSTERS; DEEP CHANDRA; NGC 3379; MULTIPARAMETRIC ANALYSIS; CATACLYSMIC VARIABLES; LUMINOSITY FUNCTION; EINSTEIN SAMPLE; VIRGO CLUSTER AB We have selected a sample of 30 normal (non-cD) early-type galaxies, for all of which optical spectroscopy is available and which have been observed with Chandra to a depth such as to ensure the detection of bright low-mass X-ray binaries (LMXBs) with L-X > 1038 erg s(-1). This sample includes a larger fraction of gas-poor galaxies than previously studied samples and covers a wide range of stellar luminosity (L-K), velocity dispersion (sigma(*)), globular cluster specific frequency (S-N), and stellar age. We derive X-ray luminosities (or upper limits) from the different significant X-ray components of these galaxies: nuclei, detected and undetected LMXBs, coronally active binaries (ABs), cataclysmic variables (CVs), and hot gas. The ABs and CVs contribution is estimated from the L-X-L-K scaling relation of M31 and M32. The contribution of undetected LMXBs is estimated both by fitting the spectra of the unresolved X-ray emission and by extrapolating the LMXB X-ray luminosity function. On average, the X-ray luminosity of LMXBs is a factor of similar to 10 higher than that of ABs+CVs. By spectral fitting the emission (also considering gas emission in the regions of point sources), we estimate the contribution of the hot gas. We find our sample equally divided among galaxies with L-X(gas) > L-X(LMXB), L-X(ABCV) <= L-X(gas) <= L-X(LMXB), and L-X(gas) <= L-X(ABCV). The results for the nuclei are consistent with those discussed by Pellegrini. We derive a revised scaling relation between the integrated X-ray luminosity of LMXBs in a galaxy and the L-K luminosity of the host galaxy: L-X(LMXB)/L-K similar to 1029 erg s(-1) L-K(-1) with 50% 1 sigma rms; moreover, we also obtain a tighter L-X(LMXB)/L-K-S-N relation than previously published. We revisit the relations between hot gas content and other galaxy parameters (L-K, sigma*), which in most previous work was based on the integrated total X-ray luminosity of the galaxy, finding a steeper L-X(gas)-L-K relation with larger scatter than reported in the literature. We find a positive correlation between the luminosity and temperature of the hot interstellarmedium, significantly tighter than reported by earlier studies. This relation is particularly well defined in the subsample with sigma(*)> 240 km s(-1), where it may be related to the analogous correlation found in cD galaxies and groups/clusters. However, the gas-poor galaxies with the shallowest potentials (sigma(*) < 200 km s(-1)) also follow this relation, contrary to the expected anti-correlation in a simple outflow/wind scenario. Galaxies with intermediate values of sigma(*) instead tend to have the same kT, while L-X(gas) spans a factor of similar to 20; among these galaxies, we find a moderate, positive correlation between L-X(gas) and the average stellar age, possibly suggesting a transition from halo retention to outflow caused by rejuvenated star formation associated with recent mergers. C1 [Boroson, Bram; Kim, Dong-Woo; Fabbiano, Giuseppina] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Boroson, B (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. FU Chandra GO grant [G08-9133X]; XMM-Newton GO grant [NNX09AT20G]; National Aeronautics and Space Administration; National Science Foundation FX The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities, and have extracted archival data from the Chandra archives. This work was supported by the Chandra GO grant G08-9133X (PI: D.-W.K.) and XMM-Newton GO grant NNX09AT20G (PI: D.-W.K.). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. We thank Silvia Pellegrini for useful discussions. NR 99 TC 85 Z9 85 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 12 DI 10.1088/0004-637X/729/1/12 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300012 ER PT J AU Debes, JH Hoard, DW Kilic, M Wachter, S Leisawitz, DT Cohen, M Kirkpatrick, JD Griffith, RL AF Debes, John H. Hoard, D. W. Kilic, Mukremin Wachter, Stefanie Leisawitz, David T. Cohen, Martin Kirkpatrick, J. Davy Griffith, Roger L. TI THE WIRED SURVEY. I. A BRIGHT IR EXCESS DUE TO DUST AROUND THE HEAVILY POLLUTED WHITE DWARF GALEX J193156.8+011745 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; white dwarfs ID ALL-SKY SURVEY; SPITZER-SPACE-TELESCOPE; GASEOUS DEBRIS DISC; SOURCE INFRARED SKY; PLANETARY SYSTEMS; STELLAR EVOLUTION; MU-M; G29-38; ACCRETION; CATALOG AB With the launch of the Wide-Field Infrared Survey Explorer (WISE), a new era of detecting planetary debris around white dwarfs (WDs) has begun with the WISE InfraRed Excesses around Degenerates (WIRED) Survey. The WIRED survey will be sensitive to substellar objects and dusty debris around WDs out to distances exceeding 100 pc, well beyond the completeness level of local WDs and covering a large fraction of known WDs detected with the SDSS DR4 WD catalog. In this paper, we report an initial result of the WIRED survey, the detection of the heavily polluted hydrogen WD (spectral type DAZ) GALEX J193156.8+011745 at 3.35 and 4.6 mu m. We find that the excess is consistent with either a narrow dusty ring with an inner radius of 29 R-WD, outer radius of 40 R-WD, and a face-on inclination, or a disk with an inclination of 70 degrees, an inner radius of 23 R-WD, and an outer radius of 80 R-WD. We also report initial optical spectroscopic monitoring of several metal lines present in the photosphere and find no variability in the line strengths or radial velocities of the lines. We rule out all but planetary mass companions to GALEX1931 out to 0.5 AU. C1 [Debes, John H.; Leisawitz, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Kilic, Mukremin] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Wachter, Stefanie; Kirkpatrick, J. Davy; Griffith, Roger L.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Cohen, Martin] Monterey Inst Res Astron, Marina, CA 93933 USA. RP Debes, JH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI Hoard, Donald W./0000-0002-6800-6519 FU NASA; National Science Foundation; NASA through UCLA [1000-S-MA756]; UCLA [FAU 26311] FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work is based on data obtained from (1) the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA); (2) the Two Micron All Sky Survey, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by NASA and the National Science Foundation; (3) the Hale Telescope, Palomar Observatory, as part of a continuing collaboration between Caltech, NASA/JPL, and Cornell University; (4) the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile; (5) the ESO Telescopes at the La Silla or Paranal Observatories; (6) the SIMBAD database, operated at CDS, Strasbourg, France; and (7) the NASA/IPAC Infrared Science Archive, which is operated by JPL, Caltech, under a contract with NASA. We thank D. Steeghs for obtaining spectra of GALEX1931 on July 7-8 and N. Morrell for obtaining spectra of GALEX1931 on August 2-3. M. C. thanks NASA for supporting his participation in this work through UCLA Sub-Award 1000-S-MA756 with a UCLA FAU 26311 to MIRA. NR 50 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 MAR 1 PY 2011 VL 729 IS 1 AR 4 DI 10.1088/0004-637X/729/1/4 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300004 ER PT J AU Foley, RJ Kasen, D AF Foley, Ryan J. Kasen, Daniel TI MEASURING EJECTA VELOCITY IMPROVES TYPE Ia SUPERNOVA DISTANCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; dust, extinction; supernovae: general ID LIGHT CURVES; DARK ENERGY; SPECTRA; LUMINOSITY; DIVERSITY; CONSTRAINTS; MODEL; INDICATORS; EXPLOSION; ASYMMETRY AB We use a sample of 121 spectroscopically normal Type Ia supernovae (SNe Ia) to show that their intrinsic color is correlated with their ejecta velocity, as measured from the blueshift of the Si II lambda 6355 feature near maximum brightness, nu(Si) (II). The SN Ia sample was originally used by Wang et al. to show that the relationship between color excess and peak magnitude, which in the absence of intrinsic color differences describes a reddening law, was different for two subsamples split by nu(Si) (II) (defined as "Normal" and "High Velocity"). We verify this result, but find that the two subsamples have the same reddening law when extremely reddened events (E(B - V) > 0.35 mag) are excluded. We also show that (1) the High-Velocity subsample is offset by similar to 0.06 mag to the red from the Normal subsample in the (B-max - V-max)-M-V plane, (2) the B-max - V-max cumulative distribution functions of the two subsamples have nearly identical shapes, but the High-Velocity subsample is offset by similar to 0.07 mag to the red in B-max - V-max, and (3) the bluest High-Velocity SNe Ia are similar to 0.10 mag redder than the bluest Normal SNe Ia. Together, this evidence indicates a difference in intrinsic color for the subsamples. Accounting for this intrinsic color difference reduces the scatter in Hubble residuals from 0.190 mag to 0.130 mag for SNe Ia with AV less than or similar to 0.7 mag. The scatter can be further reduced to 0.109 mag by exclusively using SNe Ia from the Normal subsample. Additionally, this result can at least partially explain the anomalously low values of R-V found in large SN Ia samples. We explain the correlation between ejecta velocity and color as increased line blanketing in the High-Velocity SNe Ia, causing them to become redder. We discuss some implications of this result, and stress the importance of spectroscopy for future SN Ia cosmology surveys, with particular focus on the design of WFIRST. C1 [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Kasen, Daniel] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Nucl Sci, Berkeley, CA 94720 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu FU DOE [DE-FC02-06ER41438]; INCITE award FX This research has been supported by the DOE SciDAC Program (DE-FC02-06ER41438). Computing time was provided by ORNL through an INCITE award and by NERSC. NR 56 TC 74 Z9 74 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 55 DI 10.1088/0004-637X/729/1/55 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300055 ER PT J AU Rasia, E Mazzotta, P Evrard, A Markevitch, M Dolag, K Meneghetti, M AF Rasia, E. Mazzotta, P. Evrard, A. Markevitch, M. Dolag, K. Meneghetti, M. TI SCALING RELATION IN TWO SITUATIONS OF EXTREME MERGERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: miscellaneous; galaxies: clusters: general; methods: numerical; X-rays: galaxies: clusters ID X-RAY-CLUSTERS; MASS-TEMPERATURE RELATION; GALAXY CLUSTERS; DARK-MATTER; INTRACLUSTER MEDIUM; COSMOLOGICAL SIMULATIONS; GAS MOTIONS; T RELATION; SAMPLE; EVOLUTION AB Clusters of galaxies are known to be dynamically active systems, yet X-ray studies of the low-redshift population exhibit tight scaling laws. In this work, we extend previous studies of this apparent paradox using numerical simulations of two extreme merger cases, one is a high Mach number (above 2.5) satellite merger similar to the "bullet cluster" and the other is a merger of nearly equal-mass progenitors. Creating X-ray images densely sampled in time, we construct T-X, M-gas, and Y-X measures within R-500 and compare to the calibrations of Kravtsov et al. We find that these extreme merger cases respect the scaling relations, for both intrinsic measures and for measures derived from appropriately masked, synthetic Chandra X-ray images. The masking procedure plays a critical role in the X-ray temperature calculation, while it is irrelevant in the X-ray gas mass derivation. Miscentering up to 100 kpc does not influence the result. The observationally determined radius R-500 might conduce to systematic shifts in M-gas and Y-X, which increases the total mass scatter. C1 [Rasia, E.; Evrard, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Mazzotta, P.; Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Dolag, K.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. RP Rasia, E (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM rasia@umich.edu RI Meneghetti, Massimo/O-8139-2015; Mazzotta, Pasquale/B-1225-2016; OI Meneghetti, Massimo/0000-0003-1225-7084; Mazzotta, Pasquale/0000-0002-5411-1748; Evrard, August/0000-0002-4876-956X; rasia, elena/0000-0003-4175-002X FU ASI-INAF [I/023/05/0, I/088/06/0]; NASA through Chandra X-ray Center [PF5-70042]; NSF [AST-0708150]; DFG; European Commission [228398]; INFN [PD51]; NASA [NAS8-03060, NNX09AP36G, NNX10AF61G] FX We thank Stefano Borgani, Stefano Ettori, Gabriel Pratt, Alexey Vikhlinin, and the anonymous referee for their constructive comments. We acknowledge financial contribution from contracts ASI-INAF I/023/05/0, ASI-INAF I/088/06/0, and INFN PD51. Support for this work was also provided by NASA through Chandra Postdoctoral Fellowship grant number PF5-70042 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under the contract NAS8-03060. E. R. acknowledges the Michigan Society of Fellows. A. E. E. acknowledges support from NSF AST-0708150 and NASA ATP grant NNX10AF61G. P. M. acknowledges support from NASA NNX09AP36G. K. D. acknowledges support from the DFG Priority Programme 1177 and additional support by the DFG Cluster of Excellence "Origin and Structure of the Universe." The work has been performed under the HPC-EUROPA2 project (project number: 228398) with the support of the European Commission-Capacities Area-Research Infrastructures. NR 58 TC 21 Z9 21 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2011 VL 729 IS 1 AR 45 DI 10.1088/0004-637X/729/1/45 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720BN UT WOS:000287255300045 ER PT J AU Marshall, HL Gelbord, JM Schwartz, DA Murphy, DW Lovell, JEJ Worrall, DM Birkinshaw, M Perlman, ES Godfrey, L Jauncey, DL AF Marshall, H. L. Gelbord, J. M. Schwartz, D. A. Murphy, D. W. Lovell, J. E. J. Worrall, D. M. Birkinshaw, M. Perlman, E. S. Godfrey, L. Jauncey, D. L. TI AN X-RAY IMAGING SURVEY OF QUASAR JETS: TESTING THE INVERSE COMPTON MODEL SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: jets; surveys ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; HEMISPHERE ICRF SOURCES; DOMINATED RADIO-SOURCES; LARGE-SCALE JETS; VLBI OBSERVATIONS; COMPLETE SAMPLE; CHANDRA OBSERVATIONS; RELATIVISTIC JETS; VLA OBSERVATIONS AB We present results from continued Chandra X-ray imaging and spectroscopy of a flux-limited sample of flat spectrum radio-emitting quasars with jet-like extended structure. X-rays are detected from 24 of the 39 jets observed so far. We compute the distribution of alpha(rx), the spectral index between the X-ray and radio bands, showing that it is broad, extending at least from 0.8 to 1.2. While there is a general trend that the radio brightest jets are detected most often, it is clear that predicting the X-ray flux from the radio knot flux densities is risky, so a shallow X-ray survey is the most effective means for finding jets that are X-ray bright. We test the model in which the X-rays result from inverse Compton (IC) scattering of cosmic microwave background (CMB) photons by relativistic electrons in the jet moving with a high bulk Lorentz factor nearly along the line of sight. Depending on how the jet magnetic fields vary with z, the observed X-ray to radio flux ratios do not follow the redshift dependence expected from the IC-CMB model. For a subset of our sample with known superluminal motion based on VLBI observations, we estimate the angle of the kiloparsec-scale jet to the line of sight by considering the additional information in the bends observed between parsec-and kiloparsec-scale jets. These angles are sometimes much smaller than estimates based on the IC-CMB model with a Lorentz factor of 15, indicating that these jets may decelerate significantly from parsec scales to kiloparsec scales. C1 [Marshall, H. L.; Gelbord, J. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gelbord, J. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Gelbord, J. M.] Penn State Univ, Dept Astron & Astrophys, State Coll, PA 16801 USA. [Schwartz, D. A.; Worrall, D. M.; Birkinshaw, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, D. W.; Godfrey, L.; Jauncey, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lovell, J. E. J.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Worrall, D. M.; Birkinshaw, M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Perlman, E. S.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Perlman, E. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Godfrey, L.] Curtin Univ Technol, Curtin Inst Radio Astron, Bentley, WA 6845, Australia. RP Marshall, HL (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM hermanm@space.mit.edu; jgelbord@astro.psu.edu; das@head-cfa.harvard.edu; david.murphy@jpl.nasa.gov; jim.lovell@utas.edu.au; D.Worrall@bristol.ac.uk; Mark.Birkinshaw@bristol.ac.uk; eperlman@fit.edu; L.Godfrey@curtin.edu.au; David.Jauncey@csiro.au RI Godfrey, Leith/B-5283-2013 FU National Aeronautics and Space Administration (NASA) through the Smithsonian Astrophysical Observatory (SAO) [SV3-73016]; NASA [NAS8-03060, NAS 8-39073]; CXC [GO4-5124X]; Commonwealth of Australia for operation as a National Facility FX We thank Marshall Cohen for communicating results in advance of publication. Support for this work was provided in part by the National Aeronautics and Space Administration (NASA) through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of the Chandra X-Ray Center (CXC), which is operated by SAO for and on behalf of NASA under contract NAS8-03060. Support was also provided by NASA under contract NAS 8-39073 to SAO. J.M.G. was partially supported under Chandra grant GO4-5124X to MIT from the CXC. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009a). This research has made use of the United States Naval Observatory (USNO) Radio Reference Frame Image Database (RRFID). The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 50 TC 17 Z9 18 U1 0 U2 7 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 MAR PY 2011 VL 193 IS 1 DI 10.1088/0067-0049/193/1/15 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZF UT WOS:000289059000015 ER PT J AU Krupnik, I AF Krupnik, Igor TI 'How many Eskimo words for ice?' Collecting Inuit sea ice terminologies in the International Polar Year 2007-2008 SO CANADIAN GEOGRAPHER-GEOGRAPHE CANADIEN LA English DT Article DE Inuit; sea ice; Indigenous knowledge; International Polar Year; human geography; Inuit; glace de mer; connaissances indigenes; Annee polaire internationale; geographie humaine ID FREEZE/THAW PROCESSES; HUMAN GEOGRAPHIES; NUNAVUT; CANADA; SNOW AB Inuit knowledge of the sea ice environment has been praised by generations of early explorers, arctic travellers, natural scientists, anthropologists, and popular writers. Surprisingly little has been done to systematically document and analyze the richness of the Inuit sea ice nomenclatures until quite recently. This article reviews the history of Inuit (Eskimo) sea ice terminology collection, including efforts undertaken in 2005-2009 for the International Polar Year (IPY) 2007-2008. Altogether, a database of 35 indigenous ice nomenclatures from the Bering Sea to East Greenland has been created, displaying the richness of over 1,500 terms for sea ice in all Inuit/Eskimo languages and most regional dialects, as well as in other indigenous northern languages (Chukchi, Dena'ina Athabascan, and Sami). Processing these vocabularies, analyzing the origins and historical geography of the Inuit sea ice nomenclatures, and returning the data to participating communities as educational, heritage, and language materials may become one of the lasting contributions of the IPY 2007-2008 program.Des generations de premiers explorateurs, de voyageurs des regions nordiques, de chercheurs en science naturelle, de specialistes en anthropologie et d'ecrivains populaires ont toutes admire les connaissances des Inuits au sujet de la glace de mer. Il est surprenant de constater le faible interet porte a l'etude et l'analyse systematiques de la riche nomenclature de la glace de mer utilisee par les Inuits. Cet article dresse un portrait historique de la collecte de donnees terminologiques aupres des Inuits (Esquimaux) sur la glace de mer, incluant les travaux qui se sont deroules entre 2005 et 2009 dans le cadre de l'Annee polaire internationale (API) 2007-2008. Une base terminologique a ainsi ete constituee qui regroupe un ensemble de 35 nomenclatures indigenes de la glace de mer, de la Mer de Bering jusqu'a l'est du Groenland. Elle permet de decouvrir la richesse de plus de 1500 mots pour designer la glace de mer dans toutes les langues eskimo-aleoutes et la plupart des dialectes regionaux, ainsi que dans les autres langues nordiques parlees par des groupes autochtones (les langues Chukchi, Dena'ina Athabascan, et Sami). Le traitement de ce vocabulaire, l'analyse des sources et de la geographie historique de la nomenclature de la glace de mer utilisee par les Inuits, ainsi que la restitution des donnees aux collectivites participantes sous forme de materiels pedagogiques, patrimoniaux et linguistiques compteront parmi les contributions les plus marquantes du programme API 2007-2008. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20004 USA. RP Krupnik, I (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20004 USA. EM krupniki@si.edu NR 85 TC 3 Z9 3 U1 1 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0008-3658 J9 CAN GEOGR-GEOGR CAN JI Can. Geogr.-Geogr. Can. PD SPR PY 2011 VL 55 IS 1 BP 56 EP 68 DI 10.1111/j.1541-0064.2010.00345.x PG 13 WC Geography SC Geography GA 741ZE UT WOS:000288906700007 ER PT J AU Borja, A Tunberg, BG AF Borja, A. Tunberg, B. G. TI Assessing benthic health in stressed subtropical estuaries, eastern Florida, USA using AMBI and M-AMBI SO ECOLOGICAL INDICATORS LA English DT Article DE Benthic health; Quality assessment; Biotic indices; AMBI; M-AMBI; Subtropical lagoon; Eastern Florida ID INDIAN RIVER LAGOON; MARINE-BIOTIC-INDEX; ST-LUCIE-ESTUARY; ECOLOGICAL STATUS ASSESSMENT; COUNTRY NORTHERN SPAIN; CHESAPEAKE BAY; SOUTH FLORIDA; MACROBENTHIC COMMUNITY; QUALITY ASSESSMENT; HABITAT QUALITY AB The Indian River Lagoon (IRL) and the St. Lucie Estuary (SLE), both located in Florida, USA, are affected by a variety of anthropogenic pressures. Benthic macroinvertebrates have been monitored quarterly since February 2005, at 15 stations, in order to assess benthic health. Since the SLE and IRL are situated in a subtropical area, it is affected by two major climatic seasons, dry (winter) and wet (summer). This contribution investigates the application of the AZTI's Marine Biotic Index (AMBI) and multivariate-AMBI (M-AMBI), to assess the ecological status of these estuaries. AMBI was firstly calculated after assigning most of the previously unassigned species to each of the five ecological groups (from sensitive to first order opportunistic species). Three main benthic assemblages, associated to oligohaline, meso-polyhaline and euhaline stretches, have been identified within the area. Reference conditions of richness, Shannon's diversity and AMBI have been derived for these assemblages; M-AMBI has then been calculated. Both methods show that the inner part of the SLE is affected by anthropogenic pressures (increased freshwater inflow, with elevated nutrient input, and sedimentation), whilst the IRL is less affected. We have demonstrated that AMBI and M-AMBI are insensitive to the dramatic seasonal changes occurring in the SLE/IRL. At some of the stations a significant positive trend in benthic quality has been identified, linked to the polluted freshwater discharges decrease. The use of both tools seems adequate in assessing benthic health in this subtropical area. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Borja, A.] AZTI Tecnalia, Div Marine Res, Pasaia 20110, Spain. [Tunberg, B. G.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Borja, A (reprint author), AZTI Tecnalia, Div Marine Res, Portualdea S-N, Pasaia 20110, Spain. EM aborja@pas.azti.es; tunberg@si.edu OI Borja, Angel/0000-0003-1601-2025 FU South Florida Water Management District; Fish and Wildlife Research Institute, St Petersburg, Florida; Smithsonian Institution FX This investigation was supported by the South Florida Water Management District, and the Fish and Wildlife Research Institute, St Petersburg, Florida, and the Smithsonian Institution. We are very grateful to Michelle Stephens, Scott Jones and Erin Linley for their excellent work in the field, in the laboratory, and with the database. Special thanks are due to Sherry Reed for invaluable help during the field work. The comments of two anonymous reviewers have improved this paper. This paper is contribution number 500 from AZTI-Tecnalia (Marine Research Division), and the Smithsonian Marine Station contribution No. 823. NR 74 TC 44 Z9 57 U1 2 U2 26 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1470-160X J9 ECOL INDIC JI Ecol. Indic. PD MAR PY 2011 VL 11 IS 2 BP 295 EP 303 DI 10.1016/j.ecolind.2010.05.007 PG 9 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 690UW UT WOS:000285035000009 ER PT J AU Onoda, Y Westoby, M Adler, PB Choong, AMF Clissold, FJ Cornelissen, JHC Diaz, S Dominy, NJ Elgart, A Enrico, L Fine, PVA Howard, JJ Jalili, A Kitajima, K Kurokawa, H McArthur, C Lucas, PW Markesteijn, L Perez-Harguindeguy, N Poorter, L Richards, L Santiago, LS Sosinski, EE Van Bael, SA Warton, DI Wright, IJ Wright, SJ Yamashita, N AF Onoda, Yusuke Westoby, Mark Adler, Peter B. Choong, Amy M. F. Clissold, Fiona J. Cornelissen, Johannes H. C. Diaz, Sandra Dominy, Nathaniel J. Elgart, Alison Enrico, Lucas Fine, Paul V. A. Howard, Jerome J. Jalili, Adel Kitajima, Kaoru Kurokawa, Hiroko McArthur, Clare Lucas, Peter W. Markesteijn, Lars Perez-Harguindeguy, Natalia Poorter, Lourens Richards, Lora Santiago, Louis S. Sosinski, Enio E., Jr. Van Bael, Sunshine A. Warton, David I. Wright, Ian J. Wright, S. Joseph Yamashita, Nayuta TI Global patterns of leaf mechanical properties SO ECOLOGY LETTERS LA English DT Review DE Biomechanics; fibre; global-trend; leaf traits; meta-analysis; toughness ID FRACTURE-TOUGHNESS; LIFE-SPAN; LATITUDINAL VARIATION; ECONOMICS SPECTRUM; LEAVES; PLANTS; TRAITS; SHADE; PHOTOSYNTHESIS; BIOMECHANICS AB P>Leaf mechanical properties strongly influence leaf lifespan, plant-herbivore interactions, litter decomposition and nutrient cycling, but global patterns in their interspecific variation and underlying mechanisms remain poorly understood. We synthesize data across the three major measurement methods, permitting the first global analyses of leaf mechanics and associated traits, for 2819 species from 90 sites worldwide. Key measures of leaf mechanical resistance varied c. 500-800-fold among species. Contrary to a long-standing hypothesis, tropical leaves were not mechanically more resistant than temperate leaves. Leaf mechanical resistance was modestly related to rainfall and local light environment. By partitioning leaf mechanical resistance into three different components we discovered that toughness per density contributed a surprisingly large fraction to variation in mechanical resistance, larger than the fractions contributed by lamina thickness and tissue density. Higher toughness per density was associated with long leaf lifespan especially in forest understory. Seldom appreciated in the past, toughness per density is a key factor in leaf mechanical resistance, which itself influences plant-animal interactions and ecosystem functions across the globe. C1 [Onoda, Yusuke; Westoby, Mark; Richards, Lora; Wright, Ian J.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Onoda, Yusuke] Kyushu Univ, Fac Sci, Dept Biol, Fukuoka 8128581, Japan. [Adler, Peter B.] Utah State Univ, Dept Wildland Resources, Logan, UT 84322 USA. [Choong, Amy M. F.] Republ Polytech, Singapore, Singapore. [Clissold, Fiona J.; McArthur, Clare] Univ Sydney, Sch Biol Sci, Sydney, NSW 2006, Australia. [Cornelissen, Johannes H. C.] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. [Diaz, Sandra; Enrico, Lucas; Perez-Harguindeguy, Natalia] Univ Nacl Cordoba, Inst Multidisciplinario Biol Vegetal, RA-5000 Cordoba, Argentina. [Diaz, Sandra; Enrico, Lucas; Perez-Harguindeguy, Natalia] Univ Nacl Cordoba, FCEFyN, CONICET, RA-5000 Cordoba, Argentina. [Dominy, Nathaniel J.] Dartmouth Coll, Dept Anthropol, Hanover, NH 03755 USA. [Elgart, Alison] Florida Gulf Coast Univ, Ft Myers, FL 33965 USA. [Fine, Paul V. A.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Howard, Jerome J.] Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA. [Jalili, Adel] Res Inst Forests & Rangelands, Dept Bot, Tehran, Iran. [Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL USA. [Kurokawa, Hiroko] Tohoku Univ, Grad Sch Life Sci, Sendai, Miyagi 9808578, Japan. [Lucas, Peter W.] Kuwait Univ, Fac Dent, Dept Bioclin Sci, Safat 13110, Kuwait. [Markesteijn, Lars; Poorter, Lourens] Wageningen Univ, Ctr Ecosyst Studies, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Poorter, Lourens] Wageningen Univ, Ctr Ecosyst Studies, Resource Ecol Grp, NL-6700 AA Wageningen, Netherlands. [Santiago, Louis S.] Univ Calif Riverside, Riverside, CA 92521 USA. [Sosinski, Enio E., Jr.] EMBRAPA Temperate Agr, BR-96010971 Pelotas, RS, Brazil. [Van Bael, Sunshine A.; Wright, S. Joseph] Smithsonian Trop Res Inst, Ancon, Panama. [Warton, David I.] Univ New S Wales, Sch Math & Stat, Sydney, NSW, Australia. [Warton, David I.] Univ New S Wales, Evolut & Ecol Res Ctr, Sydney, NSW, Australia. [Yamashita, Nayuta] Univ So Calif, Dept Anthropol, Los Angeles, CA 90089 USA. RP Onoda, Y (reprint author), Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. EM yusuke.onoda@gmail.com RI Adler, Peter/D-3781-2009; McArthur, Clare/A-3637-2011; Kitajima, Kaoru/E-8877-2012; Choong, Amy/J-4492-2012; Wright, Ian/G-4979-2012; Wright, Stuart/M-3311-2013; Onoda, Yusuke/L-7179-2015; Santiago, Louis/E-3185-2016; U-ID, Kyushu/C-5291-2016; Warton, David/B-5791-2009; OI Fine, Paul/0000-0002-0550-5628; McArthur, Clare/0000-0002-7867-414X; Wright, Ian/0000-0001-8338-9143; Wright, Stuart/0000-0003-4260-5676; Onoda, Yusuke/0000-0001-6245-2342; Santiago, Louis/0000-0001-5994-6122; Warton, David/0000-0001-9441-6645; Dominy, Nathaniel/0000-0001-5916-418X NR 85 TC 125 Z9 132 U1 22 U2 220 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD MAR PY 2011 VL 14 IS 3 BP 301 EP 312 DI 10.1111/j.1461-0248.2010.01582.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 723SZ UT WOS:000287528600013 PM 21265976 ER PT J AU Mumby, PJ Iglesias-Prieto, R Hooten, AJ Sale, PF Hoegh-Guldberg, O Edwards, AJ Harvell, CD Gomez, ED Knowlton, N Hatziolos, ME Kyewalyanga, MS Muthiga, N AF Mumby, Peter J. Iglesias-Prieto, Roberto Hooten, Anthony J. Sale, Peter F. Hoegh-Guldberg, Ove Edwards, Alasdair J. Harvell, C. Drew Gomez, Edgardo D. Knowlton, Nancy Hatziolos, Marea E. Kyewalyanga, Margareth S. Muthiga, Nyawira TI Revisiting climate thresholds and ecosystem collapse SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Letter ID CORAL-REEFS C1 [Mumby, Peter J.; Hoegh-Guldberg, Ove] Univ Queensland, Brisbane, Qld 4072, Australia. [Iglesias-Prieto, Roberto] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. [Edwards, Alasdair J.] Newcastle Univ, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Harvell, C. Drew] Cornell Univ, Ithaca, NY 14853 USA. [Gomez, Edgardo D.] Univ Philippines, Quezon City 1101, Philippines. [Knowlton, Nancy] Smithsonian Inst, Washington, DC 20560 USA. [Hatziolos, Marea E.] World Bank, Washington, DC USA. [Kyewalyanga, Margareth S.] Univ Dar Es Salaam, Dar Es Salaam, Tanzania. RP Mumby, PJ (reprint author), Univ Queensland, Brisbane, Qld 4072, Australia. EM p.j.mumby@uq.edu.au RI Mumby, Peter/F-9914-2010; Hoegh-Guldberg, Ove/H-6169-2011; Edwards, Alasdair/C-9558-2009 OI Hoegh-Guldberg, Ove/0000-0001-7510-6713; Edwards, Alasdair/0000-0002-2979-7389 NR 4 TC 15 Z9 15 U1 2 U2 18 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD MAR PY 2011 VL 9 IS 2 BP 94 EP 96 DI 10.1890/11.WB.002 PG 3 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 730TS UT WOS:000288058100012 ER PT J AU Brantley, SL Megonigal, JP Scatena, FN Balogh-Brunstad, Z Barnes, RT Bruns, MA Van Cappellen, P Dontsova, K Hartnett, HE Hartshorn, AS Heimsath, A Herndon, E Jin, L Keller, CK Leake, JR McDowell, WH Meinzer, FC Mozdzer, TJ Petsch, S Pett-Ridge, J Pregitzer, KS Raymond, PA Riebe, CS Shumaker, K Sutton-Grier, A Walter, R Yoo, K AF Brantley, S. L. Megonigal, J. P. Scatena, F. N. Balogh-Brunstad, Z. Barnes, R. T. Bruns, M. A. Van Cappellen, P. Dontsova, K. Hartnett, H. E. Hartshorn, A. S. Heimsath, A. Herndon, E. Jin, L. Keller, C. K. Leake, J. R. McDowell, W. H. Meinzer, F. C. Mozdzer, T. J. Petsch, S. Pett-Ridge, J. Pregitzer, K. S. Raymond, P. A. Riebe, C. S. Shumaker, K. Sutton-Grier, A. Walter, R. Yoo, K. TI Twelve testable hypotheses on the geobiology of weathering SO GEOBIOLOGY LA English DT Review ID DISSOLVED ORGANIC-CARBON; ELEVATED ATMOSPHERIC CO2; SOIL CARBON; UNITED-STATES; TERRESTRIAL ECOSYSTEMS; PHOSPHORUS LIMITATION; CLIMATE-CHANGE; LAND-USE; HYDRAULIC REDISTRIBUTION; MARINE-PHYTOPLANKTON AB Critical Zone (CZ) research investigates the chemical, physical, and biological processes that modulate the Earth's surface. Here, we advance 12 hypotheses that must be tested to improve our understanding of the CZ: (1) Solar-to-chemical conversion of energy by plants regulates flows of carbon, water, and nutrients through plant-microbe soil networks, thereby controlling the location and extent of biological weathering. (2) Biological stoichiometry drives changes in mineral stoichiometry and distribution through weathering. (3) On landscapes experiencing little erosion, biology drives weathering during initial succession, whereas weathering drives biology over the long term.(4) In eroding landscapes, weathering-front advance at depth is coupled to surface denudation via biotic processes.(5) Biology shapes the topography of the Critical Zone.(6) The impact of climate forcing on denudation rates in natural systems can be predicted from models incorporating biogeochemical reaction rates and geomorphological transport laws.(7) Rising global temperatures will increase carbon losses from the Critical Zone.(8) Rising atmospheric P-CO2 will increase rates and extents of mineral weathering in soils.(9) Riverine solute fluxes will respond to changes in climate primarily due to changes in water fluxes and secondarily through changes in biologically mediated weathering.(10) Land use change will impact Critical Zone processes and exports more than climate change. (11) In many severely altered settings, restoration of hydrological processes is possible in decades or less, whereas restoration of biodiversity and biogeochemical processes requires longer timescales.(12) Biogeochemical properties impart thresholds or tipping points beyond which rapid and irreversible losses of ecosystem health, function, and services can occur. C1 [Brantley, S. L.; Herndon, E.; Jin, L.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [Megonigal, J. P.; Mozdzer, T. J.; Sutton-Grier, A.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Scatena, F. N.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Balogh-Brunstad, Z.] Hartwick Coll, Dept Geol Environm Sci & Chem, Oneonta, NY 13820 USA. [Barnes, R. T.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Bruns, M. A.] Penn State Univ, Dept Crop & Soil Sci, University Pk, PA 16802 USA. [Van Cappellen, P.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Dontsova, K.] Univ Arizona, Tucson, AZ USA. [Hartnett, H. E.; Heimsath, A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Hartnett, H. E.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ USA. [Hartshorn, A. S.] James Madison Univ, Dept Geol & Environm Sci, Harrisonburg, VA 22807 USA. [Keller, C. K.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. [Leake, J. R.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [McDowell, W. H.] Univ New Hampshire, Dept Nat Resources & Environm, Durham, NH 03824 USA. [Meinzer, F. C.] US Forest Serv, USDA, Pacific NW Res Stn, Corvallis, OR USA. [Petsch, S.] Univ Massachusetts, Dept Geosci, Amherst, MA 01003 USA. [Pett-Ridge, J.] Oregon State Univ, Dept Crop & Soil Sci, Corvallis, OR 97331 USA. [Pregitzer, K. S.] Univ Idaho, Coll Nat Resources, Moscow, ID 83843 USA. [Raymond, P. A.] Yale Univ, Yale Sch Forestry & Environm Studies, New Haven, CT USA. [Riebe, C. S.] Univ Wyoming, Dept Geol & Geophys, Laramie, WY 82071 USA. [Shumaker, K.] Univ W Alabama, Coll Nat Sci & Math, Livingston, AL USA. [Shumaker, K.] Univ W Alabama, Dept Biol & Environm Sci, Livingston, AL USA. [Walter, R.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17604 USA. [Yoo, K.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. RP Brantley, SL (reprint author), Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. EM brantley@eesi.psu.edu RI Raymond, Peter/C-4087-2009; Meinzer, Frederick/C-3496-2012; McDowell, William/E-9767-2010; Barnes, Rebecca/A-2659-2011; Mozdzer, Thomas/G-4372-2011; Keller, C/B-3205-2012; Riebe, Clifford/B-7670-2012; Pett-Ridge, Julie/G-5842-2012; Van Cappellen, Philippe/A-2906-2013; Mozdzer, Thomas/A-3599-2014; OI Raymond, Peter/0000-0002-8564-7860; McDowell, William/0000-0002-8739-9047; Leake, Jonathan/0000-0001-8364-7616; Barnes, Rebecca/0000-0001-6385-1062; Van Cappellen, Philippe/0000-0001-5476-0820; Mozdzer, Thomas/0000-0002-1053-0967; Hartshorn, Anthony/0000-0002-0004-5749; Sutton-Grier, Ariana/0000-0002-1242-7728 FU NSF [EAR-0946877] FX Funding from NSF EAR-0946877 is acknowledged. We also acknowledge the following people for contributions to the workshop, 'Frontiers in Exploration of the Critical Zone II: The Geobiology of Weathering and Erosion', held 5-7 October 2009, at the Smithsonian Institution National Museum of Natural History: R. Amundson, T. Anderson, E. Barrera, T. Crowl, R. Cuenca, R. Davis, P. Glynn, K. Maher, D. McKnight, C. Monger, L. Patino, M. Pavich, C. Pilcher, E. Sztein, and N. Woodward. Special thanks to C. Samper, T. Anderson, and T. Karl of the Smithsonian Institution National Museum of Natural History. M. Hopkins, D. Lambert, and T. Bernier are acknowledged for organization and editing. L. Sanford and T. Cronin are acknowledged for help with Fig. 10. T. White is acknowledged for information concerning paleosols and C. Paola for the term, 'Earthcasting'. C. Anderson is acknowledged for help with figures. The manuscript benefitted from three helpful reviews and editorial handling by D. Beerling and K. Konhauser. NR 228 TC 48 Z9 48 U1 12 U2 173 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1472-4677 EI 1472-4669 J9 GEOBIOLOGY JI Geobiology PD MAR PY 2011 VL 9 IS 2 BP 140 EP 165 DI 10.1111/j.1472-4669.2010.00264.x PG 26 WC Biology; Environmental Sciences; Geosciences, Multidisciplinary SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Geology GA 719VW UT WOS:000287240600005 PM 21231992 ER PT J AU Scherer, JC AF Scherer, Joanna Cohan TI Life at the Kiowa, Comanche, and Wichita Agency: The Photographs of Annette Ross Hume SO GREAT PLAINS QUARTERLY LA English DT Book Review C1 [Scherer, Joanna Cohan] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Scherer, JC (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CENT GREAT PLAINS STUD PI LINCOLN PA UNIV NEBRASKA-LINCOLN 1214 OLDFATHER HALL, LINCOLN, NE 68588-0313 USA SN 0275-7664 J9 GREAT PLAINS QUART JI Gt. Plains Q. PD SPR PY 2011 VL 31 IS 2 BP 155 EP 155 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 766XD UT WOS:000290819000010 ER PT J AU Ortner, DJ AF Ortner, Donald J. TI Human skeletal paleopathology SO INTERNATIONAL JOURNAL OF PALEOPATHOLOGY LA English DT Editorial Material DE Paleopathology; Pathogenesis; Classification; Ancient disease AB Human skeletal remains from archaeological contexts are the main source of data about the complex interaction between disease and humankind throughout the emergence of Homo sapiens. Past and current research on these remains has revealed the presence of many diseases that affect the skeleton today. There are, however, limitations in using data from such skeletal samples to reconstruct the health of past human groups. Recently developed diagnostic procedures and methods for extracting relevant data from skeletal tissue provide new options for exploring important questions and trying to clarify the role of disease in the evolutionary process that resulted in human societies today. These past histories hold important lessons for predicting future relationships between our species and its disease load. Published by Elsevier Inc. C1 [Ortner, Donald J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Ortner, Donald J.] Univ Bradford, Dept Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. RP Ortner, DJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. EM Ortner@si.edu NR 76 TC 16 Z9 16 U1 1 U2 8 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1879-9817 EI 1879-9825 J9 INT J PALEOPATHOL JI Int. J. Paleopathol. PD MAR PY 2011 VL 1 IS 1 BP 4 EP 11 DI 10.1016/j.ijpp.2011.01.002 PG 8 WC Paleontology; Pathology SC Paleontology; Pathology GA V35IA UT WOS:000209142300002 ER PT J AU Santos-Granero, F AF Santos-Granero, Fernando TI THE VIRTUOUS MANIOC AND THE HORNY BARBASCO: SUBLIME AND GROTESQUE MODES OF TRANSFORMATION IN THE ORIGIN OF YANESHA PLANT LIFE SO JOURNAL OF ETHNOBIOLOGY LA English DT Article DE Yanesha; Amazonia; plant classification; plant domestication; indigenous cosmologies ID NORTHERN PERU; DOMESTICATION; AMAZON; HOLOCENE; AMERICA; FOREST; BRAZIL AB Like other native Amazonian peoples, the Yanesha of eastern Peru conceive of plants and trees as having been primordial human beings transformed into their present form at the end of mythic times. The events that led to their transformation can be described as being either "sublime" or "grotesque." Cultivated plants that underwent a sublime mode of transformation include manioc, the Yanesha staple, as well as maize, beans, peanuts, and cotton. These plants assumed their present form as the result of the self-transformation of powerful demiurges; a luminous, contained transformation that privileged the sensual capacities of the upper body. In contrast, the mode of transformation of barbasco, chili peppers, coca, peach palm, and yam falls on the side of the grotesque, and involves a series of immoral beings that had little control over the activities of their lower bodies. This article seeks to discern the Yanesha rationale behind this particular way of classifying plants. It proposes that sublime origin plants are those that were domesticated the earliest and have thus been part of Yanesha culture the longest. In contrast, those domesticated in more recent times - and thus less central to Yanesha cultural life-are attributed a more earthly, grotesque origin. C1 Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, MRC 0580-12,Unit 9100,Box 0948, Dpo, AA 34002 USA. EM santosf@si.edu NR 67 TC 2 Z9 2 U1 1 U2 3 PU SOC ETHNOBIOLOGY PI BOSTON PA UNIV MASSACHUSETTS BOSTON, DEPT ANTHROPOLOGY, 100 MORRISSEY BLVD, BOSTON, MA 02125 USA SN 0278-0771 J9 J ETHNOBIOL JI J. Ethnobiol. PD SPR-SUM PY 2011 VL 31 IS 1 BP 44 EP 71 DI 10.2993/0278-0771-31.1.44 PG 28 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 980PC UT WOS:000306904400003 ER PT J AU Taylor, RC Klein, BA Stein, J Ryan, MJ AF Taylor, Ryan C. Klein, Barrett A. Stein, Joey Ryan, Michael J. TI Multimodal signal variation in space and time: how important is matching a signal with its signaler? SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE anurans; mate choice; multimodal signaling; sexual selection; spatial variation; temporal synchrony; vocal sac ID TUNGARA FROG; MATE CHOICE; COURTSHIP DISPLAY; PHYSALAEMUS-PUSTULOSUS; COMMUNICATION SIGNALS; ACOUSTIC INTERFERENCE; ANIMAL COMMUNICATION; SEXUAL SELECTION; CALL COMPONENTS; VIDEO PLAYBACK AB Multimodal signals (acoustic+visual) are known to be used by many anuran amphibians during courtship displays. The relative degree to which each signal component influences female mate choice, however, remains poorly understood. In this study we used a robotic frog with an inflating vocal sac and acoustic playbacks to document responses of female tungara frogs to unimodal signal components (acoustic and visual). We then tested female responses to a synchronous multimodal signal. Finally, we tested the influence of spatial and temporal variation between signal components for female attraction. Females failed to approach the isolated visual cue of the robotic frog and they showed a significant preference for the call over the spatially separate robotic frog. When presented with a call that was temporally synchronous with the vocal sac inflation of the robotic frog, females did not show a significant preference for this over the call alone; when presented with a call that was temporally asynchronous with vocal sac inflation of the robotic frog, females discriminated strongly against the asynchronous multimodal signal in favor of the call alone. Our data suggest that although the visual cue is neither necessary nor sufficient for attraction, it can strongly modulate mate choice if females perceive a temporal disjunction relative to the primary acoustic signal. C1 [Taylor, Ryan C.] Salisbury Univ, Dept Biol Sci, Salisbury, MD 21801 USA. [Klein, Barrett A.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Stein, Joey] Moey Inc, Brooklyn, NY 11215 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. RP Taylor, RC (reprint author), Salisbury Univ, Dept Biol Sci, Salisbury, MD 21801 USA. EM rctaylor@salisbury.edu FU National Science Foundation [IBN 0517328] FX We thank Keri Athanas, Jessica Morris, and Karine Posbic for help in collecting data. Eileen Hebets and two anonymous reviewers provided valuable comments on an earlier version of the manuscript. The Smithsonian Tropical Research Institute provided logistical support. This work was supported by the National Science Foundation (IBN 0517328 to M.J.R. and R.C.T.). NR 48 TC 36 Z9 37 U1 3 U2 31 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 MAR PY 2011 VL 214 IS 5 BP 815 EP 820 DI 10.1242/jeb.043638 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 718NL UT WOS:000287130200022 PM 21307068 ER PT J AU Ferraro, J Henderson, J AF Ferraro, Jordan Henderson, Jane TI IDENTIFYING FEATURES OF EFFECTIVE EMERGENCY RESPONSE PLANS SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article AB Twelve emergency response planning manuals were reviewed to determine the characteristics of effective emergency response plans. Emergency plans were categorized as threat response plans and management response plans, depending on their content and structure. Primary characteristics of each type are discussed using five case studies. Based on the distinctions, strengths, and weaknesses of each type of plan, recommendations are made to aid institutions in selecting the most appropriate approach. C1 [Ferraro, Jordan] Smithsonian Inst, Natl Air & Space Museum, Arch Div, Washington, DC 20013 USA. [Henderson, Jane] Cardiff Univ, Sch Hist & Archaeol & Relig, Cardiff CF10 3EU, S Glam, Wales. RP Ferraro, J (reprint author), Smithsonian Inst, Natl Air & Space Museum, Arch Div, POB 37012,Rm 3100 MRC 322, Washington, DC 20013 USA. EM jbferraro@gmail.com; HendersonLJ@cardiff.ac.uk NR 43 TC 0 Z9 0 U1 0 U2 2 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SPR-SUM PY 2011 VL 50 IS 1 BP 35 EP 48 PG 14 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V29YL UT WOS:000208783600003 ER PT J AU Krzywinski, J Li, C Morris, M Conn, JE Lima, JB Povoa, MM Wilkerson, RC AF Krzywinski, Jaroslaw Li, Cong Morris, Marion Conn, Jan E. Lima, Jose B. Povoa, Marinete M. Wilkerson, Richard C. TI Analysis of the evolutionary forces shaping mitochondrial genomes of a Neotropical malaria vector complex SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Comparative genomics; Mitochondrial genome evolution; Replication origin; Introgressive hybridization; Malaria vectors ID POLYMERASE-CHAIN-REACTION; NYSSORHYNCHUS ALBITARSIS DIPTERA; ANOPHELES-GAMBIAE; GENE-SEQUENCES; PHYLOGENETIC-RELATIONSHIPS; REACTION IDENTIFICATION; MOLECULAR PHYLOGENY; CULICIDAE COMPLEX; DNA-SEQUENCE; INTROGRESSION AB Many vectors of human malaria belong to complexes of morphologically indistinguishable cryptic species. Here we report the analysis of the newly sequenced complete mitochondrial DNA molecules from six recognized or putative species of one such group, the Neotropical Anopheles albitarsis complex. The molecular evolution of these genomes had been driven by purifying selection, particularly strongly acting on the RNA genes. Directional mutation pressure associated with the strand-asynchronous asymmetric mtDNA replication mechanism may have shaped a pronounced DNA strand asymmetry in the nucleotide composition in these and other Anopheles species. The distribution of sequence polymorphism, coupled with the conflicting phylogenetic trees inferred from the mitochondrial DNA and from the published white gene fragment sequences, indicates that the evolution of the complex may have involved ancient mtDNA introgression. Six protein coding genes (nad5, nad4, cox3, atp6, cox1 and nad2) have high levels of sequence divergence and are likely informative for population genetics studies. Finally, the extent of the mitochondrial DNA variation within the complex supports the notion that the complex consists of a larger number of species than until recently believed. (C) 2011 Elsevier Inc. All rights reserved. C1 [Krzywinski, Jaroslaw; Morris, Marion] Univ Liverpool, Liverpool Sch Trop Med, Vector Grp, Liverpool L3 5QA, Merseyside, England. [Li, Cong; Wilkerson, Richard C.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA. [Li, Cong; Wilkerson, Richard C.] Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, WRAIR,MRC 534, Suitland, MD 20746 USA. [Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Slingerlands, NY 12159 USA. [Conn, Jan E.] SUNY Albany, Sch Publ Hlth, Dept Biomed Sci, Albany, NY 12201 USA. [Lima, Jose B.] Fundacao Oswaldo Cruz, Dept Entomol, Rio De Janeiro, Brazil. [Povoa, Marinete M.] Inst Evandro Chagas, Secao Parasitol, Lab Malaria, BR-67030000 Ananindeua, PA, Brazil. RP Krzywinski, J (reprint author), Univ Liverpool, Liverpool Sch Trop Med, Vector Grp, Liverpool L3 5QA, Merseyside, England. EM jarek@liv.ac.uk OI Conn, Jan/0000-0002-5301-7020 FU National Institutes of Health (USA) [2R01AI54139]; Liverpool School of Tropical Medicine FX We are grateful to Martin Donnelly for a constructive discussion on the issue of potential introgression. Comments and suggestions made by two anonymous reviewers and Stephen Cameron improved the shape of the manuscript. We thank John F. Ruiz for providing the An. albitarsis G white gene sequence for the current analysis. We also thank Laboratorio de Pesquisas Basicas at Instituto Evandro Chagas, Belem, Para state, Brazil for logistical support in the field. This study was funded by National Institutes of Health (USA) Grant 2R01AI54139 to JEC and by start-up funds from the Liverpool School of Tropical Medicine to JK. Material has been reviewed by the Walter Reed Army Institute of Research. There is no objection to its presentation and/or publication. The opinions or assertions contained herein are the private views of the author, and are not to be construed as official, or as reflecting true views of the Department of the Army or the Department of Defense. Parts of this research were performed at the Smithsonian Institution under a Memorandum of Understanding between the Walter Reed Army Institute of Research and the Smithsonian Institution, with institutional support provided by both organizations. NR 68 TC 24 Z9 24 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2011 VL 58 IS 3 BP 469 EP 477 DI 10.1016/j.ympev.2011.01.003 PG 9 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 731ZX UT WOS:000288151000006 PM 21241811 ER PT J AU Narayanan, D Cox, TJ Hayward, CC Hernquist, L AF Narayanan, Desika Cox, Thomas J. Hayward, Christopher C. Hernquist, Lars TI The Kennicutt-Schmidt star formation relation at z similar to 2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: molecules; galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies: starburst; galaxies: star formation; cosmology: theory ID ULTRALUMINOUS INFRARED GALAXIES; REDSHIFT SUBMILLIMETER GALAXIES; GIANT MOLECULAR CLOUDS; AEGIS FIELD GALAXIES; DENSE GAS RELATION; FORMING GALAXIES; RADIATIVE-TRANSFER; NEARBY GALAXIES; FORMATION EFFICIENCY; INTERSTELLAR CLOUDS AB Recent observations of excited CO emission lines from z similar to 2 disc galaxies have shed light on the SFR proportional to N relation at high z via observed Sigma(SFR)-Sigma alpha(COJ=2-1) and Sigma(SFR)-Sigma alpha(COJ=3-2) relations. Here, we describe a novel methodology for utilizing these observations of high-excitation CO to derive the underlying Schmidt (SFR proportional to N) relationship. To do this requires an understanding of the potential effects of differential CO excitation with SFR. If the most heavily star-forming galaxies have a larger fraction of their gas in highly excited CO states than the lower SFR galaxies, then the observed molecular Kennicutt-Schmidt index, alpha, will be less than the underlying SFR proportional to N index, N. Utilizing a combination of SPH models of galaxy evolution and molecular line radiative transfer, we present the first calculations of CO excitation in z similar to 2 disc galaxies with the aim of developing a mapping between various observed Sigma(SFR)-Sigma alpha(CO) relationships and the underlying SFR proportional to N relation. We find that even in relatively luminous z similar to 2 discs, differential excitation does indeed exist, resulting in alpha < N for highly excited CO lines. This means that an observed (e.g.) Sigma(SFR)-Sigma alpha(COJ=3-2) relation does not map linearly to a Sigma(SFR)-Sigma alpha(H2) relation. We utilize our model results to provide a mapping from alpha to N for the range of Schmidt indices N = 1-2. By comparing to recent observational surveys, we find that the observed and Sigma(SFR)-Sigma alpha(COJ=3-2) relations suggest that an underlying SFR proportional to 1.5 relation describes z similar to 2 disc galaxies. C1 [Narayanan, Desika; Hayward, Christopher C.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cox, Thomas J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Narayanan, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dnarayanan@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU Harvard FAS Research Computing Group FX We thank Shane Bussmann, Neal Evans, Reinhard Genzel, Patrik Jonsson, Dusan Keres, Mark Krumholz, Charlie Lada, Kai Noeske, Alice Shapley, Amiel Sternberg and Linda Tacconi for enjoyable conversations as the ideas for this study were developed. The simulations in this paper were run on the Odyssey cluster, supported by the Harvard FAS Research Computing Group. NR 79 TC 19 Z9 19 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2011 VL 412 IS 1 BP 287 EP 294 DI 10.1111/j.1365-2966.2010.17903.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 734YC UT WOS:000288378100025 ER PT J AU Madej, OK Jonker, PG AF Madej, O. K. Jonker, P. G. TI Discovery of a broad O VIII Ly alpha line in the ultracompact X-ray binary 4U 1543-624 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; X-rays: binaries; X-rays: individual: 4U 1543-624 AB We report the discovery of a broad emission feature at similar to 0.7 keV in the spectra of the ultra-compact X-ray binary 4U 1543-624, obtained with the high-resolution spectrographs of the XMM-Newton and Chandra satellites. We confirm the presence of the feature in the broadband MOS2 spectrum of the source. As suggested before in the literature, the donor star in this source is a CO or ONe white dwarf, which transfers oxygen-rich material to the accretor, conceivably a neutron star. The X-rays reprocessed in this oxygen-rich accretion disc could give a reflection spectrum with O VIII Ly alpha as the most prominent emission line. Apart from the feature at similar to 0.7 keV, we confirm the possible presence of a weak emission feature at similar to 6.6 keV, which was reported in the literature for this data set. We interpret the feature at similar to 0.7 and similar to 6.6 keV as O VIII Ly alpha and Fe K alpha emission, respectively, caused by X-rays reflected off the accretion disc in the strong gravitational field close to the accretor. C1 [Madej, O. K.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. [Madej, O. K.; Jonker, P. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, NL-6500 HC Nijmegen, Netherlands. RP Madej, OK (reprint author), Univ Utrecht, Astron Inst, POB 80000, NL-3508 TA Utrecht, Netherlands. EM O.Madej@sron.nl FU VIDI grant from the Netherlands Organization for Scientific Research FX We thank Frank Verbunt and the referee for useful comments. PGJ acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research. NR 14 TC 10 Z9 10 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2011 VL 412 IS 1 BP L11 EP L15 DI 10.1111/j.1745-3933.2010.00989.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V41JY UT WOS:000209543700003 ER PT J AU Shternin, PS Yakovlev, DG Heinke, CO Ho, WCG Patnaude, DJ AF Shternin, Peter S. Yakovlev, Dmitry G. Heinke, Craig O. Ho, Wynn C. G. Patnaude, Daniel J. TI Cooling neutron star in the Cassiopeia A supernova remnant: evidence for superfluidity in the core SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dense matter; equation of state; neutrinos; stars: neutron; supernovae: individual: Cassiopeia A; X-rays: stars AB According to recent results of Ho & Heinke, the Cassiopeia A supernova remnant contains a young (approximate to 330-yr-old) neutron star (NS) which has carbon atmosphere and shows notable decline of the effective surface temperature. We report a new (2010 November) Chandra observation which confirms the previously reported decline rate. The decline is naturally explained if neutrons have recently become superfluid (in triplet state) in the NS core, producing a splash of neutrino emission due to Cooper pair formation (CPF) process that currently accelerates the cooling. This scenario puts stringent constraints on poorly known properties of NS cores: on density dependence of the temperature T-cn(rho) for the onset of neutron superfluidity [T-cn(rho) should have a wide peak with maximum approximate to (7-9) x 10(8) K]; on the reduction factor q of CPF process by collective effects in superfluid matter (q > 0.4) and on the intensity of neutrino emission before the onset of neutron superfluidity (30-100 times weaker than the standard modified Urca process). This is serious evidence for nucleon superfluidity in NS cores that comes from observations of cooling NSs. C1 [Shternin, Peter S.; Yakovlev, Dmitry G.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Shternin, Peter S.] St Petersburg State Polytech Univ, St Petersburg 195251, Russia. [Heinke, Craig O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Ho, Wynn C. G.] Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. [Patnaude, Daniel J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Shternin, PS (reprint author), AF Ioffe Phys Tech Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia. EM pshternin@gmail.com; wynnho@slac.stanford.edu RI Shternin, Peter/A-7352-2014; OI Heinke, Craig/0000-0003-3944-6109 FU Rosnauka [NSh 3769.2010.2]; Ministry of Education and Science of Russian Federation [11.G34.31.0001]; Science and Technology Facilities Council (STFC) in the United Kingdom [PP/E001025/1]; Dynasty Foundation; RF Presidential Programme [MK-5857.2010.2]; Natural Sciences and Engineering Research Council (NSERC) of Canada; SPbSPU FX We are grateful to A. Y. Potekhin for critical remarks. PSS and DGY acknowledge support from Rosnauka (grant NSh 3769.2010.2) and the Ministry of Education and Science of Russian Federation (contract 11.G34.31.0001 with SPbSPU and Leading Scientist G. G. Pavlov). WCGH acknowledges support from the Science and Technology Facilities Council (STFC) in the United Kingdom through grant no. PP/E001025/1. PSS acknowledges support of the Dynasty Foundation and RF Presidential Programme MK-5857.2010.2. COH acknowledges support from the Natural Sciences and Engineering Research Council (NSERC) of Canada. NR 40 TC 150 Z9 150 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2011 VL 412 IS 1 BP L108 EP L112 DI 10.1111/j.1745-3933.2011.01015.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V41JY UT WOS:000209543700023 ER PT J AU Kocsis, B Sesana, A AF Kocsis, B. Sesana, A. TI Gas-driven massive black hole binaries: signatures in the nHz gravitational wave background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; gravitational waves; planet-disc interactions; pulsars: general; cosmology: theory ID ACTIVE GALACTIC NUCLEI; PULSAR TIMING ARRAYS; GALAXY FORMATION; ACCRETION DISKS; HORSESHOE DRAG; MERGERS; DISCS; EVOLUTION; COROTATION; RADIATION AB Pulsar timing arrays (PTAs) measure nHz frequency gravitational waves (GWs) generated by orbiting massive black hole binaries (MBHBs) with periods between 0.1 and 10 yr. Previous studies on the nHz GW background assumed that the inspiral is purely driven by GWs. However, torques generated by a gaseous disc can shrink the binary much more efficiently than GW emission, reducing the number of binaries at these separations. We use simple disc models for the circumbinary gas and for the binary-disc interaction to follow the orbital decay of MBHBs through physically distinct regions of the disc, until GWs take over their evolution. We extract MBHB cosmological merger rates from the Millennium simulation, generate Monte Carlo realizations of a population of gas-driven binaries and calculate the corresponding GW amplitudes of the most luminous individual binaries and the stochastic GW background. For steady state alpha-discs witha alpha > 0.1, we find that the nHz GW background can be significantly modified. The number of resolvable binaries is however not changed by the presence of gas; we predict 1-10 individually resolvable sources to stand above the noise for a 1-50 ns timing precision. Gas-driven migration reduces predominantly the number of small total mass or unequal mass ratio binaries, which leads to the attenuation of the mean stochastic GW background, but increases the detection significance of individually resolvable binaries. The results are sensitive to the model of binary-disc interaction. The GW background is not attenuated significantly for time-dependent models of Ivanov, Papaloizou & Polnarev. C1 [Kocsis, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kocsis, B.] Inst Adv Study, Princeton, NJ 08540 USA. [Kocsis, B.] Eotvos Lorand Univ, H-1117 Budapest, Hungary. [Sesana, A.] Albert Einstein Inst, D-14476 Golm, Germany. [Sesana, A.] Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA. RP Kocsis, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bkocsis@cfa.harvard.edu; alberto.sesana@aei.mpg.de RI Kocsis, Bence/C-3061-2013; Sesana, Alberto/Q-9826-2016 OI Kocsis, Bence/0000-0002-4865-7517; Sesana, Alberto/0000-0003-4961-1606 FU Chandra X-ray Center [PF9-00063]; NASA [NAS8-03060]; OTKA [68228] FX AS is grateful to M. 'penguin' Giustini and V. Cappa for enlightening discussions. BK acknowledges support by NASA through Einstein Postdoctoral Fellowship grant no. PF9-00063 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060, and partial support by OTKA grant 68228. NR 63 TC 39 Z9 39 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2011 VL 411 IS 3 BP 1467 EP 1479 DI 10.1111/j.1365-2966.2010.17782.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 723DL UT WOS:000287486400006 ER PT J AU Li, HB Blundell, R Hedden, A Kawamura, J Paine, S Tong, E AF Li, Hua-bai Blundell, Raymond Hedden, Abigail Kawamura, Jonathan Paine, Scott Tong, Edward TI Evidence for dynamically important magnetic fields in molecular clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE MHD; turbulence; stars: formation; ISM: clouds; ISM: kinematics and dynamics; ISM: magnetic fields ID TURBULENT AMBIPOLAR DIFFUSION; OH ZEEMAN OBSERVATIONS; STAR-FORMATION; MAGNETOHYDRODYNAMIC TURBULENCE; DARK CLOUD; INTERSTELLAR TURBULENCE; ALFVENIC TURBULENCE; IONIZED-GAS; ION SPECTRA; CORES AB Recent observational evidence that magnetic fields are dynamically important in molecular clouds, compared to self-gravity and turbulence, is reviewed and illustrated with data from the NGC 2024 region. One piece of evidence, turbulence anisotropy, was found in the diffuse envelope of a cloud (A(v) approximate to 1; Heyer et al. 2008); our data further suggest turbulence anisotropy in the cloud (A(v) > 7) and even near the cloud core (A(v) similar to 100). The data also show that magnetic fields can channel gravitational contraction even for a region with supercritical N(H-2)/2B(los) ratio (the ratio between the observed column density and two times the line-of-sight observed field strength), a parameter which has been widely used by observers to estimate core mass-to-flux ratios. Although the mass-to-flux ratio is constant under the flux-freezing condition, we show that N(H-2)/2B(los) grows with time if gravitational contraction is anisotropic due to magnetic fields. C1 [Li, Hua-bai] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Blundell, Raymond; Hedden, Abigail; Paine, Scott; Tong, Edward] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kawamura, Jonathan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Li, HB (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM li@mpia.de OI Paine, Scott/0000-0003-4622-5857 FU Harvard-Smithsonian Center for Astrophysics; Smithsonian Institution; National Aeronautics and Space Administration; Academia Sinica FX Our deepest appreciation goes to the staff of the SAO Submillimetre Receiver Lab: Robert Kimberk, Steven Leiker, Cosmo Papa, Patricia Riddle and Michael Smith. We are grateful for the support of RLT observations from Jorge May, Leo Bronfman, Claudio Barrientos, Marcos Diaz, Jose Donoso, Daniel Luhr, Walter Max-Moerbeck, Daniel Marrone and Kevin Rauch. We thank Zhi-Yun Li, Matthew Kunz and the referee for many insightful comments. H-bL's research is supported by the post-doctoral fellowships from Max-Planck-Institut fur Astronomie and from Harvard-Smithsonian Center for Astrophysics. The RLT was supported in part by Smithsonian Institution internal research and development funds. Part of the RLT research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Operation of the RLT on Sairecabur has been carried out in collaboration with the Universidad de Chile. The Submillimetre Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 68 TC 12 Z9 12 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2011 VL 411 IS 3 BP 2067 EP 2075 DI 10.1111/j.1365-2966.2010.17839.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 723DL UT WOS:000287486400056 ER PT J AU Johnson, EI Stouffer, PC Vargas, CF AF Johnson, Erik I. Stouffer, Philip C. Vargas, Claudeir F. TI Diversity, biomass, and trophic structure of a central amazonian rainforest bird community SO REVISTA BRASILEIRA DE ORNITOLOGIA LA English DT Article DE Amazonia; bird communities; biomass; species richness; rainforest ID SPECIES RICHNESS; GEOGRAPHIC-VARIATION; BRAZILIAN AMAZONIA; NEOTROPICAL BIRDS; SECONDARY FORESTS; SEED DISPERSAL; TERRITORY SIZE; ECOLOGY; BIOGEOGRAPHY; ABUNDANCE AB Amazonian forest bird communities are among the richest in the world. Even so, relatively little is known about the organization of the entire avian community at local scales or about differences across Amazonia. These are fundamental data not only for understanding the processes generating and maintaining tropical diversity, but also as a baseline for evaluating anthropogenic changes to Amazonian forests. Here we provide a description of the entire bird community for a 100 ha plot of terra firme forest at the Biological Dynamics of Forest Fragments Project, near Manaus, Brazil, based on spot-map and mist net surveys augmented by additional field and analytical techniques. Although our results are from a single plot surveyed in a single year, our methods and interpretation reflect nearly 30 years of ornithological research at the site. We found 228 species on the plot, of which 207 were considered part of the core regional avifauna. Median density was five individuals/100 ha. Only 13 species (6% of the core species) had densities >= 20 individuals on the plot, although 55 species (27%) had <= 2 individuals. No species had territories smaller than 3 ha; median territory size was 11 ha for the 103 species for which we could make reasonable estimates. Measured by numbers of species or individuals, the plot was dominated by insectivores (54% of species, 62% of individuals). Biomass, however, was dominated by frugivores and granivores (59%). Compared to available data from other Amazonian forests, our site appears to have comparable richness of a similar set of species, but lower density and greater patchiness. Our results suggest that the area required to support populations of many species will be even greater in central Amazonia than in western Amazonia. C1 [Johnson, Erik I.; Stouffer, Philip C.] Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Johnson, Erik I.; Stouffer, Philip C.; Vargas, Claudeir F.] Inst Nacl de Pesquisas da Amazonia, Projeto Dinam Biol Fragmentos Florestais, BR-69060000 Manaus, AM, Brazil. [Johnson, Erik I.; Stouffer, Philip C.; Vargas, Claudeir F.] Smithsonian Trop Res Inst, BR-69060000 Manaus, AM, Brazil. RP Johnson, EI (reprint author), Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. EM pstouffer@lsu.edu FU Instituto Nacional de Pesquisas da Amazonia; Smithsonian Institution; US National Science Foundation [LTREB-0545491] FX We thank field assistants S. M. de Freitas and J. Lopes for their help in mist-netting and following birds. L. Powell provided valuable guidance with territory size analyses. M. Cohn-Haft, G. Ferraz, J. V. C. de Silva, and the staff of the Biological Dynamics of Forest Fragments Project (BDFFP) provided valuable logistical support throughout the project. Discussions with M. Brooks, F. Owens, M. Cohn-Haft, D. Robinson, and J. Terborgh greatly improved the quality of this manuscript. The BDFFP is managed and supported by the Instituto Nacional de Pesquisas da Amazonia and the Smithsonian Institution. Funding for the research was provided by US National Science Foundation grant LTREB-0545491. This is publication 571 of the BDFFP Technical Series and 20 of the Amazonian Ornithology Technical Series of the INPA Collections Program. The manuscript was approved by the Director of the Louisiana State University Agricultural Center as manuscript number 2011-241-5593. NR 72 TC 17 Z9 17 U1 8 U2 30 PU SOC BRASILEIRA ORNITOLOGIA PI VICOSA PA C/O ROMULO RIBON, MUSEU ZOOLOGIA JOAO MOOJEN, LADEIRA DOS OPERARIOS 54-204, VICOSA, MG 36570-000, BRAZIL SN 0103-5657 J9 REV BRAS ORNITOL JI Rev. Bras. Ornitol. PD MAR PY 2011 VL 19 IS 1 BP 1 EP 16 PG 16 WC Ornithology SC Zoology GA 956UP UT WOS:000305115000001 ER PT J AU Narukage, N Sakao, T Kano, R Hara, H Shimojo, M Bando, T Urayama, F DeLuca, E Golub, L Weber, M Grigis, P Cirtain, J Tsuneta, S AF Narukage, N. Sakao, T. Kano, R. Hara, H. Shimojo, M. Bando, T. Urayama, F. DeLuca, E. Golub, L. Weber, M. Grigis, P. Cirtain, J. Tsuneta, S. TI Coronal-Temperature-Diagnostic Capability of the Hinode/X-Ray Telescope Based on Self-Consistent Calibration SO SOLAR PHYSICS LA English DT Article DE Corona; Instrumentation and data management ID SOLAR-A MISSION; EXTREME-ULTRAVIOLET; ATOMIC DATABASE; EMISSION-LINES; ELEMENTS HYDROGEN; ACTIVE REGIONS; CHIANTI; YOHKOH; XRT; PERFORMANCE AB The X-Ray Telescope (XRT) onboard the Hinode satellite is an X-ray imager that observes the solar corona with unprecedentedly high angular resolution (consistent with its 1 '' pixel size). XRT has nine X-ray analysis filters with different temperature responses. One of the most significant scientific features of this telescope is its capability of diagnosing coronal temperatures from less than 1 MK to more than 10 MK, which has never been accomplished before. To make full use of this capability, accurate calibration of the coronal temperature response of XRT is indispensable and is presented in this article. The effect of on-orbit contamination is also taken into account in the calibration. On the basis of our calibration results, we review the coronal-temperature-diagnostic capability of XRT. C1 [Narukage, N.; Kano, R.; Hara, H.; Bando, T.; Tsuneta, S.] Natl Astron Observ Japan NAOJ, Mitaka, Tokyo 1818588, Japan. [Sakao, T.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. [Shimojo, M.] Natl Astron Observ Japan, Nobeyama Solar Radio Observ, Minamisa Ku, Nagano 3841305, Japan. [Urayama, F.] Space Engn Dev Co Ltd, Tsukuba, Ibaraki 3050032, Japan. [DeLuca, E.; Golub, L.; Weber, M.; Grigis, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Cirtain, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Narukage, N (reprint author), Natl Astron Observ Japan NAOJ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM noriyuki.narukage@nao.ac.jp RI DeLuca, Edward/L-7534-2013; Shimojo, Masumi/J-2605-2016; OI DeLuca, Edward/0000-0001-7416-2895; Shimojo, Masumi/0000-0002-2350-3749; Golub, Leon/0000-0001-9638-3082 FU JAXA and NAOJ (Japan); STFC (UK); NASA; ESA; NSC (Norway) FX The authors thank the members of the XRT team for useful discussions and comments. We acknowledge D. Brooks and H. Warren for various pieces of information on quiet-Sun and active region DEMs. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA, ESA, and NSC (Norway). CHIANTI is a collaborative project involving the NRL (USA), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). We wish to express our sincere gratitude to the late Takeo Kosugi, former project manager of Hinode (Solar-B) at ISAS, who passed away in November 2006. Without his leadership in the development of Hinode, this mission would never have been realized. We express our sincere gratitude to those who participated in, or supported, the XRT end-to-end calibration measurement at MSFC XRCF that was carried out for two weeks in May June 2005. First of all, we are very much indebted loan extremely-talented team of people at XRCF led by C. Reily and J. McCracken, including R. Siler, E. Wright, J. Carpenter, J. Keegley and G. Zirnstein, and also M. Baker, H. Haight, B. Hale, T. Hill, B. Hoghe, D. Javins, J. Norwood, H. Rutledge, G. St. John, J. Tucker, and D. Watson. Without their continuous, enormous support including preparation of the LN2-cooled cold plate facing XRT radiators in the cryogenic chamber of XRCF, from an early preparation phase of the XRCF experiment and throughout the experiment's duration, the filter calibration at XRCF would have been totally impossible. We are also grateful to people from SAO who supported the XRCF measurement; G. Austin, W. Podgorski, E. Dennis, J. Chappel, D. Caldwell, W. Martell, M. Harris, M. Cosmo, D. Weaver, S. Park and T. Kent who participated in the experiment, and P. Cheimets, J. Bookbinder, J. Boczenowski. Also A. Sabbag of Naval Research Laboratory is appreciated for his support during a pre-shipment instrument check performed at SAO. K. Kumagai and M. Tamura of NAOJ, K. Yaji of Rikkyo U., and K. Kobayashi of MSFC are greatly appreciated for preparing, and participating in, the XRCF experiment. Also, people from MSFC, L. Hill, J. Owens, B. Cobb, D. Coleman, R. Jayroe, T. Perrin, D. Schultz, A. Sterling and C. Talley are sincerely acknowledged for their various supportive contributions throughout our stay in Huntsville and also for our transportation to and from XRCF. Finally, the authors are grateful to the referees for their detailed and careful reviews. NR 36 TC 42 Z9 42 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAR PY 2011 VL 269 IS 1 BP 169 EP 236 DI 10.1007/s11207-010-9685-2 PG 68 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 738FZ UT WOS:000288626700012 ER PT J AU Mello, MAR Marquitti, FMD Guimaraes, PR Kalko, EKV Jordano, P de Aguiar, MAM AF Ribeiro Mello, Marco Aurelio Darcie Marquitti, Flavia Maria Guimaraes, Paulo Roberto, Jr. Viktoria Kalko, Elisabeth Klara Jordano, Pedro Martinez de Aguiar, Marcus Aloizio TI The Missing Part of Seed Dispersal Networks: Structure and Robustness of Bat-Fruit Interactions SO PLOS ONE LA English DT Article ID ANIMAL MUTUALISTIC NETWORKS; CAROLLIA-PERSPICILLATA; POLLINATION NETWORKS; COMPLEX NETWORKS; FRUGIVOROUS BATS; ATLANTIC FOREST; NESTEDNESS; BIODIVERSITY; PHYLLOSTOMIDAE; SPECIALIZATION AB Mutualistic networks are crucial to the maintenance of ecosystem services. Unfortunately, what we know about seed dispersal networks is based only on bird-fruit interactions. Therefore, we aimed at filling part of this gap by investigating bat-fruit networks. It is known from population studies that: (i) some bat species depend more on fruits than others, and (ii) that some specialized frugivorous bats prefer particular plant genera. We tested whether those preferences affected the structure and robustness of the whole network and the functional roles of species. Nine bat-fruit datasets from the literature were analyzed and all networks showed lower complementary specialization (H-2' = 0.3760.10, mean 6 SD) and similar nestedness (NODF = 0.5660.12) than pollination networks. All networks were modular (M=0.32 +/- 0.07), and had on average four cohesive subgroups (modules) of tightly connected bats and plants. The composition of those modules followed the genus-genus associations observed at population level (Artibeus-Ficus, Carollia-Piper, and Sturnira-Solanum), although a few of those plant genera were dispersed also by other bats. Bat-fruit networks showed high robustness to simulated cumulative removals of both bats (R = 0.55 +/- 0.10) and plants (R = 0.68 +/- 0.09). Primary frugivores interacted with a larger proportion of the plants available and also occupied more central positions; furthermore, their extinction caused larger changes in network structure. We conclude that bat-fruit networks are highly cohesive and robust mutualistic systems, in which redundancy is high within modules, although modules are complementary to each other. Dietary specialization seems to be an important structuring factor that affects the topology, the guild structure and functional roles in bat-fruit networks. C1 [Ribeiro Mello, Marco Aurelio; Viktoria Kalko, Elisabeth Klara] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Darcie Marquitti, Flavia Maria] Univ Estadual Campinas, Programa Posgrad Ecol, Campinas, SP, Brazil. [Guimaraes, Paulo Roberto, Jr.] Univ Sao Paulo, Dept Ecol, Sao Paulo, Brazil. [Viktoria Kalko, Elisabeth Klara] Smithsonian Trop Res Inst, Balboa, Panama. [Jordano, Pedro] CSIC, Estn Biol Donana, E-41080 Seville, Spain. [Martinez de Aguiar, Marcus Aloizio] Univ Estadual Campinas, Inst Fis Gleb Wataghin, Campinas, SP, Brazil. RP Mello, MAR (reprint author), Univ Ulm, Inst Expt Ecol, Ulm, Germany. EM marmello@gmail.com RI Mello, Marco/B-1095-2008; de Aguiar, Marcus/C-9137-2012; CSIC, EBD Donana/C-4157-2011; Guimaraes, Paulo/B-1099-2008; Habe, Neusa/D-6316-2011; Jordano, Pedro/A-5162-2008; Darcie Marquitti, Flavia Maria/B-2697-2013; Guimaraes, Paulo/E-1915-2016; Guimaraes-Junior, Paulo/M-1298-2016; Inst. of Physics, Gleb Wataghin/A-9780-2017 OI Mello, Marco/0000-0002-9098-9427; de Aguiar, Marcus/0000-0003-1379-7568; CSIC, EBD Donana/0000-0003-4318-6602; Jordano, Pedro/0000-0003-2142-9116; Darcie Marquitti, Flavia Maria/0000-0003-0510-3992; FU Humboldt Foundation [1134644]; DFG; MEC; [2006/00265-0] FX Fapesp (http://www.fapesp.br) sponsored M. A. R. Mello (2006/00265-0), F. M. D. Marquitti, M. A. M. Aguiar, and P. R. Guimaraes. M. A. R. Mello was also supported (1134644) by the Humboldt Foundation (http://www.humboldt-foundation.de), E. K. V. Kalko by DFG (http://www.dfg.de), and P. Jordano by MEC (http://www.educacion.es/). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 56 TC 39 Z9 44 U1 2 U2 49 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 28 PY 2011 VL 6 IS 2 AR e17395 DI 10.1371/journal.pone.0017395 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 729EM UT WOS:000287931400069 PM 21386981 ER PT J AU Tafoya, D Imai, H Gomez, Y Torrelles, JM Patel, NA Anglada, G Miranda, LF Honma, M Hirota, T Miyaji, T AF Tafoya, Daniel Imai, Hiroshi Gomez, Yolanda Torrelles, Jose M. Patel, Nimesh A. Anglada, Guillem Miranda, Luis F. Honma, Mareki Hirota, Tomoya Miyaji, Takeshi TI Measurement of the Distance and Proper Motions of the H2O Masers in the Young Planetary Nebula K 3-35 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE ISM: planetary nebulae: individual (K 3-35); masers(H2O); stars: kinematics; stars: late-type; stars: winds, outflow ID EMISSION; PARALLAX; SCALE; KINEMATICS; VERA; STAR; K3-35; TORUS; VLBA; JET AB In this paper we present the results of very long baseline interferometry (VLBI) observations carried out with the VLBI Exploration of Radio Astrometry (VERA) array and the Very Long Baseline Array (VLBA) toward H2O masers in a young planetary nebula K 3-35. From the VERA observations we measured the annual parallax and proper motion of a bright water maser spot in K 3-35. The resulting distance is D = 3.9(-0.5)(+0.7) kpc. This is the first time that the parallax of a planetary nebula is obtained by observations of its maser emission. On the other hand, the proper motion of K 3-35 as a whole was estimated to mu(alpha) = -3.34 +/- 0.10 mas yr(-1), mu(delta) = -5.93 +/- 0.07 mas yr(-1). From these results we determined the position and velocity of K 3-35 in Galactic cylindrical coordinates: (R, theta, z) = (7.11(-0.06)(+0.08) kpc, 27 degrees +/- 5 degrees, 140(-18)(+25) pc) and (V-R, V-theta,V- V-z) = (33 +/- 16, 233 +/- 11 11 2) km. Additionally, from our VLBA observations we measured the relative proper motions among the water maser spots located in the central region of the nebula, which have been proposed to be tracing a toroidal structure. The distribution and relative proper motions of the masers, compared with previous reported observed epochs, suggest that such structure could be totally destroyed within a few years, due to the action of high-velocity winds and the expansion of the ionization front in the nebula. C1 [Tafoya, Daniel; Imai, Hiroshi] Kagoshima Univ, Grad Sch Sci & Engn, Dept Phys & Astron, Kagoshima 8900065, Japan. [Gomez, Yolanda] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Torrelles, Jose M.] Univ Barcelona, Fac Fis, Inst Ciencias Espacio CSIC UB IEEC, E-08028 Barcelona, Spain. [Patel, Nimesh A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Anglada, Guillem] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Miranda, Luis F.] Inst Astrofis Andalucia CSIC, E-18008 Granada, Spain. [Honma, Mareki; Hirota, Tomoya; Miyaji, Takeshi] Natl Astron Observ Japan, Mizusawa VLBI Observ, Mizusawa Ku, Oshu, Iwate 0230861, Japan. RP Tafoya, D (reprint author), Kagoshima Univ, Grad Sch Sci & Engn, Dept Phys & Astron, 1-21-35 Korimoto, Kagoshima 8900065, Japan. EM dtafoya@milkiway.kagoshima-u.ac.jp OI Torrelles, Jose Maria/0000-0002-6896-6085 FU Japan Society for the Promotion of Science [22-00022, 20540234]; Ministry of Education, Culture, Sports, Science and Technology [18740109]; CONACyT [80769]; MICINN (Spain) [AYA2008-06189-C03]; Junta de Andalucia (Spain); Spanish MICINN [AYA2008-01934]; Junta de Andalucia [FQM1747] FX D. T. acknowledges support from Japan Society for the Promotion of Science (project ID: 22-00022). H. I. has been financially supported by a Grant-in-Aid for Young Scientists from the Ministry of Education, Culture, Sports, Science and Technology (18740109), and by a Grant-in-Aid for Scientific Research from Japan Society for the Promotion of Science (20540234). Y. G. acknowledges support from CONACyT grant 80769. G. A. and J. M. T. acknowledge support from MICINN (Spain) AYA2008-06189-C03 grant (co-funded with FEDER funds) and from Junta de Andalucia (Spain). L. F. M. is supported partially by grants AYA2008-01934 of the Spanish MICINN (co-funded by FEDER funds) and FQM1747 of the Junta de Andalucia. NR 34 TC 13 Z9 14 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2011 VL 63 IS 1 BP 71 EP 80 DI 10.1093/pasj/63.1.71 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 733SS UT WOS:000288283700009 ER PT J AU Yunes, N Buonanno, A Hughes, SA Pan, Y Barausse, E Miller, MC Throwe, W AF Yunes, Nicolas Buonanno, Alessandra Hughes, Scott A. Pan, Yi Barausse, Enrico Miller, M. Coleman Throwe, William TI Extreme mass-ratio inspirals in the effective-one-body approach: Quasicircular, equatorial orbits around a spinning black hole SO PHYSICAL REVIEW D LA English DT Article ID EVALUATE HOMOGENEOUS SOLUTIONS; GRAVITATIONAL-WAVES; TEUKOLSKY EQUATION; NUMERICAL-METHODS; LISA; RADIATION; PARTICLE; PERTURBATIONS; ENERGY; FIELD AB We construct effective-one-body waveform models suitable for data analysis with the Laser Interferometer Space Antenna for extreme mass-ratio inspirals in quasicircular, equatorial orbits about a spinning supermassive black hole. The accuracy of our model is established through comparisons against frequency-domain, Teukolsky-based waveforms in the radiative approximation. The calibration of eight high-order post-Newtonian parameters in the energy flux suffices to obtain a phase and fractional amplitude agreement of better than 1 rad and 1%, respectively, over a period between 2 and 6 months depending on the system considered. This agreement translates into matches higher than 97% over a period between 4 and 9 months, depending on the system. Better agreements can be obtained if a larger number of calibration parameters are included. Higher-order mass-ratio terms in the effective-one-body Hamiltonian and radiation reaction introduce phase corrections of at most 30 rad in a 1 yr evolution. These corrections are usually 1 order of magnitude larger than those introduced by the spin of the small object in a 1 yr evolution. These results suggest that the effective-one-body approach for extreme mass-ratio inspirals is a good compromise between accuracy and computational price for Laser Interferometer Space Antenna data-analysis purposes. C1 [Yunes, Nicolas] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Yunes, Nicolas; Hughes, Scott A.; Throwe, William] MIT, Dept Phys, Cambridge, MA 02139 USA. [Yunes, Nicolas; Hughes, Scott A.; Throwe, William] MIT, MIT Kavli Inst, Cambridge, MA 02139 USA. [Yunes, Nicolas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buonanno, Alessandra; Pan, Yi; Barausse, Enrico] Univ Maryland, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA. [Buonanno, Alessandra; Pan, Yi; Barausse, Enrico] Univ Maryland, Joint Space Sci Inst, Dept Phys, College Pk, MD 20742 USA. [Miller, M. Coleman] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA. [Miller, M. Coleman] Univ Maryland, Joint Space Sci Inst, Dept Astron, College Pk, MD 20742 USA. RP Yunes, N (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. FU NSF [PHY-0745779, PHY-0903631, PHY-0449884]; National Aeronautics and Space Administration (NASA) [NNX09AI81G, NNX08AL42G, NNX08AH29G, PF0-110080, NAS8-03060] FX We are grateful to Leor Barack, Carlos Sopuerta and Frans Pretorius for useful suggestions and comments. N. Y., A. B., E. B., Y. P., and S. A. H. acknowledge support from the NSF Grants No. PHY-0745779, No. PHY-0903631, and No. PHY-0449884; A. B., S. A. H., and M. C. M. also acknowledge support from NASA Grants No. NNX09AI81G, No. NNX08AL42G, and No. NNX08AH29G. N. Y. acknowledges support from the National Aeronautics and Space Administration through the Einstein Postdoctoral Fellowship Award No. PF0-110080 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under Contract No. NAS8-03060. NR 85 TC 46 Z9 47 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD FEB 24 PY 2011 VL 83 IS 4 AR 044044 DI 10.1103/PhysRevD.83.044044 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 726IK UT WOS:000287713500012 ER PT J AU Bittleston, LS Brockmann, F Wcislo, W Van Bael, SA AF Bittleston, L. S. Brockmann, F. Wcislo, W. Van Bael, S. A. TI Endophytic fungi reduce leaf-cutting ant damage to seedlings SO BIOLOGY LETTERS LA English DT Article DE Attini; herbivory; symbiosis; endophytes; mutualism ID LEAVES AB Our study examines how the mutualism between Atta colombica leaf-cutting ants and their cultivated fungus is influenced by the presence of diverse foliar endophytic fungi (endophytes) at high densities in tropical leaf tissues. We conducted laboratory choice trials in which ant colonies chose between Cordia alliodora seedlings with high (E-high) or low (E-low) densities of endophytes. The Ehigh seedlings contained 5.5 times higher endophyte content and a greater diversity of fungal morphospecies than the E-low treatment, and endophyte content was not correlated with leaf toughness or thickness. Leaf-cutting ants cut over 2.5 times the leaf area from E-low relative to E-high seedlings and had a tendency to recruit more ants to E-low plants. Our findings suggest that leaf-cutting ants may incur costs from cutting and processing leaves with high endophyte loads, which could impact Neotropical forests by causing variable damage rates within plant communities. C1 [Bittleston, L. S.; Brockmann, F.; Wcislo, W.; Van Bael, S. A.] Smithsonian Trop Res Inst, Panama City, Panama. RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM vanbaels@si.edu OI Bittleston, Leonora/0000-0003-4007-5405 NR 14 TC 17 Z9 18 U1 1 U2 17 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD FEB 23 PY 2011 VL 7 IS 1 BP 30 EP 32 DI 10.1098/rsbl.2010.0456 PG 3 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 705LX UT WOS:000286135000010 PM 20610420 ER PT J AU Hughes, DP Wappler, T Labandeira, CC AF Hughes, David P. Wappler, Torsten Labandeira, Conrad C. TI Ancient death-grip leaf scars reveal ant-fungal parasitism SO BIOLOGY LETTERS LA English DT Article DE ant-fungal parasitism; tritrophic interaction; middle Eocene; Messel ID TROPICAL FOREST ECOSYSTEMS; FORMICIDAE; AMBER AB Parasites commonly manipulate host behaviour, and among the most dramatic examples are diverse fungi that cause insects to die attached to leaves. This death-grip behaviour functions to place insects in an ideal location for spore dispersal from a dead body following host death. Fossil leaves record many aspects of insect behaviour (feeding, galls, leaf mining) but to date there are no known examples of behavioural manipulation. Here, we document, to our knowledge, the first example of the stereotypical death grip from 48 Ma leaves of Messel, Germany, indicating the antiquity of this behaviour. As well as probably being the first example of behavioural manipulation in the fossil record, these data support a biogeographical parallelism between mid Eocene northern Europe and recent southeast Asia. C1 [Hughes, David P.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Hughes, David P.] Univ Exeter, Sch Biosci, Exeter EX4 4QJ, Devon, England. [Hughes, David P.] Penn State Univ, Dept Entomol, University Pk, PA 16802 USA. [Wappler, Torsten] Univ Bonn, Steinmann Inst, D-53113 Bonn, Germany. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Hughes, DP (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. EM dhughes@oeb.harvard.edu; labandec@si.edu RI Wappler, Torsten/D-4287-2011 OI Wappler, Torsten/0000-0003-1592-0988 FU Deutsche Forschungsgemeinschaft (DFG); Marie Curie International Fellowship FX This is contribution 157 of the Evolution of Terrestrial Ecosystems consortium at the National Museum of Natural History. D. P. H. is supported by an individual Marie Curie International Fellowship. T. W. gratefully acknowledges financial support by the Deutsche Forschungsgemeinschaft (DFG). Thanks go to F. Marsh for formatting figure 1; B. Farrell for access to imaging facilities for extant samples, and local scientists in Thailand (Khao Chong Botanic Gardens, DNP and BIOTEC) for hospitality. NR 20 TC 14 Z9 17 U1 4 U2 31 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD FEB 23 PY 2011 VL 7 IS 1 BP 67 EP 70 DI 10.1098/rsbl.2010.0521 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 705LX UT WOS:000286135000021 PM 20719770 ER PT J AU Newsome, SD Collins, PW Rick, TC Guthrie, DA Erlandson, JM Fogel, ML AF Newsome, Seth D. Collins, Paul W. Rick, Torben C. Guthrie, Daniel A. Erlandson, Jon M. Fogel, Marilyn L. TI Reply to Hudgens et al.: Bald eagles, no-analog ecological scenarios, and conservation strategies on the Channel Islands SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Newsome, Seth D.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82070 USA. [Collins, Paul W.] Santa Barbara Museum Nat Hist, Santa Barbara, CA 93105 USA. [Rick, Torben C.] Smithsonian Inst, Program Human Ecol, Washington, DC 20013 USA. [Rick, Torben C.] Smithsonian Inst, Archaeobiol Program, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Guthrie, Daniel A.] Claremont Mckenna Coll, Joint Sci Dept, Claremont, CA 91711 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Newsome, Seth D.; Fogel, Marilyn L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. RP Newsome, SD (reprint author), Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82070 USA. EM snewsome@uwyo.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 5 TC 1 Z9 1 U1 1 U2 13 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 22 PY 2011 VL 108 IS 8 BP E26 EP E26 DI 10.1073/pnas.1017611108 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 724ML UT WOS:000287580400004 ER PT J AU Barnes, DKA Kuklinski, P Jackson, JA Keel, GW Morley, SA Winston, JE AF Barnes, David K. A. Kuklinski, Piotr Jackson, Jennifer A. Keel, Geoff W. Morley, Simon A. Winston, Judith E. TI Scott's collections help reveal accelerating marine life growth in Antarctica SO CURRENT BIOLOGY LA English DT Letter ID BRYOZOANS C1 [Barnes, David K. A.; Jackson, Jennifer A.; Morley, Simon A.] British Antarctic Survey, NERC, Cambridge CB3 0ET, England. [Kuklinski, Piotr] Polish Acad Sci, Inst Oceanol, Sopot, Poland. [Kuklinski, Piotr] Nat Hist Museum, London SW7 5BD, England. [Keel, Geoff W.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Winston, Judith E.] Virginia Museum Nat Hist, Martinsville, VA 24112 USA. RP Barnes, DKA (reprint author), British Antarctic Survey, NERC, Madingley Rd, Cambridge CB3 0ET, England. EM dkab@bas.ac.uk RI Jackson, Jennifer/E-7997-2013 NR 8 TC 7 Z9 7 U1 0 U2 11 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD FEB 22 PY 2011 VL 21 IS 4 BP R147 EP R148 DI 10.1016/j.cub.2011.01.033 PG 2 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 726ZS UT WOS:000287767600006 PM 21334291 ER PT J AU Krennrich, F Bautista, M Beilicke, M Benbow, W Boltuch, D Bradbury, SM Cesarini, A Ciupik, L Duke, C Finley, JP Finnegan, G Fortson, L Gall, D Guenette, R Gyuk, G Hanna, D Hui, CM Humensky, TB Kaaret, P Karlsson, N Maier, G McCutcheon, M Ong, RA Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Wagner, RG Wakely, SP Weinstein, A Weisgarber, T Wissel, S AF Krennrich, F. Bautista, M. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Cesarini, A. Ciupik, L. Duke, C. Finley, J. P. Finnegan, G. Fortson, L. Gall, D. Guenette, R. Gyuk, G. Hanna, D. Hui, C. M. Humensky, T. B. Kaaret, P. Karlsson, N. Maier, G. McCutcheon, M. Ong, R. A. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Wagner, R. G. Wakely, S. P. Weinstein, A. Weisgarber, T. Wissel, S. TI Results from the first two years of VERITAS observations SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 2nd Roma International Conference on Astro-particle Physics CY MAY 13-15, 2009 CL Rome, ITALY DE Gamma rays; Observations ID EXTRAGALACTIC BACKGROUND LIGHT; HIGH-ENERGY EMISSION; BL LACERTAE OBJECTS; GAMMA-RAY EMISSION; REMNANT IC 443; HESS J0632+057; CASSIOPEIA-A; RADIATION; TELESCOPE; BLAZARS AB The VERITAS observatory is an imaging atmospheric Cherenkov telescope array located in southern Arizona and covers an energy range between 100 GeV and 30 TeV. The VERITAS collaboration pursues a rigorous observing program that targets a range of key science objectives in astrophysics and particle physics; the understanding of the origin of cosmic rays, the search for supersymmetric dark matter self-annihilation, illuminating the connection between black holes and relativistic jets and constraints to the cosmological diffuse infrared background. We provide a summary of results from the first two years of observations with the full 4-telecope array reported at RICAP09. (C) 2010 Elsevier B.V. All rights reserved. C1 [Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Bautista, M.; Guenette, R.; Hanna, D.; Maier, G.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Boltuch, D.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Perkins, J. S.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Cesarini, A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Finley, J. P.; Gall, D.; Sembroski, G. H.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Finnegan, G.; Hui, C. M.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Ong, R. A.; Weinstein, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Krennrich, F (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM krennrich@iastate.edu OI Cesarini, Andrea/0000-0002-8611-8610; Pandel, Dirk/0000-0003-2085-5586 NR 33 TC 2 Z9 2 U1 0 U2 9 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 FEB 21 PY 2011 VL 630 IS 1 BP 16 EP 21 DI 10.1016/j.nima.2010.06.019 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 727EQ UT WOS:000287780800005 ER PT J AU Lewis, JJ Bowman, TE Feller, DJ AF Lewis, Julian J. Bowman, Thomas E. Feller, Daniel J. TI A synopsis of the subterranean asellids of Maryland, USA, with description of Caecidotea alleghenyensis, new species (Crustacea: Isopoda: Asellota) SO ZOOTAXA LA English DT Article DE Asellidae; Lirceus brachyurus; Caecidotea kenki; Caecidotea pricei; Caecidotea franzi; Caecidotea holsingeri; Caecidotea mausi; Caecidotea vandeli; Caecidotea nordeni ID VIRGINIA; RECORDS AB Nine species of asellid isopods are reported from groundwater habitats in Maryland. Three of these species are habitually found in springs: Lirceus brachyurus, Caecidotea kenki, and C. alleghenyensis, n. sp. The latter, described herein, is a member of the hobbsi group known only from the Allegheny Mountains in Garrett Co. Six species are obligate inhabitants of subterranean waters and are found primarily in Appalachian caves, although some have broad ranges that span noncavernous areas. The obligate subterranean species are Caecidotea pricei, C. franzi, C. holsingeri, C. mausi, C. vandeli and C. nordeni. C1 [Lewis, Julian J.] Karst & Groundwater Biol Consulting LLC, Lewis & Associates Cave, Borden, IN 47106 USA. [Bowman, Thomas E.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Feller, Daniel J.] Maryland Dept Nat Resources, Frostburg, MD 21532 USA. RP Lewis, JJ (reprint author), Karst & Groundwater Biol Consulting LLC, Lewis & Associates Cave, 17903 State Rd 60, Borden, IN 47106 USA. EM lewisbioconsult@aol.com; dfeller@dnr.state.md.us FU National Museum of Natural History; Smithsonian Institution; U.S. Congress; Maryland Department of Natural Resources' Wildlife and Heritage Service FX Funding for this project was provided by the National Museum of Natural History, Smithsonian Institution, kindly facilitated by Ms. Marilyn Schotte. This work was funded in part by State Wildlife Grant funds provided to the state wildlife agencies by U.S. Congress and administered through the Maryland Department of Natural Resources' Wildlife and Heritage Service. Thanks are also extended to Karen Reed and Chad Walter for their assistance during a visit by JJL to the Smithsonian Museum Support Center to work on this project. NR 21 TC 1 Z9 1 U1 1 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 21 PY 2011 IS 2769 BP 54 EP 64 PG 11 WC Zoology SC Zoology GA 723LY UT WOS:000287509300002 ER PT J AU David, LP O'Sullivan, E Jones, C Giacintucci, S Vrtilek, J Raychaudhury, S Nulsen, PEJ Forman, W Sun, M Donahue, M AF David, Laurence P. O'Sullivan, Ewan Jones, Christine Giacintucci, Simona Vrtilek, Jan Raychaudhury, Somak Nulsen, Paul E. J. Forman, William Sun, Ming Donahue, Megan TI ACTIVE-GALACTIC-NUCLEUS-DRIVEN WEATHER AND MULTIPHASE GAS IN THE CORE OF THE NGC 5044 GALAXY GROUP SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: active; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: groups: individual (NGC 5044) ID X-RAY SPECTROSCOPY; XMM-NEWTON; ELLIPTIC GALAXIES; PERSEUS CLUSTER; STAR-FORMATION; ABUNDANCES; SOLAR; TEMPERATURE; CAVITIES; NGC-5044 AB A deep Chandra observation of the X-ray bright group, NGC 5044, shows that the central region of this group has been strongly perturbed by repeated active galactic nucleus (AGN) outbursts. These recent AGN outbursts have produced many small X-ray cavities, cool filaments, and cold fronts. We find a correlation between the coolest X-ray emitting gas and the morphology of the Ha filaments. The Ha filaments are oriented in the direction of the X-ray cavities, suggesting that the warm gas responsible for the Ha emission originated near the center of NGC 5044 and was dredged up behind the buoyant, AGN-inflated X-ray cavities. A detailed spectroscopic analysis shows that the central region of NGC 5044 contains spatially varying amounts of multiphase gas. The regions with the most inhomogeneous gas temperature distribution tend to correlate with the extended 235 MHz and 610 MHz radio emission detected by the Giant Metrewave Radio Telescope. This may result from gas entrainment within the radio emitting plasma or mixing of different temperature gas in the regions surrounding the radio emitting plasma by AGN-induced turbulence. Accounting for the effects of multiphase gas, we find that the abundance of heavy elements is fairly uniform within the central 100 kpc, with abundances of 60%-80% solar for all elements except oxygen, which has a significantly sub-solar abundance. In the absence of continued AGN outbursts, the gas in the center of NGC 5044 should attain a more homogeneous distribution of gas temperature through the dissipation of turbulent kinetic energy and heat conduction in approximately 10(8) yr. The presence of multiphase gas in NGC 5044 indicates that the time between recent AGN outbursts has been less than similar to 10(8) yr. C1 [David, Laurence P.; Jones, Christine; Giacintucci, Simona; Vrtilek, Jan; Nulsen, Paul E. J.; Forman, William] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [O'Sullivan, Ewan; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Sun, Ming] Univ Virginia, Dept Astron, Charlottesville, VA 22901 USA. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP David, LP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ldavid@head.cfa.harvard.edu RI Donahue, Megan/B-5361-2012; OI O'Sullivan, Ewan/0000-0002-5671-6900; Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU European Community under the Marie Curie Research Training Network; [GO8-9122X]; [GO0-11003X] FX We acknowledge Seth Bruch for obtaining the narrow band H alpha + [N II] images at the SOAR. This work was supported by grants GO8-9122X and GO0-11003X. E.O.S. acknowledges the support of the European Community under the Marie Curie Research Training Network. NR 27 TC 29 Z9 29 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2011 VL 728 IS 2 AR 162 DI 10.1088/0004-637X/728/2/162 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600088 ER PT J AU Oberoi, D Matthews, LD Cairns, IH Emrich, D Lobzin, V Lonsdale, CJ Morgan, EH Prabu, T Vedantham, H Wayth, RB Williams, A Williams, C White, SM Allen, G Arcus, W Barnes, D Benkevitch, L Bernardi, G Bowman, JD Briggs, FH Bunton, JD Burns, S Cappallo, RC Clark, MA Corey, BE Dawson, M DeBoer, D De Gans, A deSouza, L Derome, M Edgar, RG Elton, T Goeke, R Gopalakrishna, MR Greenhill, LJ Hazelton, B Herne, D Hewitt, JN Kamini, PA Kaplan, DL Kasper, JC Kennedy, R Kincaid, BB Kocz, J Koeing, R Kowald, E Lynch, MJ Madhavi, S McWhirter, SR Mitchell, DA Morales, MF Ng, A Ord, SM Pathikulangara, J Rogers, AEE Roshi, A Salah, JE Sault, RJ Schinckel, A Shankar, NU Srivani, KS Stevens, J Subrahmanyan, R Thakkar, D Tingay, SJ Tuthill, J Vaccarella, A Waterson, M Webster, RL Whitney, AR AF Oberoi, Divya Matthews, Lynn D. Cairns, Iver H. Emrich, David Lobzin, Vasili Lonsdale, Colin J. Morgan, Edward H. Prabu, T. Vedantham, Harish Wayth, Randall B. Williams, Andrew Williams, Christopher White, Stephen M. Allen, G. Arcus, Wayne Barnes, David Benkevitch, Leonid Bernardi, Gianni Bowman, Judd D. Briggs, Frank H. Bunton, John D. Burns, Steve Cappallo, Roger C. Clark, M. A. Corey, Brian E. Dawson, M. DeBoer, David De Gans, A. deSouza, Ludi Derome, Mark Edgar, R. G. Elton, T. Goeke, Robert Gopalakrishna, M. R. Greenhill, Lincoln J. Hazelton, Bryna Herne, David Hewitt, Jacqueline N. Kamini, P. A. Kaplan, David L. Kasper, Justin C. Kennedy, Rachel Kincaid, Barton B. Kocz, Jonathan Koeing, R. Kowald, Errol Lynch, Mervyn J. Madhavi, S. McWhirter, Stephen R. Mitchell, Daniel A. Morales, Miguel F. Ng, A. Ord, Stephen M. Pathikulangara, Joseph Rogers, Alan E. E. Roshi, Anish Salah, Joseph E. Sault, Robert J. Schinckel, Antony Shankar, N. Udaya Srivani, K. S. Stevens, Jamie Subrahmanyan, Ravi Thakkar, D. Tingay, Steven J. Tuthill, J. Vaccarella, Annino Waterson, Mark Webster, Rachel L. Whitney, Alan R. TI FIRST SPECTROSCOPIC IMAGING OBSERVATIONS OF THE SUN AT LOW RADIO FREQUENCIES WITH THE MURCHISON WIDEFIELD ARRAY PROTOTYPE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: interferometers; radiation mechanisms: non-thermal; Sun: corona; Sun: radio radiation ID SOLAR CORONA; IMAGES; FLARE; MHZ AB We present the first spectroscopic images of solar radio transients from the prototype for the Murchison Widefield Array, observed on 2010 March 27. Our observations span the instantaneous frequency band 170.9-201.6 MHz. Though our observing period is characterized as a period of "low" to "medium" activity, one broadband emission feature and numerous short-lived, narrowband, non-thermal emission features are evident. Our data represent a significant advance in low radio frequency solar imaging, enabling us to follow the spatial, spectral, and temporal evolution of events simultaneously and in unprecedented detail. The rich variety of features seen here reaffirms the coronal diagnostic capability of low radio frequency emission and provides an early glimpse of the nature of radio observations that will become available as the next generation of low-frequency radio interferometers come online over the next few years. C1 [Oberoi, Divya; Matthews, Lynn D.; Lonsdale, Colin J.; Benkevitch, Leonid; Cappallo, Roger C.; Corey, Brian E.; Derome, Mark; Kennedy, Rachel; Kincaid, Barton B.; McWhirter, Stephen R.; Rogers, Alan E. E.; Salah, Joseph E.; Whitney, Alan R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Cairns, Iver H.; Lobzin, Vasili; Thakkar, D.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Emrich, David; Wayth, Randall B.; Arcus, Wayne; Herne, David; Lynch, Mervyn J.; Tingay, Steven J.; Waterson, Mark] Curtin Univ, Curtin Inst Radio Astron, Perth, WA, Australia. [Morgan, Edward H.; Williams, Christopher; Goeke, Robert; Hewitt, Jacqueline N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Prabu, T.; Vedantham, Harish; Gopalakrishna, M. R.; Kamini, P. A.; Madhavi, S.; Roshi, Anish; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, Ravi] Raman Res Inst, Bangalore 560080, Karnataka, India. [Williams, Andrew] Univ Western Australia, Perth Observ, Perth, WA 6009, Australia. [White, Stephen M.] USAF, Res Lab, Kirtland, NM USA. [Allen, G.; Bunton, John D.; DeBoer, David; deSouza, Ludi; Elton, T.; Ng, A.; Pathikulangara, Joseph; Schinckel, Antony; Stevens, Jamie; Tuthill, J.] CSIRO Astron & Space Sci, Epping, NSW, Australia. [Barnes, David] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Melbourne, Vic, Australia. [Bernardi, Gianni; Greenhill, Lincoln J.; Kasper, Justin C.; Mitchell, Daniel A.; Ord, Stephen M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, Judd D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Briggs, Frank H.; Dawson, M.; De Gans, A.; Kocz, Jonathan; Kowald, Errol; Vaccarella, Annino; Waterson, Mark] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Burns, Steve] Burns Ind Inc, Nashua, NH USA. [Clark, M. A.; Edgar, R. G.] Harvard Univ, Fac Arts & Sci, Cambridge, MA 02138 USA. [DeBoer, David; Kennedy, Rachel] Univ Calif Berkeley, Berkeley Astron Dept, Berkeley, CA 94720 USA. [Edgar, R. G.] Massachusetts Gen Hosp, Boston, MA 02114 USA. [Hazelton, Bryna; Morales, Miguel F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI USA. [Roshi, Anish] Natl Radio Astron Observ, Green Bank, WV USA. [Sault, Robert J.; Webster, Rachel L.] Univ Melbourne, Sch Phys, Melbourne, Vic, Australia. RP Oberoi, D (reprint author), MIT, Haystack Observ, Westford, MA 01886 USA. RI Bunton, John/A-4944-2008; Astronomy & Astrophysics Group, Raman Res Institute/D-4046-2012; Kasper, Justin/D-1152-2010; Wayth, Randall/B-2444-2013; Tingay, Steven/B-5271-2013; Emrich, David/B-7002-2013; Waterson, Mark/B-7352-2013; Ord, Stephen/C-6138-2013; Subrahmanyan, Ravi/D-4889-2012; Williams, Andrew/K-2931-2013; Udayashankar , N/D-4901-2012; M, Manjunath/N-4000-2014; OI Kasper, Justin/0000-0002-7077-930X; Wayth, Randall/0000-0002-6995-4131; Emrich, David/0000-0002-4058-1837; Waterson, Mark/0000-0002-0192-2686; Kocz, Jonathon/0000-0003-0249-7586; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Cairns, Iver/0000-0001-6978-9765 FU Commonwealth Government of Australia; Western Australian State government; U.S. National Science Foundation [AST-0457585, PHY-0835713]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; National Collaborative Infrastructure Strategy; Australian federal government via Astronomy Australia Limited; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; iVEC; Initiative in Innovative Computing; NVIDIA; International Centre for Radio Astronomy Research, a Joint Venture of Curtin University FX This work uses data obtained from the Murchison Radioastronomy Observatory (MRO), jointly funded by the Commonwealth Government of Australia and Western Australian State government. The MRO is managed by the CSIRO, who also provides operational support to the MWA. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support came from the U.S. National Science Foundation (grants AST-0457585 and PHY-0835713), the Australian Research Council (grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), the National Collaborative Infrastructure Strategy, funded by the Australian federal government via Astronomy Australia Limited, the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, The Australian National University, iVEC, the Initiative in Innovative Computing and NVIDIA sponsored Center for Excellence at Harvard, and the International Centre for Radio Astronomy Research, a Joint Venture of Curtin University, and The University of Western Australia funded by the Western Australian State government. NR 17 TC 15 Z9 15 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2011 VL 728 IS 2 AR L27 DI 10.1088/2041-8205/728/2/L27 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 715YI UT WOS:000286931200003 ER PT J AU Perets, HB Gal-yam, A Crockett, RM Anderson, JP James, PA Sullivan, M Neill, JD Leonard, DC AF Perets, Hagai B. Gal-yam, Avishay Crockett, R. Mark Anderson, Joseph P. James, Phil A. Sullivan, Mark Neill, James D. Leonard, Douglas C. TI THE OLD ENVIRONMENT OF THE FAINT CALCIUM-RICH SUPERNOVA SN 2005cz SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: star formation; HII regions; stars: formation; supernovae: general; supernovae: individual (SN 2005cz); white dwarfs ID EARLY-TYPE GALAXIES; CORE-COLLAPSE SUPERNOVAE; WOLF-RAYET STARS; IA SUPERNOVAE; HOST GALAXIES; PHOTOMETRIC PERFORMANCE; ELLIPTIC GALAXIES; H-ALPHA; CALIBRATION; MASS AB The supernova SN 2005cz has recently attracted some attention due to the fact that it was spectroscopically similar to type Ib supernovae (SNe Ib), a class that is presumed to result from the core collapse of massive stars, yet it occurred in an elliptical galaxy, where one expects very few massive stars to exist. Two explanations for this remarkable event were put forward. Perets et al. associate SN 2005cz with the class of Ca-rich, faint SNe Ib, which likely result from old double-white-dwarf systems with an He-rich secondary. On the other hand, Kawabata et al. suggest that SN 2005cz is indeed a core-collapse event (in a binary system), albeit of a star at the lower end of the mass range, 10-12 M-circle dot. The existence of this star in its elliptical host is explained as resulting from low-level star formation (SF) activity in that galaxy. Here we present extensive observations of the location of SN 2005cz, sensitive to a variety of SF tracers, including optical spectroscopy, H alpha emission, UV emission, and Hubble Space Telescope photometry. We show that NGC 4589, the host galaxy of SN 2005cz, does not show any signatures of a young stellar population or recent SF activity either close to or far from the location of SN 2005cz. C1 [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02338 USA. [Gal-yam, Avishay] Weizmann Inst Sci, IL-76100 Rehovot, Israel. [Crockett, R. Mark; Sullivan, Mark] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Anderson, Joseph P.] Univ Chile, Dept Astron, Santiago, Chile. [James, Phil A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Neill, James D.] CALTECH, Pasadena, CA 91125 USA. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02338 USA. RI Perets, Hagai/K-9605-2015; OI Perets, Hagai/0000-0002-5004-199X; Sullivan, Mark/0000-0001-9053-4820; James, Philip/0000-0003-4131-5183 NR 46 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2011 VL 728 IS 2 AR L36 DI 10.1088/2041-8205/728/2/L36 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 715YI UT WOS:000286931200012 ER PT J AU Adams, ER Lopez-Morales, M Elliot, JL Seager, S Osip, DJ AF Adams, E. R. Lopez-Morales, M. Elliot, J. L. Seager, S. Osip, D. J. TI TRANSIT TIMING VARIATION ANALYSIS OF OGLE-TR-132b WITH SEVEN NEW TRANSITS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (OGLE-TR-132) ID STELLAR ATMOSPHERE MODELS; LIMB-DARKENING LAW; EXTRASOLAR PLANETS; TERRESTRIAL PLANETS; SURFACE GRAVITIES; LIGHT CURVES; MASS; SYSTEMS; BINARY; PHOTOMETRY AB We report the results of the first transit timing variation analysis of the very hot Jupiter OGLE-TR-132b, using 10 transits collected over a seven-year period. Our analysis combines three previously published transit light curves with seven new transits, which were observed between 2008 February and 2009 May with the new MagIC-e2V instrument on the Magellan Telescopes in Chile. We provide a revised planetary radius of R-p = 1.23 +/- 0.07R(J), which is slightly larger, but consistent within the errors, than that given by previously published results. Analysis of the planet-to-star radius ratio, orbital separation, inclination, and transit duration reveals no apparent variation in any of those parameters during the time span observed. We also find no sign of transit timing variations larger than -108 +/- 49s, with most residuals very close to zero. This allows us to place an upper limit of 5-10 M-circle plus for a coplanar, low-eccentricity perturber in either the 2:1 or 3:2 mean-motion resonance with OGLE-TR-132b. We similarly find that the data are entirely consistent with a constant orbital period and there is no evidence for orbital decay within the limits of precision of our data. C1 [Adams, E. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Adams, E. R.; Elliot, J. L.; Seager, S.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Lopez-Morales, M.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, E-08193 Barcelona, Spain. [Elliot, J. L.; Seager, S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Elliot, J. L.] Lowell Observ, Flagstaff, AZ 86001 USA. [Osip, D. J.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. RP Adams, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Lopez Moya, Marcos/L-2304-2014 OI Lopez Moya, Marcos/0000-0002-8791-7908 FU NASA [NNX07AN63G, HF-01210.01-A/HF-51233.01]; STScI [NAS5-26555] FX E.R.A. received partial support from NASA Origins grant NNX07AN63G. M.L.-M. acknowledges support from NASA through Hubble Fellowship grant HF-01210.01-A/HF-51233.01 awarded by the STScI, which is operated by the AURA, Inc. for NASA, under contract NAS5-26555. We thank Paul Schechter, Brian Taylor, and the Magellan staff for their invaluable assistance with the observations, Josh Carter and Dan Fabrycky for the use of their software, and Dave Charbonneau and Josh Winn for helpful discussions. NR 38 TC 5 Z9 6 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 FEB 20 PY 2011 VL 728 IS 2 AR 125 DI 10.1088/0004-637X/728/2/125 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600051 ER PT J AU Borucki, WJ Koch, DG Basri, G Batalha, N Boss, A Brown, TM Caldwell, D Christensen-Dalsgaard, J Cochran, WD DeVore, E Dunham, EW Dupree, AK Gautier, TN Geary, JC Gilliland, R Gould, A Howell, SB Jenkins, JM Kjeldsen, H Latham, DW Lissauer, JJ Marcy, GW Monet, DG Sasselov, D Tarter, J Charbonneau, D Doyle, L Ford, EB Fortney, J Holman, MJ Seager, S Steffen, JH Welsh, WF Allen, C Bryson, ST Buchhave, L Chandrasekaran, H Christiansen, JL Ciardi, D Clarke, BD Dotson, JL Endl, M Fischer, D Fressin, F Haas, M Horch, E Howard, A Isaacson, H Kolodziejczak, J Li, J MacQueen, P Meibom, S Prsa, A Quintana, EV Rowe, J Sherry, W Tenenbaum, P Torres, G Twicken, JD Van Cleve, J Walkowicz, L Wu, H AF Borucki, William J. Koch, David G. Basri, Gibor Batalha, Natalie Boss, Alan Brown, Timothy M. Caldwell, Douglas Christensen-Dalsgaard, Jorgen Cochran, William D. DeVore, Edna Dunham, Edward W. Dupree, Andrea K. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald Gould, Alan Howell, Steve B. Jenkins, Jon M. Kjeldsen, Hans Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Monet, David G. Sasselov, Dimitar Tarter, Jill Charbonneau, David Doyle, Laurance Ford, Eric B. Fortney, Jonathan Holman, Matthew J. Seager, Sara Steffen, Jason H. Welsh, William F. Allen, Christopher Bryson, Stephen T. Buchhave, Lars Chandrasekaran, Hema Christiansen, Jessie L. Ciardi, David Clarke, Bruce D. Dotson, Jessie L. Endl, Michael Fischer, Debra Fressin, Francois Haas, Michael Horch, Elliott Howard, Andrew Isaacson, Howard Kolodziejczak, Jeffery Li, Jie MacQueen, Phillip Meibom, Soren Prsa, Andrej Quintana, Elisa V. Rowe, Jason Sherry, William Tenenbaum, Peter Torres, Guillermo Twicken, Joseph D. Van Cleve, Jeffrey Walkowicz, Lucianne Wu, Hayley TI CHARACTERISTICS OF KEPLER PLANETARY CANDIDATES BASED ON THE FIRST DATA SET SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: detection; surveys ID TRANSITING PLANET; INITIAL CHARACTERISTICS; TERRESTRIAL PLANETS; CADENCE DATA; PERFORMANCE; SCIENCE; STAR AB In the spring of 2009, the Kepler Mission commenced high-precision photometry on nearly 156,000 stars to determine the frequency and characteristics of small exoplanets, conduct a guest observer program, and obtain asteroseismic data on a wide variety of stars. On 2010 June 15, the Kepler Mission released most of the data from the first quarter of observations. At the time of this data release, 705 stars from this first data set have exoplanet candidates with sizes from as small as that of Earth to larger than that of Jupiter. Here we give the identity and characteristics of 305 released stars with planetary candidates. Data for the remaining 400 stars with planetary candidates will be released in 2011 February. More than half the candidates on the released list have radii less than half that of Jupiter. Five candidates are present in and near the habitable zone; two near super-Earth size, and three bracketing the size of Jupiter. The released stars also include five possible multi-planet systems. One of these has two Neptune-size (2.3 and 2.5 Earth radius) candidates with near-resonant periods. C1 [Borucki, William J.; Koch, David G.; Lissauer, Jack J.; Bryson, Stephen T.; Dotson, Jessie L.; Haas, Michael; Rowe, Jason] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basri, Gibor; Marcy, Geoffrey W.; Howard, Andrew; Isaacson, Howard; Walkowicz, Lucianne] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Batalha, Natalie] San Jose State Univ, San Jose, CA 95192 USA. [Boss, Alan] Carnegie Inst Washington, Washington, DC 20015 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas; DeVore, Edna; Jenkins, Jon M.; Tarter, Jill; Doyle, Laurance; Chandrasekaran, Hema; Christiansen, Jessie L.; Clarke, Bruce D.; Li, Jie; Quintana, Elisa V.; Tenenbaum, Peter; Twicken, Joseph D.; Van Cleve, Jeffrey; Wu, Hayley] SETI Inst, Mountain View, CA 94043 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Aarhus, Denmark. [Cochran, William D.; Endl, Michael; MacQueen, Phillip] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Dupree, Andrea K.; Geary, John C.; Latham, David W.; Sasselov, Dimitar; Charbonneau, David; Holman, Matthew J.; Buchhave, Lars; Fressin, Francois; Meibom, Soren; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Howell, Steve B.; Sherry, William] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Monet, David G.] USN Observ, Flagstaff, AZ 86001 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Seager, Sara] MIT, Cambridge, MA 02139 USA. [Steffen, Jason H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. [Allen, Christopher] Orbital Sci Corp, Mountain View, CA 94043 USA. [Ciardi, David] Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA. [Fischer, Debra] Yale Univ, New Haven, CT 06520 USA. [Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA. [Kolodziejczak, Jeffery] MSFC, Huntsville, AL 35805 USA. [Prsa, Andrej] Villanova Univ, Villanova, PA 19085 USA. RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM William.J.Borucki@nasa.gov RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861 FU NASA's Science Mission Directorate; W. M. Keck Foundation FX Kepler was competitively selected as the 10th Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors thank the many people who gave so generously of their time to make this mission a success. NR 30 TC 192 Z9 192 U1 0 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2011 VL 728 IS 2 AR 117 DI 10.1088/0004-637X/728/2/117 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600043 ER PT J AU Dupree, AK Strader, J Smith, GH AF Dupree, A. K. Strader, Jay Smith, Graeme H. TI DIRECT EVIDENCE FOR AN ENHANCEMENT OF HELIUM IN GIANT STARS IN OMEGA CENTAURI SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (Omega Centauri); stars: abundances; stars: Population II ID DOUBLE MAIN-SEQUENCE; GLOBULAR-CLUSTERS; HORIZONTAL-BRANCH; RED GIANTS; 2ND-GENERATION STARS; NGC 5139; ABUNDANCES; POPULATION; OXYGEN; FIELD AB The double main sequence identified in the globular cluster Omega Centauri has been interpreted using isochrones to indicate a large variation in the abundance of helium. If true, a helium enhancement carries strong implications for the chemical and stellar evolutionary history of this cluster. However, only indirect measures currently support this conjecture. We report the discovery of a variation in the line strength of the near-infrared He I 10830 angstrom transition in 12 similar red giants in Omega Centauri observed with PHOENIX on Gemini-S. Abundances of these stars derived from Magellan/MIKE spectra taken at the Las Campanas Observatory show that the helium transition is not detected in the most metal-poor population ([Fe/H] < -1.8), yet is present in the majority of stars with [Fe/H] >= -1.8. These observations give the first direct evidence for an enhancement of helium in Omega Centauri. The appearance of helium appears better correlated with increased [Al/Fe] and [Na/Fe] abundances than as a function of [Fe/H], giving observational support to the presence of high-temperature H burning in a prior generation of stars. C1 [Dupree, A. K.; Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, Graeme H.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dupree@cfa.harvard.edu; jstrader@cfa.harvard.edu; graeme@ucolick.org FU NASA [HST-HF-51237.01, NAS 5-26555]; Space Telescope Science Institute FX This research has made use of NASA's Astrophysics Data System. We thank the US Gemini Office for assistance in preparing Phase II and for providing travel support to Gemini-S. We thank Steve Margheim and Claudia Winge for Phase II advice and support during our classical run at Gemini-S. J.S. acknowledges support provided by NASA through Hubble Fellowship grant HST-HF-51237.01, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 58 TC 41 Z9 41 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 FEB 20 PY 2011 VL 728 IS 2 AR 155 DI 10.1088/0004-637X/728/2/155 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600081 ER PT J AU Gillaspy, JD Lin, T Tedesco, L Tan, JN Pomeroy, JM Laming, JM Brickhouse, N Chen, GX Silver, E AF Gillaspy, J. D. Lin, T. Tedesco, L. Tan, J. N. Pomeroy, J. M. Laming, J. M. Brickhouse, N. Chen, G. -X. Silver, E. TI Fe XVII X-RAY LINE RATIOS FOR ACCURATE ASTROPHYSICAL PLASMA DIAGNOSTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; line: formation; opacity; plasmas; X-rays: general ID BEAM ION-TRAP; PHOTOIONIZATION CROSS-SECTIONS; LABORATORY MEASUREMENTS; COLLISION STRENGTHS; RELATIVE INTENSITY; RATE COEFFICIENTS; TRANSITIONS; EMISSION; EBIT; RECOMBINATION AB New laboratory measurements using an electron beam ion trap and an X-ray microcalorimeter are presented for the n = 3 to n = 2 Fe XVII emission lines in the 15-17 angstrom range, along with new theoretical predictions for a variety of electron energy distributions. This work improves upon our earlier work on these lines by providing measurements at more electron-impact energies (seven values from 846 to 1185 eV), performing an in situ determination of the X-ray window transmission, taking steps to minimize the ion impurity concentrations, correcting the electron energies for space charge shifts, and estimating the residual electron energy uncertainties. The results for the 3C/3D and 3s/3C line ratios are generally in agreement with the closest theory to within 10%, and in agreement with previous measurements from an independent group to within 20%. Better consistency between the two experimental groups is obtained at the lowest electron energies by using theory to interpolate, taking into account the significantly different electron energy distributions. Evidence for resonance collision effects in the spectra is discussed. Renormalized values for the absolute cross sections of the 3C and 3D lines are obtained by combining previously published results and shown to be in agreement with the predictions of converged R-matrix theory. This work establishes consistency between results from independent laboratories and improves the reliability of these lines for astrophysical diagnostics. Factors that should be taken into account for accurate diagnostics are discussed, including electron energy distribution, polarization, absorption/scattering, and line blends. C1 [Gillaspy, J. D.; Tedesco, L.; Tan, J. N.; Pomeroy, J. M.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Lin, T.; Brickhouse, N.; Chen, G. -X.; Silver, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laming, J. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Gillaspy, JD (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. EM john.gillaspy@nist.gov RI Sanders, Susan/G-1957-2011; OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA [NNX08AK33G] FX We thank Stuart Loch and Connor Ballance for their calculations (done in collaboration with Mitch Pindzola and Don Griffin), and Don Landis, Norm Madden, Jeff Beeman, Eugene Haller, Gerry Austin, and David Caldwell for contributing to the development of the microcalorimeter. This work is supported by NASA grant NNX08AK33G. NR 52 TC 26 Z9 26 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2011 VL 728 IS 2 AR 132 DI 10.1088/0004-637X/728/2/132 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600058 ER PT J AU Hartman, JD Bakos, GA Kipping, DM Torres, G Kovacs, G Noyes, RW Latham, DW Howard, AW Fischer, DA Johnson, JA Marcy, GW Isaacson, H Quinn, SN Buchhave, LA Beky, B Sasselov, DD Stefanik, RP Esquerdo, GA Everett, M Perumpilly, G Lazar, J Papp, I Sari, P AF Hartman, J. D. Bakos, G. A. Kipping, D. M. Torres, G. Kovacs, G. Noyes, R. W. Latham, D. W. Howard, A. W. Fischer, D. A. Johnson, J. A. Marcy, G. W. Isaacson, H. Quinn, S. N. Buchhave, L. A. Beky, B. Sasselov, D. D. Stefanik, R. P. Esquerdo, G. A. Everett, M. Perumpilly, G. Lazar, J. Papp, I. Sari, P. TI HAT-P-26b: A LOW-DENSITY NEPTUNE-MASS PLANET TRANSITING A K STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-26, GSC 0320-01027); techniques: photometric; techniques: spectroscopic ID SKY SURVEY 2MASS; HOT-JUPITERS; ECLIPSING BINARIES; SUPER-EARTH; EXTRASOLAR PLANETS; ATMOSPHERIC LOSS; BLEND SCENARIOS; ECCENTRIC ORBIT; OPEN CLUSTERS; LIGHT CURVES AB We report the discovery of HAT-P-26b, a transiting extrasolar planet orbiting the moderately bright V = 11.744 K1 dwarf star GSC 0320-01027, with a period P = 4.234516 +/- 0.000015 days, transit epoch T-c = 2455304.65122 +/- 0.00035 ( BJD; Barycentric Julian dates throughout the paper are calculated from Coordinated Universal Time (UTC)), and transit duration 0.1023 +/- 0.0010 days. The host star has a mass of 0.82 +/- 0.03 M-circle dot, radius of 0.79(0.04)(+0.10) R-circle dot, effective temperature 5079 +/- 88 K, and metallicity [Fe/H] = -0.04 +/- 0.08. The planetary companion has a mass of 0.059 +/- 0.007 M-J, and radius of 0.565(-0.032)(+0.072) R-J yielding a mean density of 0.40 +/- 0.10 g cm(-3). HAT-P-26b is the fourth Neptune-mass transiting planet discovered to date. It has a mass that is comparable to those of Neptune and Uranus, and slightly smaller than those of the other transiting Super-Neptunes, but a radius that is similar to 65% larger than those of Neptune and Uranus, and also larger than those of the other transiting Super-Neptunes. HAT-P-26b is consistent with theoretical models of an irradiated Neptune-mass planet with a 10 M-circle plus heavy element core that comprises greater than or similar to 50% of its mass with the remainder contained in a significant hydrogen-helium envelope, though the exact composition is uncertain as there are significant differences between various theoretical models at the Neptune-mass regime. The equatorial declination of the star makes it easily accessible to both Northern and Southern ground-based facilities for follow-up observations. C1 [Hartman, J. D.; Bakos, G. A.; Kipping, D. M.; Torres, G.; Noyes, R. W.; Latham, D. W.; Quinn, S. N.; Buchhave, L. A.; Beky, B.; Sasselov, D. D.; Stefanik, R. P.; Esquerdo, G. A.; Everett, M.; Perumpilly, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kipping, D. M.] UCL, Dept Phys & Astron, London, England. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Howard, A. W.; Marcy, G. W.; Isaacson, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Perumpilly, G.] Univ S Dakota, Dept Phys, Vermillion, SD 57069 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NASA [NNG04GN74G, NNX08AF23G, AST-0702843, AST-0702821, NNX09AF59G, NCC2-1390, N018Hr, N167Hr]; SAO IRD; Hungarian Scientific Research Foundation (OTKA) [K-81373] FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D. Work of G.A.B. and J.A.J. were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G.T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (PI: D.W.L.). G.K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. This research has made use of Keck telescope time granted through NASA (N018Hr and N167Hr). NR 87 TC 39 Z9 40 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 FEB 20 PY 2011 VL 728 IS 2 AR 138 DI 10.1088/0004-637X/728/2/138 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600064 ER PT J AU Liu, CZ Peng, EW Jordan, A Ferrarese, L Blakeslee, JP Cote, P Mei, S AF Liu, Chengze Peng, Eric W. Jordan, Andres Ferrarese, Laura Blakeslee, John P. Cote, Patrick Mei, Simona TI THE ACS FORNAX CLUSTER SURVEY. X. COLOR GRADIENTS OF GLOBULAR CLUSTER SYSTEMS IN EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Virgo, Fornax); galaxies: elliptical and lenticular, cD; galaxies: star clusters: general; galaxies: stellar content; globular clusters: general ID STELLAR POPULATION GRADIENTS; DATA REDUCTION PROCEDURES; DIGITAL SKY SURVEY; HALF-LIGHT RADII; VIRGO-CLUSTER; ELLIPTIC GALAXIES; METALLICITY GRADIENTS; LUMINOSITY FUNCTION; MAGNITUDE RELATION; WASHINGTON PHOTOMETRY AB We use the largest homogeneous sample of globular clusters (GCs), drawn from the ACS Virgo Cluster Survey (ACSVCS) and ACS Fornax Cluster Survey (ACSFCS), to investigate the color gradients of GC systems in 76 early-type galaxies. We find that most GC systems possess an obvious negative gradient in (g-z) color with radius (bluer outward), which is consistent with previous work. For GC systems displaying color bimodality, both metal-rich and metal-poor GC subpopulations present shallower but significant color gradients on average, and the mean color gradients of these two subpopulations are of roughly equal strength. The field of view of ACS mainly restricts us to measuring the inner gradients of the studied GC systems. These gradients, however, can introduce an aperture bias when measuring the mean colors of GC subpopulations from relatively narrow central pointings. Inferred corrections to previous work imply a reduced significance for the relation between the mean color of metal-poor GCs and their host galaxy luminosity. The GC color gradients also show a dependence with host galaxy mass where the gradients are weakest at the ends of the mass spectrum-in massive galaxies and dwarf galaxies-and strongest in galaxies of intermediate mass, around a stellar mass of M-* approximate to 10(10) M-circle dot. We also measure color gradients for field stars in the host galaxies. We find that GC color gradients are systematically steeper than field star color gradients, but the shape of the gradient-mass relation is the same for both. If gradients are caused by rapid dissipational collapse and weakened by merging, these color gradients support a picture where the inner GC systems of most intermediate-mass and massive galaxies formed early and rapidly with the most massive galaxies having experienced greater merging. The lack of strong gradients in the GC systems of dwarfs, which probably have not experienced many recent major mergers, suggests that low-mass halos were inefficient at retaining and mixing metals during the epoch of GC formation. C1 [Liu, Chengze; Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Peng, Eric W.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Jordan, Andres] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferrarese, Laura; Blakeslee, John P.; Cote, Patrick] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Mei, Simona] Univ Paris Denis Diderot, Bur Galaxies Etoiles Phys Instrumentat GEPI, F-75205 Paris 13, France. [Mei, Simona] Observ Paris, Sect Meudon, GEPI, F-92195 Meudon, France. RP Liu, CZ (reprint author), Peking Univ, Dept Astron, Beijing 100871, Peoples R China. EM czliu@pku.edu.cn; peng@bac.pku.edu.cn; ajordan@astro.puc.cl; laura.ferrarese@nrc-cnrc.gc.ca; John.Blakeslee@nrc-cnrc.gc.ca; patrick.cote@nrc-cnrc.gc.ca; Simona.Mei@obspm.fr RI Liu, Chengze/O-1034-2015; OI Liu, Chengze/0000-0002-4718-3428; Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548 FU NASA [NAS 5-26555]; National Science Foundation of China [10973028]; Peking University; Fonde-cyt project [1095213]; BASAL CATA [PFB-06]; FONDAP CFA [15010003]; MIDEPLAN ICM Nucleus [P07-021-F]; National Natural Science Foundation of China [10873001]; Space Telescope Science Institute [GO-9401, GO-10217]; National Aeronautics and Space Administration; National Science Foundation FX Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.; The authors thank the anonymous referee for useful comments. C.L. would like to thank Ian Mcnabb for assistance, and the National Science Foundation of China (Grant No. 10973028) and the Peking University Postdoctoral Fund for their support. E.W.P. acknowledges support from the Peking University 985 Fund, and grant 10873001 from the National Natural Science Foundation of China. A.J. acknowledges support from Fonde-cyt project 1095213, BASAL CATA PFB-06, FONDAP CFA 15010003, and MIDEPLAN ICM Nucleus P07-021-F.; Support for programs GO-9401 and GO-10217 was provided through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.; This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.; This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 81 TC 33 Z9 33 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2011 VL 728 IS 2 AR 116 DI 10.1088/0004-637X/728/2/116 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600042 ER PT J AU Macario, G Markevitch, M Giacintucci, S Brunetti, G Venturi, T Murray, SS AF Macario, Giulia Markevitch, Maxim Giacintucci, Simona Brunetti, Gianfranco Venturi, Tiziana Murray, Stephen S. TI A SHOCK FRONT IN THE MERGING GALAXY CLUSTER A754: X-RAY AND RADIO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A754); radio continuum: general; shock waves; X-rays: galaxies: clusters ID COMA CLUSTER; CHANDRA OBSERVATION; TEMPERATURE MAP; BOW SHOCK; ABELL 754; HALO; EMISSION; PHYSICS; ACCELERATION; SUBCLUSTERS AB We present new Chandra X-ray and Giant Metrewave Radio Telescope (GMRT) radio observations of the nearby merging galaxy cluster A754. Our X-ray data confirm the presence of a shock front by obtaining the first direct measurement of a gas-temperature jump across the X-ray brightness edge previously seen in the imaging data. A754 is only the fourth galaxy cluster with confirmed merger shock fronts, and it has the weakest shock of those, with a Mach number, M = 1.57(-0.12)(+0.16). In our new GMRT observation at 330 MHz, we find that the previously known centrally located radio halo extends eastward to the position of the shock. The X-ray shock front also coincides with the position of a radio relic previously observed at 74 MHz. The radio spectrum of the post-shock region, using our radio data and the earlier results at 74 MHz and 1.4 GHz, is very steep. We argue that acceleration of electrons at the shock front directly from thermal to ultrarelativistic energies is problematic due to energy arguments, while reacceleration of pre-existing relativistic electrons is more plausible. C1 [Macario, Giulia; Giacintucci, Simona; Brunetti, Gianfranco; Venturi, Tiziana] INAF Ist Radioastron, I-40129 Bologna, Italy. [Macario, Giulia; Markevitch, Maxim; Giacintucci, Simona; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Macario, G (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM g.macario@ira.inaf.it OI Brunetti, Gianfranco/0000-0003-4195-8613; Venturi, Tiziana/0000-0002-8476-6307 FU INAF; ASI-INAF [E/088/06/0]; Chandra [GO8-9128X]; NASA [NAS8-39073] FX G. M. thanks the hospitality of the Harvard-Smithsonian Center for Astrophysics where most of this work was done. We thank N. Kassim and T. Clarke for providing the VLA image at 74 MHz and for useful comments. We thank Alexey Vikhlinin for stimulating discussions. We thank the staff of GMRT for their help during the observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. This research is partially funded by INAF under grant PRIN-INAF 2008 and by ASI-INAF under grant E/088/06/0. Support was also provided by Chandra grant GO8-9128X and NASA contract NAS8-39073. NR 41 TC 72 Z9 72 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 FEB 20 PY 2011 VL 728 IS 2 AR 82 DI 10.1088/0004-637X/728/2/82 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600009 ER PT J AU Shirley, YL Huard, TL Pontoppidan, KM Wilner, DJ Stutz, AM Bieging, JH Evans, NJ AF Shirley, Yancy L. Huard, Tracy L. Pontoppidan, Klaus M. Wilner, David J. Stutz, Amelia M. Bieging, John H. Evans, Neal J., II TI OBSERVATIONAL CONSTRAINTS ON SUBMILLIMETER DUST OPACITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: clouds; stars: formation ID MASS STAR-FORMATION; CLERK-MAXWELL-TELESCOPE; PROTOSTELLAR COLLAPSE; INFRARED EXTINCTION; MOLECULAR CLOUDS; INTERSTELLAR EXTINCTION; EVOLUTIONARY SIGNATURES; TEMPERATURE-DEPENDENCE; CONTINUUM OBSERVATIONS; INITIAL CONDITIONS AB Infrared extinction maps and submillimeter dust continuum maps are powerful probes of the density structure in the envelope of star-forming cores. We make a direct comparison between infrared and submillimeter dust continuum observations of the low-mass Class 0 core, B335, to constrain the ratio of submillimeter to infrared opacity (kappa(smm)/kappa(ir)) and the submillimeter opacity power-law index (kappa alpha lambda(-beta)). Using the average value of theoretical dust opacity models at 2.2 mu m, we constrain the dust opacity at 850 and 450 mu m. Using new dust continuum models based upon the broken power-law density structure derived from interferometric observations of B335 and the infall model derived from molecular line observations of B335, we find that the opacity ratios are kappa(850)/kappa(2.2) = (3.21-4.80)(-0.30)(+0.44) x 10(-4) and kappa(450)/kappa(2.2) = (12.8-24.8)(-1.3)(+2.4) x 10(-4)with a submillimeter opacity power-law index of beta(smm) = (2.18-2.58)(-0.30)(+0.30). The range of quoted values is determined from the uncertainty in the physical model for B335. For an average 2.2 mu m opacity of 3800 +/- 700 cm(2) g(-1), we find a dust opacity at 850 and 450 mu m of kappa(850) = (1.18-1.77)(-0.24)(+0.36) and kappa(450) = (4.72-9.13)(-0.98)(+1.9) cm(2) g(-1) of dust. These opacities are from (0.65-0.97) kappa(OH5)(850) of the widely used theoretical opacities of Ossenkopf and Henning for coagulated ice grains with thin mantles at 850 mu m. C1 [Huard, Tracy L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Pontoppidan, Klaus M.] CALTECH, Pasadena, CA 91125 USA. [Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stutz, Amelia M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Shirley, Yancy L.; Bieging, John H.] Steward Observ, Tucson, AZ 85721 USA. RP Shirley, YL (reprint author), Natl Radio Astron Observ, Charlottesville, VA 22903 USA. OI Stutz, Amelia/0000-0003-2300-8200 FU NASA [01201.01, NAS 5-26555, NNG04GG24G]; Jet Propulsion Laboratory, California Institute of Technology, under NASA [1407, 1224608, 1230779] FX We sincerely thank the referee for a very thorough and careful reading of the manuscript. We thank Brandon Kelly for comments that improved this paper. Guest User, Canadian Astronomy Data Centre, is operated by the Dominion Astrophysical Observatory for the National Research Council of Canada's Herzberg Institute of Astrophysics. K.M.P. is supported by NASA through Hubble Fellowship grant no. 01201.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Additional support came from NASA Origins grant NNG04GG24G and the Spitzer Legacy Science Program, provided by NASA through contracts 1224608 and 1230779 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407 to N.J.E. NR 78 TC 41 Z9 41 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2011 VL 728 IS 2 AR 143 DI 10.1088/0004-637X/728/2/143 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600069 ER PT J AU Wong, KC Blanton, MR Burles, SM Coil, AL Cool, RJ Eisenstein, DJ Moustakas, J Zhu, GT Arnouts, S AF Wong, Kenneth C. Blanton, Michael R. Burles, Scott M. Coil, Alison L. Cool, Richard J. Eisenstein, Daniel J. Moustakas, John Zhu, Guangtun Arnouts, Stephane TI PRIMUS: ENHANCED SPECIFIC STAR FORMATION RATES IN CLOSE GALAXY PAIRS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: interactions ID DIGITAL SKY SURVEY; INFRARED LUMINOSITY FUNCTIONS; DEEP-FIELD-SOUTH; REDSHIFT SURVEY; MERGER RATE; FORMING GALAXIES; DUST ATTENUATION; FORMATION HISTORY; SPIRAL GALAXIES; MAJOR MERGERS AB Tidal interactions between galaxies can trigger star formation, which contributes to the global star formation rate (SFR) density of the universe and could be a factor in the transformation of blue, star-forming galaxies to red, quiescent galaxies over cosmic time. We investigate tidally triggered star formation in isolated close galaxy pairs drawn from the Prism Multi-Object Survey (PRIMUS), a low-dispersion prism redshift survey that has measured similar to 120,000 robust galaxy redshifts over 9.1 deg(2) out to z similar to 1. We select a sample of galaxies in isolated galaxy pairs at redshifts 0.25 <= z <= 0.75, with no other objects within a projected separation of 300 h(-1) kpc and Delta z/(1 + z) = 0.01, and compare them to a control sample of isolated galaxies to test for systematic differences in their rest-frame FUV - r and NUV - r colors as a proxy for relative specific star formation rates (SSFRs). We find that galaxies in r(p) <= 50 h(-1) kpc pairs have bluer dust-corrected UV - r colors on average than the control galaxies by -0.134 +/- 0.045 mag in FUV - r and -0.075 +/- 0.038 mag in NUV - r, corresponding to an similar to 15%-20% increase in SSFR. This indicates an enhancement in SSFR due to tidal interactions. We also find that this relative enhancement is greater for a subset of r(p) <= 30 h(-1) kpc pair galaxies, for which the average color offsets are -0.193 +/- 0.065 mag in FUV - r and -0.159 +/- 0.048 mag in NUV - r, corresponding to an similar to 25%-30% increase in SSFR. We test for evolution in the enhancement of tidally triggered star formation with redshift across our sample redshift range and find marginal evidence for a decrease in SSFR enhancement from 0.25 <= z <= 0.5 to 0.5 <= z <= 0.75. This indicates that a change in enhanced star formation triggered by tidal interactions in low-density environments is not a contributor to the decline in the global SFR density across this redshift range. C1 [Wong, Kenneth C.; Eisenstein, Daniel J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Blanton, Michael R.; Zhu, Guangtun] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Burles, Scott M.] DE Shaw & Co, LP, Cupertino, CA 95014 USA. [Coil, Alison L.; Moustakas, John] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Cool, Richard J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arnouts, Stephane] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. RP Wong, KC (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Zhu, Guangtun/C-8552-2012; OI Zhu, Guangtun/0000-0002-7574-8078 FU NSF [AST-0607701, 0908246, 0908442, 0908354]; NASA [08-ADP08-0019, NAS 5-26555]; Space Telescope Science Institute [HF-01217] FX We acknowledge James Aird, Rebecca Bernstein, Adam Bolton, Douglas Finkbeiner, David Hogg, Timothy McKay, Sam Roweis, and Wiphu Rujopakarn for their contributions to the PRIMUS project. We also thank Elizabeth Barton, Lihwai Lin, and Daniel McIntosh for insightful discussions regarding this project. We thank the CFHTLS, COSMOS, DLS, and SWIRE teams for their public data releases and access to early releases. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. We thank the support staff at LCO for their help during our observations, and we acknowledge the use of community access through NOAO observing time. Funding for PRIMUS has been provided by NSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA grant 08-ADP08-0019. Support for this work was provided by NASA through Hubble Fellowship grant HF-01217 awarded by the Space Telescope Science Institute, which is operated by the Associated of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. We acknowledge NASA's support for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. NR 92 TC 24 Z9 24 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2011 VL 728 IS 2 AR 119 DI 10.1088/0004-637X/728/2/119 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716MP UT WOS:000286973600045 ER PT J AU Eriksen, KA Hughes, JP Badenes, C Fesen, R Ghavamian, P Moffett, D Plucinksy, PP Rakowski, CE Reynoso, EM Slane, P AF Eriksen, Kristoffer A. Hughes, John P. Badenes, Carles Fesen, Robert Ghavamian, Parviz Moffett, David Plucinksy, Paul P. Rakowski, Cara E. Reynoso, Estela M. Slane, Patrick TI EVIDENCE FOR PARTICLE ACCELERATION TO THE KNEE OF THE COSMIC RAY SPECTRUM IN TYCHO'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; cosmic rays; ISM: individual objects (SN 1572, Tycho); ISM: supernova remnants ID MAGNETIC-FIELD; SHOCK; AMPLIFICATION; CASSIOPEIA; EMISSION; EXPANSION; ENERGY AB Supernova remnants (SNRs) have long been assumed to be the source of cosmic rays (CRs) up to the "knee" of the CR spectrum at 10(15) eV, accelerating particles to relativistic energies in their blast waves by the process of diffusive shock acceleration (DSA). Since CR nuclei do not radiate efficiently, their presence must be inferred indirectly. Previous theoretical calculations and X-ray observations show that CR acceleration significantly modifies the structure of the SNR and greatly amplifies the interstellar magnetic field. We present new, deep X-ray observations of the remnant of Tycho's supernova (SN 1572, henceforth Tycho), which reveal a previously unknown, strikingly ordered pattern of non-thermal high-emissivity stripes in the projected interior of the remnant, with spacing that corresponds to the gyroradii of 10(14)-10(15) eV protons. Spectroscopy of the stripes shows the plasma to be highly turbulent on the (smaller) scale of the Larmor radii of TeV energy electrons. Models of the shock amplification of magnetic fields produce structure on the scale of the gyroradius of the highest energy CRs present, but they do not predict the highly ordered pattern we observe. We interpret the stripes as evidence for acceleration of particles to near the knee of the CR spectrum in regions of enhanced magnetic turbulence, while the observed highly ordered pattern of these features provides a new challenge to models of DSA. C1 [Eriksen, Kristoffer A.; Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Badenes, Carles] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Badenes, Carles] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Fesen, Robert] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Ghavamian, Parviz] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Moffett, David] Furman Univ, Dept Phys, Greenville, SC 29613 USA. [Plucinksy, Paul P.; Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rakowski, Cara E.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Reynoso, Estela M.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reynoso, Estela M.] Univ Buenos Aires, Fac Exact & Nat Sci, RA-1053 Buenos Aires, DF, Argentina. RP Eriksen, KA (reprint author), Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA. FU Rutgers University [GO9-0078X]; CONICET; UBA; ANPCyT FX This work was partially supported by Chandra award (grant number GO9-0078X) to Rutgers University. E.M.R. is a member of the CIC (CONICET) and is funded by the CONICET, UBA, and ANPCyT projects. J.P.H. acknowledges helpful discussions with Mario Riquelme, Anatoly Spitkovsky, Tom Jones, Roger Blandford, and Martin Laming. We also thank Christopher McKee for contributing to the original Chandra proposal. NR 26 TC 49 Z9 49 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2011 VL 728 IS 2 AR L28 DI 10.1088/2041-8205/728/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 715YI UT WOS:000286931200004 ER PT J AU Tscherbul, TV Yu, HG Dalgarno, A AF Tscherbul, T. V. Yu, H. -G. Dalgarno, A. TI Sympathetic Cooling of Polyatomic Molecules with S-State Atoms in a Magnetic Trap SO PHYSICAL REVIEW LETTERS LA English DT Article ID AMMONIA MOLECULES; METHYLENE AB We present a rigorous theoretical study of low-temperature collisions of polyatomic molecular radicals with (1)S(0) atoms in the presence of an external magnetic field. Accurate quantum scattering calculations based on ab initio and scaled interaction potentials show that collision-induced spin relaxation of the prototypical organic molecule CH(2)((X) over tilde (3)B(1)) (methylene) and nine other triatomic radicals in cold (3)He gas occurs at a slow rate, demonstrating that cryogenic buffer-gas cooling and magnetic trapping of these molecules is feasible with current technology. Our calculations further suggest that it may be possible to create ultracold gases of polyatomic molecules by sympathetic cooling with alkaline-earth atoms in a magnetic trap. C1 [Tscherbul, T. V.; Dalgarno, A.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Yu, H. -G.] Brookhaven Natl Lab, Dept Chem, Upton, NY 11973 USA. RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. RI Tscherbul, Timur/K-3286-2014; Yu, Hua-Gen/N-7339-2015 OI Tscherbul, Timur/0000-0001-5689-040X; FU NSF FX We thank G. E. Hall and J. M. Doyle for discussions. This work was supported by NSF grants to the Harvard-MIT CUA and ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 24 TC 23 Z9 23 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 FEB 18 PY 2011 VL 106 IS 7 AR 073201 DI 10.1103/PhysRevLett.106.073201 PG 4 WC Physics, Multidisciplinary SC Physics GA 769JU UT WOS:000291009500001 PM 21405515 ER PT J AU Lumbsch, HT Ahti, T Altermann, S De Paz, GA Aptroot, A Arup, U Pena, AB Bawingan, PA Benatti, MN Betancourt, L Bjork, CR Boonpragob, K Brand, M Bungartz, F Caceres, MES Candan, M Chaves, JL Clerc, P Common, R Coppins, BJ Crespo, A Dal-Forno, M Divakar, PK Duya, MV Elix, JA Elvebakk, A Fankhauser, JD Farkas, E Ferraro, LI Fischer, E Galloway, DJ Gaya, E Giralt, M Goward, T Grube, M Hafellner, J Hernandez, JE Campos, MDH Kalb, K Karnefelt, I Kantvilas, G Killmann, D Kirika, P Knudsen, K Komposch, H Kondratyuk, S Lawrey, JD Mangold, A Marcelli, MP Mccune, B Messuti, MI Michlig, A Gonzalez, RM Moncada, B Naikatini, A Nelsen, MP Ovstedal, DO Palice, Z Papong, K Parnmen, S Perez-Ortega, S Printzen, C Rico, VJ Plata, ER Robayo, J Rosabal, D Ruprecht, U Allen, NS Sancho, L De Jesus, LS Vieira, TS Schultz, M Seaward, MRD Serusiaux, E Schmitt, I Sipman, HJM Sohrabi, M Sochting, U Sogaard, MZ Sparrius, LB Spielmann, A Spribille, T Sutjaritturakan, J Thammathaworn, A Thell, A Thor, G Thus, H Timdal, E Truong, C Turk, R Tenorio, LU Upreti, DK Van den Boom, P Rebuelta, MV Wedin, M Will-Wolf, S Wirth, V Wirtz, N Yahr, R Yeshitela, K Ziemmeck, F Wheeler, T Lucking, R AF Lumbsch, H. Thorsten Ahti, Teuvo Altermann, Susanne Amo De Paz, Guillermo Aptroot, Andre Arup, Ulf Barcenas Pena, Alejandrina Bawingan, Paulina A. Benatti, Michel N. Betancourt, Luisa Bjoerk, Curtis R. Boonpragob, Kansri Brand, Maarten Bungartz, Frank Caceres, Marcela E. S. Candan, Mehtmet Luis Chaves, Jose Clerc, Philippe Common, Ralph Coppins, Brian J. Crespo, Ana Dal-Forno, Manuela Divakar, Pradeep K. Duya, Melizar V. Elix, John A. Elvebakk, Arve Fankhauser, Johnathon D. Farkas, Edit Ferraro, Lidia Itati Fischer, Eberhard Galloway, David J. Gaya, Ester Giralt, Mireia Goward, Trevor Grube, Martin Hafellner, Josef Hernandez M, Jesus E. Herrera Campos, Maria De Los Angeles Kalb, Klaus Karnefelt, Ingvar Kantvilas, Gintaras Killmann, Dorothee Kirika, Paul Knudsen, Kerry Komposch, Harald Kondratyuk, Sergey Lawrey, James D. Mangold, Armin Marcelli, Marcelo P. Mccune, Bruce Messuti, Maria Ines Michlig, Andrea Gonzalez, Ricardo Miranda Moncada, Bibiana Naikatini, Alifereti Nelsen, Matthew P. Ovstedal, Dag O. Palice, Zdenek Papong, Khwanruan Parnmen, Sittiporn Perez-Ortega, Sergio Printzen, Christian Rico, Victor J. Plata, Eimy Rivas Robayo, Javier Rosabal, Dania Ruprecht, Ulrike Allen, Noris Salazar Sancho, Leopoldo De Jesus, Luciana Santos Vieira, Tamires Santos Schultz, Matthias Seaward, Mark R. D. Serusiaux, Emmanuel Schmitt, Imke Sipman, Harrie J. M. Sohrabi, Mohammad Sochting, Ulrik Sogaard, Majbrit Zeuthen Sparrius, Laurens B. Spielmann, Adriano Spribille, Toby Sutjaritturakan, Jutarat Thammathaworn, Achra Thell, Arne Thor, Goeran Thues, Holger Timdal, Einar Truong, Camille Tuerk, Roman Umana Tenorio, Loengrin Upreti, Dalip K. Van den Boom, Pieter Vivas Rebuelta, Mercedes Wedin, Mats Will-Wolf, Susan Wirth, Volkmar Wirtz, Nora Yahr, Rebecca Yeshitela, Kumelachew Ziemmeck, Frauke Wheeler, Tim Luecking, Robert TI One hundred new species of lichenized fungi: a signature of undiscovered global diversity SO PHYTOTAXA LA English DT Article DE Darwin declaration; Encyclopedia of Life; Global Taxonomy Initiative; lichens; taxonomy; taxonomic impediment ID TICOLICHEN BIODIVERSITY INVENTORY; WORLD-WIDE KEY; GRAPHIS OSTROPALES-GRAPHIDACEAE; FAMILY GOMPHILLACEAE OSTROPALES; SENSU-STRICTO LECANORALES; WESTERN NORTH-AMERICA; COSTA-RICA; CRYPTIC SPECIATION; GENUS PORPIDIA; 1ST ASSESSMENT AB The number of undescribed species of lichenized fungi has been estimated at roughly 10,000. Describing and cataloging these would take the existing number of taxonomists several decades; however, the support for taxonomy is in decline worldwide. In this paper we emphasize the dire need for taxonomic expertise in lichenology. We bring together 103 colleagues from institutions worldwide to describe a total of 100 new species of lichenized fungi, representing a wide taxonomic and geographic range. The newly described species are: Acarospora flavisparsa, A. janae, Aderkomyces thailandicus, Amandinea maritima, Ampliotrema cocosense, Anomomorpha lecanorina, A. tuberculata, Aspicilia mansourii, Bacidina sorediata, Badimia multiseptata, B. vezdana, Biatora epirotica, Buellia sulphurica, Bunodophoron pinnatum, Byssoloma spinulosum, Calopadia cinereopruinosa, C. editae, Caloplaca brownlieae, C. decipioides, C. digitaurea, C. magnussoniana, C. mereschkowskiana, C. yorkensis, Calvitimela uniseptata, Chapsa microspora, C. psoromica, C. rubropulveracea, C. thallotrema, Chiodecton pustuliferum, Cladonia mongkolsukii, Clypeopyrenis porinoides, Coccocarpia delicatula, Coenogonium flammeum, Cresponea ancistrosporelloides, Crocynia microphyllina, Dictyonema hernandezii, D. hirsutum, Diorygma microsporum, D. sticticum, Echinoplaca pernambucensis, E. schizidiifera, Eremithallus marusae, Everniastrum constictovexans, Fellhanera borbonica, Fibrillithecis sprucei, Fissurina astroisidiata, F. nigrolabiata, F. subcomparimuralis, Graphis caribica, G. cerradensis, G. itatiaiensis, G. marusa, Gyalideopsis chicaque, Gyrotrema papillatum, Harpidium gavilaniae, Hypogymnia amplexa, Hypotrachyna guatemalensis, H. indica, H. lueckingii, H. paracitrella, H. paraphyscioides, H. parasinuosa, Icmadophila eucalypti, Krogia microphylla, Lecanora mugambii, L. printzenii, L. xanthoplumosella, Lecidea lygommella, Lecidella greenii, Lempholemma corticola, Lepraria sekikaica, Lobariella sipmanii, Megalospora austropacifica, M. galapagoensis, Menegazzia endocrocea, Myriotrema endoflavescens, Ocellularia albobullata, O. vizcayensis, Ochrolechia insularis, Opegrapha viridipruinosa, Pannaria phyllidiata, Parmelia asiatica, Pertusaria conspersa, Phlyctis psoromica, Placopsis imshaugii, Platismatia wheeleri, Porina huainamdungensis, Ramalina hyrcana, R. stoffersii, Relicina colombiana, Rhizocarpon diploschistidina, Sticta venosa, Sagenidiopsis isidiata, Tapellaria albomarginata, Thelotrema fijiense, Tricharia nigriuncinata, Usnea galapagona, U. pallidocarpa, Verrucaria rhizicola, and Xanthomendoza rosmarieae. In addition, three new combinations are proposed: Fibrillithecis dehiscens, Lobariella botryoides, and Lobariella pallida. C1 [Lumbsch, H. Thorsten; Nelsen, Matthew P.; Plata, Eimy Rivas; Luecking, Robert] Field Museum, Dept Bot, Chicago, IL 60605 USA. [Ahti, Teuvo; Sohrabi, Mohammad] Univ Helsinki, Bot Museum, FI-00014 Helsinki, Finland. [Altermann, Susanne] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Amo De Paz, Guillermo; Crespo, Ana; Divakar, Pradeep K.; Perez-Ortega, Sergio; Rico, Victor J.; Sancho, Leopoldo; Vivas Rebuelta, Mercedes] Univ Complutense Madrid, Dept Biol Vegetal 2, E-28040 Madrid, Spain. [Aptroot, Andre] ABL Herbarium, NL-3762 XK Soest, Netherlands. [Arup, Ulf; Karnefelt, Ingvar; Thell, Arne] Lund Univ, Bot Museum, SE-22361 Lund, Sweden. [Barcenas Pena, Alejandrina; Herrera Campos, Maria De Los Angeles; Gonzalez, Ricardo Miranda] Univ Nacl Autonoma Mexico, Inst Biol, Dept Bot, Mexico City 04360, DF, Mexico. [Bawingan, Paulina A.] St Louis Univ, Coll Nat Sci, Baguio, Philippines. [Benatti, Michel N.; Marcelli, Marcelo P.] Nucleo Pesquisa Micol, Inst Bot, BR-01031970 Sao Paulo, Brazil. [Betancourt, Luisa; Moncada, Bibiana] Univ Distrital Francisco Jose de Caldas, Torre Labs Herbario, Bogota, Colombia. [Bjoerk, Curtis R.] Univ Idaho, Stillinger Herbarium, Moscow, ID 83843 USA. [Boonpragob, Kansri; Parnmen, Sittiporn] Ramkhamhang Univ, Fac Sci, Dept Biol, Bangkok 10240, Thailand. [Bungartz, Frank; Ziemmeck, Frauke] Fdn Charles Darwin, Santa Cruz, Galapagos, Ecuador. [Caceres, Marcela E. S.; De Jesus, Luciana Santos; Vieira, Tamires Santos] Univ Fed Sergipe, Dept Biociencias, BR-4950000 Itabaiana, Sergipe, Brazil. [Candan, Mehtmet] Anadolu Univ, Fac Sci, Dept Biol, TR-26470 Eskisehir, Turkey. [Luis Chaves, Jose; Umana Tenorio, Loengrin] Inst Nacl Biodiversidad INBio, Lab Hongos, Santo Domingo De Heredia, Costa Rica. [Clerc, Philippe; Truong, Camille] Conservatoire & Jardin Bot, CH-1292 Chambesy, Switzerland. [Coppins, Brian J.; Yahr, Rebecca] Royal Bot Garden, Edinburgh EH3 5LR, Midlothian, Scotland. [Dal-Forno, Manuela; Lawrey, James D.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Duya, Melizar V.] Conservat Int Philippines, Quezon City, Philippines. [Elix, John A.] Australian Natl Univ, Res Sch Chem, Canberra, ACT 0200, Australia. [Elvebakk, Arve] Univ Tromso, Tromso Univ Museum, N-9037 Tromso, Norway. [Fankhauser, Johnathon D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Farkas, Edit] Hungarian Acad Sci, Inst Ecol & Bot, H-2163 Vacratot, Hungary. [Ferraro, Lidia Itati; Michlig, Andrea] Inst Bot Nordeste IBONE, RA-3400 Corrientes, Argentina. [Fischer, Eberhard; Killmann, Dorothee; Yeshitela, Kumelachew] Univ Koblenz Landau, Dept Biol, Inst Integrated Nat Sci, D-56070 Koblenz, Germany. [Galloway, David J.] Landcare Res, Dunedin 9054, New Zealand. [Gaya, Ester] Univ Barcelona, Fac Biol, Bot Unit, Dept Plant Biol, E-08028 Barcelona, Spain. [Giralt, Mireia] Univ Rovira & Virgili, Fac Enol Tarragona, Area Bot, Dept Bioquim & Biotecnol, Tarragona, Spain. [Goward, Trevor] Univ British Columbia, Dept Bot, Herbarium, Vancouver, BC V6G 2B1, Canada. [Grube, Martin; Hafellner, Josef; Spribille, Toby] Graz Univ, Inst Pflanzensyst, A-8010 Graz, Austria. [Hernandez M, Jesus E.] Cent Univ Venezuela, Secc Hongos & Liquenes, Div Plantas Vasc, Fdn Inst Bot Venezuela, Caracas 1010A, Venezuela. [Kalb, Klaus] Lichenol Inst Neumarkt, D-92318 Neumarkt, Germany. [Kantvilas, Gintaras] Tasmanian Herbarium, Hobart, Tas 7001, Australia. [Kirika, Paul] Natl Museums Kenya, E Africa Herbarium, Dept Bot, Nairobi, Kenya. [Knudsen, Kerry] Univ Calif Riverside, Dept Bot & Plant Sci, Herbarium, Riverside, CA 92521 USA. [Komposch, Harald] OIKOS Inst Appl Ecol & Basic Res, A-8200 Gleisdorf, Austria. [Kondratyuk, Sergey] MG Kholodny Inst Bot, UA-252601 Kiev 4, Ukraine. [Mccune, Bruce] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Messuti, Maria Ines] Univ Comahue, CONICET, Inst Invest Biodiversidad & Medioambiente INIBIOM, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. [Naikatini, Alifereti] Univ S Pacific, Fac Sci & Technol, Inst Appl Sci, Suva, Fiji. [Nelsen, Matthew P.] Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. [Ovstedal, Dag O.] DNS, Bergen Museum, N-5020 Bergen, Norway. [Palice, Zdenek] Acad Sci Czech Republic, Inst Bot, CZ-25243 Pruhonice, Czech Republic. [Palice, Zdenek] Charles Univ Prague, Fac Nat Sci, Dept Bot, CZ-12801 Prague, Czech Republic. [Papong, Khwanruan] Mahasarakham Univ, Fac Sci, Dept Biol, Khamrieng 44150, Kantarawichai M, Thailand. [Papong, Khwanruan] Mahasarakham Univ, Fac Sci, Nat Med Mushroom Museum, Khamrieng 44150, Kantarawichai M, Thailand. [Printzen, Christian] Forschungsinst Senckenberg, Dept Bot & Mol Evolut, D-60325 Frankfurt, Germany. [Plata, Eimy Rivas] Univ Illinois, Dept Biol Sci, Chicago, IL 60607 USA. [Robayo, Javier] Bosque Protector Rio Guajalito, Quito, Ecuador. [Rosabal, Dania] Univ Oriente, Dept Biol, Santiago De Cuba 90500, Cuba. [Ruprecht, Ulrike] Salzburg Univ, Fachbereich Organism Biol, A-5020 Salzburg, Austria. [Allen, Noris Salazar] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Schultz, Matthias] Univ Hamburg, Bioctr Klein Flottbek, D-22609 Hamburg, Germany. [Schultz, Matthias] Univ Hamburg, Bot Garden, D-22609 Hamburg, Germany. [Seaward, Mark R. D.] Univ Bradford, Dept Environm Sci, Bradford BD7 1DP, W Yorkshire, England. [Serusiaux, Emmanuel] Univ Liege, Plant Taxon & Conservat Biol Unit, B-4000 Liege, Belgium. [Schmitt, Imke] Goethe Univ Frankfurt, Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany. [Schmitt, Imke] Senckenberg, D-60325 Frankfurt, Germany. [Sipman, Harrie J. M.] Bot Garden, D-14195 Berlin, Germany. [Sipman, Harrie J. M.] Bot Museum Berlin Dahlem, D-14195 Berlin, Germany. [Sohrabi, Mohammad] Univ Tabriz, Dept Plant Sci, Tabriz 51666, Iran. [Sochting, Ulrik; Sogaard, Majbrit Zeuthen] Univ Copenhagen, Dept Biol, DK-2100 Copenhagen O, Denmark. [Spielmann, Adriano] Univ Fed Mato Grosso do Sul, Ctr Ciencias Biol & Saude, Dept Biol, Lab Bot, BR-79070900 Campo Grande, MG, Brazil. [Sutjaritturakan, Jutarat] King Mongkut Inst Technol Ladkrabang, Patiew 86160, Chumphon, Thailand. [Thammathaworn, Achra] Khon Kaen Univ, Fac Sci, Dept Biol, Khon Kaen 40002, Khon Kaen Prov, Thailand. [Thor, Goeran] Swedish Univ Agr Sci, Dept Ecol, SE-75007 Uppsala, Sweden. [Thues, Holger] Nat Hist Museum, Dept Bot, London SW7 5BD, England. [Timdal, Einar] Univ Oslo, Nat Hist Museum, N-0318 Oslo, Norway. [Upreti, Dalip K.] Natl Bot Res Inst, Lichenol Lab, Lucknow 226001, Uttar Pradesh, India. [Wedin, Mats] Swedish Museum Nat Hist, Dept Cryptogam Bot, SE-10405 Stockholm, Sweden. [Will-Wolf, Susan] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Wirth, Volkmar] Staatl Museum Nat Kunde, D-76133 Karlsruhe, Germany. RP Lumbsch, HT (reprint author), Field Museum, Dept Bot, 1400 S Lake Shore Dr, Chicago, IL 60605 USA. EM tlumbsch@fieldmuseum.org; teuvo.ahti@helsinki.fi; salter@biology.ucsc.edu; g_amo@farm.ucm.es; andreaptroot@gmail.com; ulf.arup@botmus.lu.se; abarcenas@ibunam2.ibiologia.unam.mx; pbawingan@slu.edu.ph; michel_benatti@yahoo.com.br; macualu@gmail.com; crbjork@gmail.com; kansri@ru.ac.th; fbungartz@fcdarwin.org.ec; mscaceres@hotmail.com; mecandan@anadolu.edu.tr; jchaves@inbio.ac.crm; philippe.clerc@ville-ge.ch; common@msu.edu; lichensEL@btopenworld.com; acrespo@farm.ucm.es; manudalforno@hotmail.com; pdivakar@farm.ucm.es; mvduya@conservation.org; john.elix@anu.edu.au; arve.elvebakk@uit.no; fank0006@umn.edu; efarkas@botanika.hu; itati_liq@yahoo.com.ar; efischer@uni-koblenz.de; gallowayd@xtra.co.nz; eb62@duke.edu; mireia.giralt@urv.cat; tgoward@interchange.ubc.ca; martin.grube@uni-graz.at; josef.hafellner@uni-graz.at; jesus.hernandez@ucv.ve; mahc@ibiologia.unam.mx; klaus.kalb@arcor.de; ingvar.karnefelt@botmus.lu.se; gintaras.kantvilas@tmag.tas.gov.au; killmann@uni-koblenz.de; paulkirika@yahoo.com; knudsen@ucr.edu; harald.komposch@utanet.at; ksya_net@ukr.net; jlawrey@gmu.edu; arminmangold@gmail.com; mpmarcelli@msn.com; bruce.mccune@science.oregonstate.edu; mmessuti@crub.uncoma.edu.ar; andreamichlig@hotmail.com; mirandar_g@yahoo.com.mx; lbmoncada@udistrital.edu.co; naikatini_a@usp.ac.fj; mpnelsen@gmail.com; dag.ovstedal@bm.uib.no; zpalice@yahoo.com; khwanruan.p@msu.ac.th; sparnmen@gmail.com; sperezortega@farm.ucm.es; christian.printzen@senckenberg.de; rico@farm.ucm.es; erivasplata@fieldmuseum.org; javierobayo@gmail.com; drl@cnt.uo.edu.cu; ulrike.carl@sbg.ac.at; salazarn@si.edu; sancholg@farm.ucm.es; lucianaufsbio@hotmail.com; tamy_phn@hotmail.com; schultzm@botanik.uni-hamburg.de; m.r.d.seaward@bradford.ac.uk; e.serusiaux@ulg.ac.be; imke.schmitt@senckenberg.de; h.sipman@bgbm.org; mohammad.sohrabi@helsinki.fi; ulriks@bio.ku.dk; mzsogaard@snm.ku.dk; sparrius@biodiv.nl; adrianospielmann@yahoo.com.br; toby.spribille@uni-graz.at; sea_flora@hotmail.com; achara@kku.ac.th; arne.thell@botmus.lu.se; goran.thor@ekol.slu.se; h.thues@nhm.ac.uk; einar.timdal@nhm.uio.no; camille.truong@ville-ge.ch; roman.tuerk@sbg.ac.at; lumana@inbio.ac.cr; upretidk@rediffmail.com; pvdboom@kpnmail.nl; mpvivas@farm.ucm.es; mats.wedin@nrm.se; swwolf@wisc.edu; volkmar.wirth@online.de; norawirtz@googlemail.com; r.yahr@rbge.org.uk; kumeyesh@yahoo.com; frauke.ziemmeck@fcdarwin.org.ec; timothybwheeler@gmail.com; rlucking@fieldmuseum.org RI Divakar, Pradeep/E-5603-2014; Caceres, Marcela/H-7039-2012; Fankhauser, Johnathon/G-4442-2011; Palice, Zdenek/H-1616-2014; Crespo, Ana/N-6236-2014; SANCHO, LEOPOLDO/G-9120-2015; Spielmann, Adriano/J-8176-2015; Perez-Ortega, Sergio/G-1257-2016; Biodiversity & Climate Res Ctr, BiK-F/C-4266-2012; Marcelli, Marcelo/G-4800-2012; Lumbsch, Thorsten/K-3573-2012; Benatti, Michel/A-7486-2013; Gaya, Ester/B-2305-2014 OI Divakar, Pradeep/0000-0002-0300-0124; Crespo, Ana/0000-0002-5271-0157; SANCHO, LEOPOLDO/0000-0002-4751-7475; Spielmann, Adriano/0000-0003-0137-0807; Perez-Ortega, Sergio/0000-0002-5411-3698; Marcelli, Marcelo/0000-0002-0065-1933; Lumbsch, Thorsten/0000-0003-1512-835X; FU National Geographic Research Grant [8162-07]; Universidad Nacional del Comahue; CONICET; Academy of CR [AV0Z60050516]; Ministry of Education, Youth and Sports [0021620828]; Swedish Research Council (VR) [621-2006-3760, 621-2009-5372]; Carlsberg Foundation [2008_01_0645]; Myndel Botanica Foundation; Societe de Physique et d'Histoire Naturelle de Geneve; Hungarian Scientific Research Fund (OTKA) [K81232]; CONACYT [35008-V]; PAPIIT-UNAM [IN025808]; Spanish Ministerio de Educacion y Ciencia [CGL2007-66734-C03-01]; BSCH-UCM [GR58/08-910773]; EOL initiative; NSF FX Giralt et al. are grateful to Harrie Sipman for his assistance with the Latin diagnosis of Amandinea maritima. The Galapagos National Park Service provided specimens permits for analysis of the new species in the genera Buellia, Calopadia, Coccocarpia, and Megalospora by Bungartz et al. Specimens were collected in the Galapagos Islands with support from a National Geographic Research Grant # 8162-07 to F. Bungartz. This publication is contribution number 2030 of the Charles Darwin Foundation for the Galapagos Islands. Maria Ines Messuti thanks Universidad Nacional del Comahue and CONICET for financial support. ZP acknowledges support of a project of Academy of CR (AV0Z60050516) and the Ministry of Education, Youth and Sports of CR (no. 0021620828). P. Lambley kindly supplied interesting Bunodophoron-collections from Papua New Guinea. M. Wedin acknowledges financial support from The Swedish Research Council (VR 621-2006-3760, VR 621-2009-5372). U. Arup thanks G. Thor for placing the material of Caloplaca decipioides at his disposal and letting him describe this new species. He also thanks P. Lassen for help with the Latin and L. Christiansen for help with the chemical analysis. Sogaard et al. (authors of Caloplaca digitaurea) appreciate the assistance of L. Knudsen for production of the ITS sequences, L. Christiansen for operating the HPLC analyzer, and A. Elvebakk, Tromso, for the possibility to study his collections from Torres del Paine; the work was supported by grant 2008_01_0645 from the Carlsberg Foundation. A. Frisch kindly wrote the Latin diagnosis for Calvitimela uniseptata. L. Ferraro and A. Michlig, authors of Coenogonium flammeum, are grateful to the Myndel Botanica Foundation for financial support of our fieldwork and to the authorities of the National Park of Argentina for collection permits. D. Ovstedal and J. A. Elix are indepted to Mrs. B. Helle and Mr. J. Berge, both Bergen, for help with the illustration, and to Mr. L. Silva, Recife, for donation of the material of Echinoplaca pernambucensis. Goward et al. thank T. Spribille and C. Miller for performing TLC of Hypogymnia samples and Platismatia wheeleri, and Tim Wheeler for providing a photograph. E. Timdal would like to thank the curator of NY for the loan of the West-Indian Phyllopsora material in which the new species of Krogia was discovered. A. Elvebakk would like to thank the staff at CANB for kind help and for possibility to study their material of Pannaria phyllidiata, P. P. Aspaas, the University Library of Tromso, for translating the diagnosis, and J. A. Elix, National University of Australia for hospitality and company in the field, together with G. Kantvilas and P. McCarthy. D. Galloway is grateful to P. M. Jorgensen for providing the Latin diagnosis of Placopsis imshaugii; to J. A. Elix for chemical help, and to A. Fryday (MSC) for the loan of specimens. A. Nordin (Uppsala) kindly wrote the latin diagnosis of Sagenidiopsis isidiata. Bibiana Moncada and Robert Lucking thank David Galloway for valuable comments on the taxonomy of Sticta venosa. Fieldwork on the genus Usnea on the Galapagos Islands by C. Truong and P. Clerc was supported by a grant "Augustin Lombard" from the Societe de Physique et d'Histoire Naturelle de Geneve. The work was made in collaboration with F. Bungartz and the Charles Darwin Foundation, and Maria de los Angeles Herrera-Campos participated in the field trip. The ministry of environment of the Parque Nacional Galapagos provided collection permits. N. Wirtz thanks M. I.; Messuti for organizing and accompanying her on a field trip t Tierra del Fuego. Andre Aptroot and Holger Thus thank U. Passauer and A. Igersheimer (W) for the loan of the type of Verrucaria lignicola Research in Hungary on foliicolous lichens is supported by the Hungarian Scientific Research Fund (OTKA K81232). Edit Farkas is also grateful for the loan of type specimens to the director Dr. Jan Kirschner, the curator Dr Zdenek Palice and the staff at herbarium PRA-V (Pruhonice, Czech Republic). K. Papong thanks Mahasarakham University for support of her study on Thai foliicolous lichens. M. A. Herrera-Campos, A. Barcenas, R. Miranda, and R. Lucking are grateful for grants by CONACYT (# 35008-V) and PAPIIT-UNAM (# IN025808). Victor J. Rico acknowledges support from the Spanish Ministerio de Educacion y Ciencia (Flora Liquenologica Iberica project, CGL2007-66734-C03-01) and from BSCH-UCM (GR58/08-910773). This publication was also supported by a grant of EOL initiative to support a meeting entitled "Parmeliaceae-Improving our understanding of taxonomy, classification and biogeography of the largest family of lichen-forming fungi". Material of some of the new species was collected and studied in the frame of the NSF-funded projects TICOLICHEN (DEB 0206125 to The Field Museum; PI Robert Lucking), "Phylogeny and Taxonomy of Ostropalean Fungi, with Emphasis on the Lichen-forming Thelotremataceae" (DEB 0516116 to The Field Museum; PI H. T. Lumbsch; Co-PI R. Lucking), and "Neotropical Epiphytic Microlichens - An Innovative Inventory of a Highly Diverse yet Little Known Group of Symbiotic Organisms" (DEB 715660 to The Field Museum; PI R. Lucking). The Caterpillar (R) company provided funds to study lichens and other cryptogams from Panama. Maarten Christenhusz is thanked for editing the final version of this manuscript. This publication initiates our worldwide and community-wide revision of the lichen family Graphidaceae in the frame of the NSF-funded project "ATM - Assembling a taxonomic monograph: The lichen family Graphidaceae" (DEB-1025861 to The Field Museum; PI T. Lumbsch, CoPI R. Lucking). NR 303 TC 105 Z9 120 U1 4 U2 57 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 J9 PHYTOTAXA JI Phytotaxa PD FEB 18 PY 2011 VL 18 BP 1 EP 127 PG 127 WC Plant Sciences SC Plant Sciences GA 814EF UT WOS:000294428700001 ER PT J AU Marrow, JC Johnson-Neitman, JL West, GD AF Marrow, Judilee C. Johnson-Neitman, Jennifer L. West, Gary D. TI What Is Your Diagnosis? SO JAVMA-JOURNAL OF THE AMERICAN VETERINARY MEDICAL ASSOCIATION LA English DT Editorial Material C1 [Marrow, Judilee C.; Johnson-Neitman, Jennifer L.; West, Gary D.] Kansas State Univ, Coll Vet Med, Vet Med Teaching Hosp, Manhattan, KS 66506 USA. RP Marrow, JC (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. EM marrowj@si.edu NR 2 TC 0 Z9 0 U1 1 U2 1 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 USA SN 0003-1488 J9 JAVMA-J AM VET MED A JI JAVMA-J. Am. Vet. Med. Assoc. PD FEB 15 PY 2011 VL 238 IS 4 BP 427 EP 428 DI 10.2460/javma.238.4.427 PG 2 WC Veterinary Sciences SC Veterinary Sciences GA 716XT UT WOS:000287007500014 PM 21320008 ER PT J AU Zug, GR Hamilton, AM Austin, CC AF Zug, George R. Hamilton, Alison M. Austin, Christopher C. TI A new Emoia samoensis group lizard (Squamata: Scincidae) from the Cook Islands, South-central Pacific SO ZOOTAXA LA English DT Article DE Emoia samoensis group; Pacific Ocean; Oceania; geographic variation; new species AB The first published report of a large treeskink from Rarotonga, Cook Islands, appeared in 1988. The first museum voucher specimen was collected in 1984. Although this skink seems likely to be a recent arrival to the island of Rarotonga, it represents a unique member of the Emoia samoensis species group. We compare this population with other members of the E. samoensis group and describe the population as Emoia tuitarere n. sp., distinguished by a suite of external characters including SVL, number of dorsal scale rows, and number of subdigital lamellae of the fourth toe. We provide preliminary definitions for the concolor and samoensis species subgroups proposed by Brown (1991), although current molecular data do not support their monophyly (Hamilton et al., 2010). C1 [Zug, George R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hamilton, Alison M.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hamilton, Alison M.; Austin, Christopher C.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Hamilton, Alison M.; Austin, Christopher C.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Zug, GR (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. EM zugg@si.edu; ahamilton@ucla.edu; ccaustin@lsu.edu FU National Science Foundation [DEB 0408010, DEB 0445213, DBI 0400797]; EPSCoR; Graduate Women in Science; American Society of Ichthyologists and Herpetologists; Society for the Study of Amphibians and Reptiles; Sigma Xi (LSU chapter); University of North Dakota (Graduate School, Office of Research and Program Development, Department of Biology); Louisiana State University (Museum of Natural Science and BioGrads); Smithsonian Scholarly Studies Program; NMNH-Research Opportunities Fund FX Our research into the biology and evolution of Pacific lizards has received support from several sources: National Science Foundation (DEB 0408010, DEB 0445213, DBI 0400797) to CCA and AMH; an EPSCoR Fellowship to AMH; grants from Graduate Women in Science, American Society of Ichthyologists and Herpetologists, Society for the Study of Amphibians and Reptiles, Sigma Xi (LSU chapter), University of North Dakota (Graduate School, Office of Research and Program Development, Department of Biology), and Louisiana State University (Museum of Natural Science and BioGrads) to AMH; and the Smithsonian Scholarly Studies Program and NMNH-Research Opportunities Fund to GRZ. We thank these organization and their representatives for enabling our biodiversity research. NR 16 TC 4 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 15 PY 2011 IS 2765 BP 47 EP 57 PG 11 WC Zoology SC Zoology GA 721AH UT WOS:000287323300004 ER PT J AU Chakraborti, S Ray, A AF Chakraborti, Sayan Ray, Alak TI AN EXPANDING NEUTRAL HYDROGEN SUPERSHELL EVACUATED BY MULTIPLE SUPERNOVAE IN M101 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M101); ISM: bubbles; radio lines: ISM; supernovae: general ID LARGE-MAGELLANIC-CLOUD; H-I SUPERSHELLS; STAR-FORMATION; INTERSTELLAR-MEDIUM; HOLMBERG-II; OB ASSOCIATIONS; GALAXIES; SUPERBUBBLES; EVOLUTION; REMNANTS AB Several neutral hydrogen (H I) cavities have been detected in the Milky Way and other nearby star-forming galaxies. It has been suggested that at least a fraction of them may be expanding supershells driven by the combined mechanical feedback from multiple supernovae (SNe) occurring in an OB association. Yet most extragalactic Hi holes have neither a demonstrated expansion velocity nor an identified OB association inside them. In this work, we report on the discovery of an unbroken expanding H I supershell in the nearby spiral galaxy M101, with a UV-emitting young stellar association inside it. We measure its size (500 pc) and expansion velocity (20 km s(-1)) by identifying both its approaching and receding components in the position-velocity space, using 21 cm emission spectroscopy. This provides us with an ideal system to test the theory of supershells driven by the mechanical feedback from multiple SNe. The UV emission of the cluster inside the supershell is compared with simulated spectral energy distribution of synthetic clusters of the appropriate age (similar to 15 Myr). The observed UV flux is found to be consistent with an association of the appropriate mass (similar to 10(5) M-circle dot) and age required by the energy budget of the supershell. Properties of this supershell and another previously reported in the same galaxy are used to infer its neutral hydrogen scale height and mean neutral hydrogen density in the disk. The presence of another UV-emitting stellar association in overdense swept-up gas is discussed in the context of propagating star formation. C1 [Chakraborti, Sayan; Ray, Alak] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Chakraborti, Sayan; Ray, Alak] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Chakraborti, S (reprint author), Tata Inst Fundamental Res, Dept Astron & Astrophys, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. EM sayan@tifr.res.in; akr@tifr.res.in FU Tata Institute of Fundamental Research [11P-409] FX We thank Richard McCray for discussions at Darjeeling which motivated this work. We thank an anonymous referee for detailed comments which helped in improving this work. S.C. thanks Nimisha Kantharia and Nirupam Roy for discussions on AIPS methods for handling HI data. This work has made use of data from The GALEX Nearby Galaxies Survey. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. This work made use of THINGS, The HI Nearby Galaxy Survey, conducted with the NRAO Very Large Array (VLA). We thank the Institute for Theory and Computation, Harvard University, for its hospitality. At the Tata Institute of Fundamental Research, this work is supported by the 11th Five Year Plan 11P-409. NR 46 TC 6 Z9 6 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 FEB 10 PY 2011 VL 728 IS 1 AR 24 DI 10.1088/0004-637X/728/1/24 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500024 ER PT J AU Qiu, KP Zhang, QZ Menten, KM AF Qiu, Keping Zhang, Qizhou Menten, Karl M. TI OUTFLOWS, ACCRETION, AND CLUSTERED PROTOSTELLAR CORES AROUND A FORMING O STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM: individual objects (NGC 7538); ISM: jets and outflows; stars: early-type; stars: formation; techniques: interferometric ID H-II REGIONS; ULTRACOMPACT HII-REGIONS; NGC-7538 MOLECULAR CLOUD; ORION NEBULA CLUSTER; MASSIVE YOUNG STARS; 7538 IRS 1; HOT CORE; INTERSTELLAR AMMONIA; RECOMBINATION LINE; CIRCUMSTELLAR DISK AB We present a Submillimeter Array study in the 1.3mm wave band of the NGC 7538 IRS 1-3 massive star-forming region. The brightest core in the millimeter continuum map, MM1, harbors the IRS 1 young O star. The core has a gas temperature of about 245 K and shows spatially unresolved emission in complex organic molecules, all typical of a hot molecular core. Toward MM1, redshifted absorption is seen in molecular lines with different energies above the ground state. This absorption probes the inward motion of the dense gas toward the central young O star, and the estimated mass accretion rate reaches 10(-3) M-circle dot yr(-1). Multiple outflows are seen in the CO and (CO)-C-13 maps. The gas mass of 50M(circle dot) and the mass outflow rate of 2.5 x 10(-3) M-circle dot yr(-1) measured in CO line wings are dominated by the MM1 outflow, which is most likely driven by a fast wide-angle wind. Apart from MM1, we discover eight new dusty cores, MM2-9, within a projected distance of 0.35 pc from MM1. These cores show no counterpart in infrared or radio continuum emission, while seven of them appear to be forming intermediate-to high-mass stars. This manifests a deeply embedded star-forming component of the parent cloud of IRS 1-3. Apparently, we are observing a Trapezium system in formation, and the system is presumably surrounded by a cluster of lower mass stars. C1 [Qiu, Keping] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Qiu, Keping; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Qiu, Keping; Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Qiu, KP (reprint author), Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. EM kqiu@mpifr-bonn.mpg.de; qzhang@cfa.harvard.edu; kmenten@mpifr-bonn.mpg.de OI Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; Academia Sinica; NSF [AST-0229008] FX The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.; The CSO is supported by the NSF grant AST-0229008 NR 80 TC 29 Z9 29 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 6 DI 10.1088/0004-637X/728/1/6 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500006 ER PT J AU Hopwood, R Wardlow, J Cooray, A Khostovan, AA Kim, S Negrello, M da Cunha, E Burgarella, D Aretxaga, I Auld, R Baes, M Barton, E Bertoldi, F Bonfield, DG Blundell, R Buttiglione, S Cava, A Clements, DL Cooke, J Dannerbauer, H Dariush, A de Zotti, G Dunlop, J Dunne, L Dye, S Eales, S Fritz, J Frayer, D Gurwell, MA Hughes, DH Ibar, E Ivison, RJ Jarvis, MJ Lagache, G Leeuw, L Maddox, S Michallowski, MJ Omont, A Pascale, E Pohlen, M Rigby, E Rodighiero, G Scott, D Serjeant, S Smail, I Smith, DJB Temi, P Thompson, MA Valtchanov, I van der Werf, P Verma, A Vieira, JD AF Hopwood, R. Wardlow, J. Cooray, A. Khostovan, A. A. Kim, S. Negrello, M. da Cunha, E. Burgarella, D. Aretxaga, I. Auld, R. Baes, M. Barton, E. Bertoldi, F. Bonfield, D. G. Blundell, R. Buttiglione, S. Cava, A. Clements, D. L. Cooke, J. Dannerbauer, H. Dariush, A. de Zotti, G. Dunlop, J. Dunne, L. Dye, S. Eales, S. Fritz, J. Frayer, D. Gurwell, M. A. Hughes, D. H. Ibar, E. Ivison, R. J. Jarvis, M. J. Lagache, G. Leeuw, L. Maddox, S. Michallowski, M. J. Omont, A. Pascale, E. Pohlen, M. Rigby, E. Rodighiero, G. Scott, D. Serjeant, S. Smail, I. Smith, D. J. B. Temi, P. Thompson, M. A. Valtchanov, I. van der Werf, P. Verma, A. Vieira, J. D. TI SPITZER IMAGING OF HERSCHEL-ATLAS GRAVITATIONALLY LENSED SUBMILLIMETER SOURCES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (SDP.81: H-ATLAS J090311.6+003906, SDP.130: H-ATLAS J091305.0-005343); galaxies: starburst; gravitational lensing: strong ID SIMILAR-TO 2; GALAXIES; CO; SPECTROMETER; ULTRAVIOLET; EMISSION; STELLAR; ULIRGS AB We present physical properties of two submillimeter selected gravitationally lensed sources, identified in the Herschel Astrophysical Terahertz Large Area Survey. These submillimeter galaxies (SMGs) have flux densities >100 mJy at 500 mu m, but are not visible in existing optical imaging. We fit light profiles to each component of the lensing systems in Spitzer IRAC 3.6 and 4.5 mu m data and successfully disentangle the foreground lens from the background source in each case, providing important constraints on the spectral energy distributions (SEDs) of the background SMG at rest-frame optical-near-infrared wavelengths. The SED fits show that these two SMGs have high dust obscuration with A(V) similar to 4-5 and star formation rates of similar to 100M(circle dot) yr(-1). They have low gas fractions and low dynamical masses compared with 850 mu m selected galaxies. C1 [Hopwood, R.; Negrello, M.; Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Wardlow, J.; Cooray, A.; Khostovan, A. A.; Kim, S.; Barton, E.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [da Cunha, E.; Cooke, J.] Univ Crete, Dept Phys, Iraklion, Greece. [Burgarella, D.] Aix Marseille Univ, CNRS, OAMP, Lab Astrophys Marseille, Marseille, France. [Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Bertoldi, F.] Univ Bonn, Argenlander Inst Astron, D-53121 Bonn, Germany. [Bonfield, D. G.; Jarvis, M. J.; Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Ctr, Hatfield AL10 9AB, Herts, England. [Blundell, R.; Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buttiglione, S.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Cava, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Cava, A.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Astrophys Grp, London SW7 2AZ, England. [Cooke, J.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Dannerbauer, H.] CEA Saclay, CEA CNRS Univ, Lab AIM Paris Saclay, Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France. [Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran. [de Zotti, G.] Scuola Int Super Studi Avanzati, I-34136 Trieste, Italy. [Dunlop, J.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Dunne, L.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Michallowski, M. J.; van der Werf, P.] Univ Edinburgh, Royal Observ, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. [Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Leeuw, L.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA. [Omont, A.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.] CNRS, F-75014 Paris, France. [Rodighiero, G.] Univ Padua, Dipartimento Astron, Vicolo Osservatorio, I-35122 Padua, Italy. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Smail, I.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Valtchanov, I.] European Space Agcy, Herschel Sci Ctr, Madrid 28691, Spain. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 Leiden, Netherlands. [Verma, A.] Univ Oxford, Oxford OX1 3RH, England. RP Hopwood, R (reprint author), Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. RI Baes, Maarten/I-6985-2013; Smail, Ian/M-5161-2013; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017; OI Smith, Daniel/0000-0001-9708-253X; Rodighiero, Giulia/0000-0002-9415-2296; da Cunha, Elisabete/0000-0001-9759-4797; Baes, Maarten/0000-0002-3930-2757; Smail, Ian/0000-0003-3037-257X; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840; Dye, Simon/0000-0002-1318-8343 FU Science and Technology Facilities Council [D/002400/1, SF/F005288/1]; NASA; NASA Herschel Science Center through JPL/Caltech; CONACyT [50786, 60878]; NASA through JPL/Caltech FX Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS Web site is http://www.h-atlas.org/ We thank the Science and Technology Facilities Council, grant D/002400/1 and studentship/SF/F005288/1. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. US participants in H-ATLAS also acknowledge support from NASA Herschel Science Center through a contract from JPL/Caltech. I. A. and D. H. H. are partially funded by CONACyT grants 50786 and 60878. NR 30 TC 13 Z9 13 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2011 VL 728 IS 1 AR L4 DI 10.1088/2041-8205/728/1/L4 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 711WV UT WOS:000286623000004 ER PT J AU Assef, RJ Kochanek, CS Ashby, MLN Brodwin, M Brown, MJI Cool, R Forman, W Gonzalez, AH Hickox, RC Jannuzi, BT Jones, C Le Floc'h, E Moustakas, J Murray, SS Stern, D AF Assef, R. J. Kochanek, C. S. Ashby, M. L. N. Brodwin, M. Brown, M. J. I. Cool, R. Forman, W. Gonzalez, A. H. Hickox, R. C. Jannuzi, B. T. Jones, C. Le Floc'h, E. Moustakas, J. Murray, S. S. Stern, D. TI THE MID-IR- AND X-RAY-SELECTED QSO LUMINOSITY FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: distances and redshifts; galaxies: luminosity function, mass function; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; WIDE-FIELD SURVEY; RESOLUTION SPECTRAL TEMPLATES; SPITZER-SPACE-TELESCOPE; GALAXY EVOLUTION SURVEY; HIGH-REDSHIFT QUASARS; BLACK-HOLES; MIDINFRARED SELECTION; HOST GALAXIES AB We present the J-band luminosity function (LF) of 1838 mid-infrared and X-ray-selected active galactic nuclei (AGNs) in the redshift range 0 < z < 5.85. These LFs are constructed by combining the deep multi-wavelength broadband observations from the UV to the mid-IR of the NDWFS Bootes field with the X-ray observations of the XBootes survey and the spectroscopic observations of the same field by AGES. Our sample is primarily composed of IRAC-selected AGNs, targeted using modifications of the Stern et al. criteria, complemented by MIPS 24 mu m and X-ray-selected AGNs to alleviate the biases of IRAC mid-IR selection against z similar to 4.5 quasars and AGNs faint with respect to their hosts. This sample provides an accurate link between low-and high-redshift AGN LFs and does not suffer from the usual incompleteness of optical samples at z similar to 3. We use a set of low-resolution spectral energy distribution templates for AGNs and galaxies presented in a previous paper by Assef et al. to model the selection function of these sources and apply host and reddening corrections. We find that the space density of the brightest quasars strongly decreases from z = 3 to z = 0, while the space density of faint quasars is at least flat, and possibly increasing, over the same redshift range. At z > 3, we observe a decrease in the space density of quasars of all brightnesses. We model the LF by a double power law and find that its evolution cannot be described by either pure luminosity or pure density evolution, but must be a combination of both. We used the bright-end slope determined by Croom et al. (2QZ) as a prior to fit the data in order to minimize the effects of our small survey area. The bright-end power-law index of our best-fit model remains consistent with the prior, while the best-fit faint-end index is consistent with the low-redshift measurements based on the 2QZ and 2SLAQ surveys. Our best-fit model generally agrees with the number of bright quasars predicted by other LFs at all redshifts. If we construct the QSO luminosity function using only the IRAC-selected AGNs, we find that the biases inherent to this selection method significantly modify the behavior of the characteristic density phi(*)(z) only for z < 1 and have no significant impact upon the characteristic magnitude M-*,J(z). C1 [Assef, R. J.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Ashby, M. L. N.; Brodwin, M.; Forman, W.; Hickox, R. C.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Cool, R.] Princeton Univ, Princeton, NJ 08540 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. [Hickox, R. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Jannuzi, B. T.] Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Le Floc'h, E.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Moustakas, J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Assef, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM rjassef@astronomy.ohio-state.edu RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Forman, William/0000-0002-9478-1682 FU W. M. Keck Foundation; Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA; National Optical Astronomy Observatory (NOAO); AURA, Inc., under a cooperative agreement with the National Science Foundation FX We thank all the people in the NDWFS, FLAMEX, and SDWFS collaborations that did not directly participate in this work. We also thank the anonymous referee for comments and suggestions that helped improve this work. Support for M. B. was provided by the W. M. Keck Foundation. The work of D.S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The AGES observations were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This work made use of images and/or data products provided by the NOAO Deep Wide-Field Survey (Jannuzi & Dey 1999; B. T. Jannuzi et al. 2011, in preparation; A. Dey et al. 2011, in preparation), which is supported by the National Optical Astronomy Observatory (NOAO). This research draws upon data provided by Dr. Buell Jannuzi and Dr. Arjun Dey as distributed by the NOAO Science Archive. NOAO is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. NR 61 TC 43 Z9 43 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 56 DI 10.1088/0004-637X/728/1/56 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500056 ER PT J AU Brooks, AM Solomon, AR Governato, F McCleary, J MacArthur, LA Brook, CBA Jonsson, P Quinn, TR Wadsley, J AF Brooks, A. M. Solomon, A. R. Governato, F. McCleary, J. MacArthur, L. A. Brook, C. B. A. Jonsson, P. Quinn, T. R. Wadsley, J. TI INTERPRETING THE EVOLUTION OF THE SIZE-LUMINOSITY RELATION FOR DISK GALAXIES FROM REDSHIFT 1 TO THE PRESENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; methods: numerical ID COLD DARK-MATTER; STAR-FORMING GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; ANGULAR-MOMENTUM PROBLEM; BAND SURFACE PHOTOMETRY; LAMBDA-CDM UNIVERSE; DEEP-FIELD SOUTH; MASS-METALLICITY RELATION; TULLY-FISHER RELATION; DIGITAL SKY SURVEY AB A sample of very high resolution cosmological disk galaxy simulations is used to investigate the evolution of galaxy disk sizes back to redshift 1 within the ACDM cosmology. Artificial images in the rest-frame B band are generated, allowing for a measurement of disk scale lengths using surface brightness profiles as observations would, and avoiding any assumption that light must follow mass as previous models have assumed. We demonstrate that these simulated disks are an excellent match to the observed magnitude-size relation for both local disks and for disks at z = 1 in the magnitude/mass range of overlap. We disentangle the evolution seen in the population as a whole from the evolution of individual disk galaxies. In agreement with observations, our simulated disks undergo roughly 1.5 mag arcsec(-2) of surface brightness dimming since z = 1. We find evidence that evolution in the magnitude-size plane varies by mass, such that galaxies with M-* >= 10(9) M-circle dot undergo more evolution in size than luminosity, while dwarf galaxies tend to evolve potentially more in luminosity. The disks grow in such a way as to stay on roughly the same stellar-mass-size relation with time. Finally, due to an evolving stellar-mass-star-formation-rate (SFR) relation, a galaxy at a given stellar mass (or size) at z = 1 will reside in a more massive halo and have a higher SFR, and thus a higher luminosity, than a counterpart of the same stellar mass at z = 0. C1 [Brooks, A. M.; Solomon, A. R.] CALTECH, Pasadena, CA 91125 USA. [Solomon, A. R.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Governato, F.; Quinn, T. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [McCleary, J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [MacArthur, L. A.] NRC Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [MacArthur, L. A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Brook, C. B. A.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Jonsson, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wadsley, J.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L88 4M1, Canada. RP Brooks, AM (reprint author), CALTECH, M-C 350-17, Pasadena, CA 91125 USA. EM abrooks@tapir.caltech.edu OI Solomon, Adam/0000-0002-7411-3951 FU Sherman Fairchild Foundation; Gordon & Betty Moore Foundation; NSF [AST-0908499, AST-0607819]; HST [GO-1125]; NASA ATP [NNX08AG84G]; W. M. Keck Foundation; UK's Science & Technology Facilities Council (STFC) [ST/F002432/1] FX We thank S. Miller and R. Ellis for the use of their z = 1 disk scale length data. A.M.B. acknowledges support from the Sherman Fairchild Foundation. A.R.S. was supported by the Gordon & Betty Moore Foundation. F.G. and T.R.Q. were funded by NSF AST-0908499. F.G. acknowledges support from a Theodore Dunham grant, HST GO-1125, NSF grant AST-0607819, and NASA ATP NNX08AG84G. P.J. acknowledges support from the W. M. Keck Foundation. Simulations were run at TACC, ARSC, and NAS. C.B.A.B. acknowledges the support of the UK's Science & Technology Facilities Council (STFC Grant ST/F002432/1). NR 177 TC 60 Z9 60 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 51 DI 10.1088/0004-637X/728/1/51 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500051 ER PT J AU Espaillat, C Furlan, E D'Alessio, P Sargent, B Nagel, E Calvet, N Watson, DM Muzerolle, J AF Espaillat, C. Furlan, E. D'Alessio, P. Sargent, B. Nagel, E. Calvet, N. Watson, Dan M. Muzerolle, J. TI A SPITZER IRS STUDY OF INFRARED VARIABILITY IN TRANSITIONAL AND PRE-TRANSITIONAL DISKS AROUND T TAURI STARS SO ASTROPHYSICAL JOURNAL LA English DT Article ID PRE-MAIN-SEQUENCE; PROTOPLANETARY ACCRETION DISKS; INTERSTELLAR SILICATE MINERALOGY; ECCENTRIC STELLAR BINARIES; HERBIG AE/BE STARS; FORMING REGION; CHAMELEON-I; CIRCUMSTELLAR DISKS; GRAIN-GROWTH; GM-AURIGAE AB We present a Spitzer IRS study of variability in 14 T Tauri stars in the Taurus and Chamaeleon star-forming regions. The sample is composed of transitional and pre-transitional objects which contain holes and gaps in their disks. We detect variability between 5 and 38 mu m in all but two of our objects on timescales of 2-3 years. Most of the variability observed can be classified as seesaw behavior, whereby the emission at shorter wavelengths varies inversely with the emission at longer wavelengths. For many of the objects we can reasonably reproduce the observed variability using irradiated disk models, particularly by changing the height of the inner disk wall by similar to 20%. When the inner wall is taller, the emission at the shorter wavelengths is higher since the inner wall dominates the emission at 2-8 mu m. The taller inner wall casts a larger shadow on the outer disk wall, leading to less emission at wavelengths beyond 20 mu m where the outer wall dominates. We discuss how the possible presence of planets in these disks could lead to warps that cause changes in the height of the inner wall. We also find that crystalline silicates are common in the outer disks of our objects and that in the four disks in the sample with the most crystalline silicates, variability on timescales of 1 week is present. In addition to explaining the infrared variability described above, planets can create shocks and collisions which can crystallize the dust and lead to short timescale variability. C1 [Espaillat, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Sargent, B.; Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Nagel, E.] Univ Guanajuato, Dept Astron, Guanajuato 36240, Gto, Mexico. [Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Espaillat, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM cespaillat@cfa.harvard.edu; Elise.Furlan@jpl.nasa.gov; p.dalessio@crya.unam.mx; sargent@stsci.edu; erick@astro.ugto.mx; ncalvet@umich.edu; dmw@pas.rochester.edu; muzerol@stsci.edu OI Furlan, Elise/0000-0001-9800-6248 FU National Science Foundation [0901947]; NASA [NNX08AH94G]; PAPIIT-DGAPA UNAM; CONACyT FX We thank the referee for a constructive and thorough report. We thank Lee Hartmann for providing comments on the manuscript and Steve Lubow for useful discussions. C.E. was supported by the National Science Foundation under Award No. 0901947. E.F. was supported by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by JPL/Caltech under a contract with NASA. P.D. acknowledges a grant from PAPIIT-DGAPA UNAM. E.N. acknowledges a postdoctoral grant from CONACyT. N.C. acknowledges support from NASA Origins Grant NNX08AH94G. NR 123 TC 81 Z9 81 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 49 DI 10.1088/0004-637X/728/1/49 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500049 ER PT J AU Goddi, C Humphreys, EML Greenhill, LJ Chandler, CJ Matthews, LD AF Goddi, C. Humphreys, E. M. L. Greenhill, L. J. Chandler, C. J. Matthews, L. D. TI A MULTI-EPOCH STUDY OF THE RADIO CONTINUUM EMISSION OF ORION SOURCE. I. CONSTRAINTS ON THE DISK EVOLUTION OF A MASSIVE YSO AND THE DYNAMICAL HISTORY OF ORION BN/KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; ISM: individual objects (Orion BN/KL); methods: numerical; stars: formation ID LARGE PROPER MOTIONS; BECKLIN-NEUGEBAUER OBJECT; HYPERCOMPACT HII-REGIONS; YOUNG STELLAR OBJECTS; STAR-FORMING REGION; CEPHEUS-A HW2; SUBMILLIMETER ARRAY; HIGH-RESOLUTION; MOLECULAR CLOUDS; NEBULA CLUSTER AB We present new lambda 7 mm continuum observations of Orion BN/KL with the Very Large Array. We resolve the emission from the young stellar objects radio Source I and BN at several epochs. Radio Source I is highly elongated northwest-southeast, and remarkably stable in flux density, position angle, and overall morphology over nearly a decade. This favors the extended emission component arising from an ionized edge-on disk rather than an outwardly propagating jet. We have measured the proper motions of Source I and BN for the first time at 43 GHz. We confirm that both sources are moving at high speed (12 and 26 km s(-1), respectively) approximately in opposite directions, as previously inferred from measurements at lower frequencies. We discuss dynamical scenarios that can explain the large motions of both BN and Source I and the presence of disks around both. Our new measurements support the hypothesis that a close (similar to 50 AU) dynamical interaction occurred around 500 years ago between Source I and BN as proposed by Gomez et al. From the dynamics of encounter, we argue that Source I today is likely to be a binary with a total mass on the order of 20M(circle dot) and that it probably existed as a softer binary before the close encounter. This enables preservation of the original accretion disk, though truncated to its present radius of similar to 50 AU. N-body numerical simulations show that the dynamical interaction between a binary of 20M(circle dot) total mass (Source I) and a single star of 10M(circle dot) mass (BN) may lead to the ejection of both and binary hardening. The gravitational energy released in the process would be large enough to power the wide-angle, high-velocity flow traced by H-2 and CO emission in the BN/KL nebula. Assuming that the proposed dynamical history is correct, the smaller mass for Source I recently estimated from SiO maser dynamics (greater than or similar to 7M(circle dot)) by Matthews et al., suggests that non-gravitational forces (e.g., magnetic) must play an important role in the circumstellar gas dynamics. C1 [Goddi, C.; Humphreys, E. M. L.] European So Observ, D-85748 Garching, Germany. [Goddi, C.; Humphreys, E. M. L.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandler, C. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Goddi, C (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. FU National Science Foundation [NSF AST 0507478] FX We are grateful to Nickolas Moeckel, Mark Krumholz, Leonardo Testi, Daniele Galli, and Malcolm Walmsley for useful discussions. The data presented here were obtained under the VLA programs AM668A, AG622, AC817, and AC952. This work was supported by the National Science Foundation under grant no. NSF AST 0507478. NR 80 TC 50 Z9 50 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 15 DI 10.1088/0004-637X/728/1/15 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500015 ER PT J AU Owers, MS Randall, SW Nulsen, PEJ Couch, WJ David, LP Kempner, JC AF Owers, Matt S. Randall, Scott W. Nulsen, Paul E. J. Couch, Warrick J. David, Laurence P. Kempner, Joshua C. TI THE DISSECTION OF ABELL 2744: A RICH CLUSTER GROWING THROUGH MAJOR AND MINOR MERGERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Abell 2744); X-rays: galaxies: clusters ID RELAXED GALAXY CLUSTERS; COLD-FRONT CLUSTER; X-RAY DATA; XMM-NEWTON; MERGING CLUSTERS; STAR-FORMATION; COMA CLUSTER; DARK-MATTER; RADIO HALO; SKY SURVEY AB New Chandra X-ray data and extensive optical spectroscopy, obtained with AAOmega on the 3.9 m Anglo-Australian Telescope, are used to study the complex merger taking place in the galaxy cluster Abell 2744. Combining our spectra with data from the literature provides a catalog of 1237 redshifts for extragalactic objects lying within 15' of the cluster center. From these, we confirm 343 cluster members projected within 3 Mpc of the cluster center. Combining positions and velocities, we identify two major substructures, corresponding to the remnants of two major subclusters. The new data are consistent with a post-core-passage, major merger taking place along an axis that is tilted well out of the plane of the sky, together with an interloping minor merger. Supporting this interpretation, the new X-ray data reveal enriched, low entropy gas from the core of the approaching, major subcluster, lying similar to 2' north of the cluster center, and a shock front to the southeast of the previously known bright, compact core associated with the receding subcluster. The X-ray morphology of the compact core is consistent with a Bullet-like cluster viewed from within similar to 45 degrees of the merger axis. An X-ray peak similar to 3' northwest of the cluster center, with an associated cold front to the northeast and a trail of low entropy gas to the south, is interpreted as the remnant of an interloping minor merger taking place roughly in the plane of the sky. We infer approximate paths for the three merging components. C1 [Owers, Matt S.; Couch, Warrick J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Randall, Scott W.; Nulsen, Paul E. J.; David, Laurence P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Owers, MS (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM mowers@astro.swin.edu.au OI Randall, Scott/0000-0002-3984-4337; Owers, Matt/0000-0002-2879-1663; Nulsen, Paul/0000-0003-0297-4493 FU Australian Research Council; NASA [NAS8-03060]; Chandra [GO7-8127X] FX We thank Gregory Poole for useful discussions and sanity checks. We are grateful to Will Saunders and the staff at the Anglo-Australian Observatory for their support during AAT observations. We thank Lee Spitler for his assistance in preparing the AAT image and Emily Wisnioski for supplying code for the PCA sky subtraction. We acknowledge the financial support of the Australian Research Council (via its Discovery Project Scheme) throughout the course of this work. P.E.J.N. was partly supported by NASA grant NAS8-03060. This work was partly supported through Chandra GO7-8127X. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa and also of data obtained from the Chandra archive at the NASA Chandra X-ray Center (http://cxc.harvard.edu/cda/). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 96 TC 62 Z9 62 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 FEB 10 PY 2011 VL 728 IS 1 AR 27 DI 10.1088/0004-637X/728/1/27 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500027 ER PT J AU Pignata, G Stritzinger, M Soderberg, A Mazzali, P Phillips, MM Morrell, N Anderson, JP Boldt, L Campillay, A Contreras, C Folatelli, G Forster, F Gonzalez, S Hamuy, M Krzeminski, W Maza, J Roth, M Salgado, F Levesque, EM Rest, A Crain, JA Foster, AC Haislip, JB Ivarsen, KM LaCluyze, AP Nysewander, MC Reichart, DE AF Pignata, Giuliano Stritzinger, Maximilian Soderberg, Alicia Mazzali, Paolo Phillips, M. M. Morrell, Nidia Anderson, J. P. Boldt, Luis Campillay, Abdo Contreras, Carlos Folatelli, Gaston Foerster, Francisco Gonzalez, Sergio Hamuy, Mario Krzeminski, Wojtek Maza, Jose Roth, Miguel Salgado, Francisco Levesque, Emily M. Rest, Armin Crain, J. Adam Foster, Andrew C. Haislip, Joshua B. Ivarsen, Kevin M. LaCluyze, Aaron P. Nysewander, Melissa C. Reichart, Daniel E. TI SN 2009bb: A PECULIAR BROAD-LINED TYPE Ic SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 3278); supernovae: general; supernovae: individual (SN 2009bb) ID GAMMA-RAY BURST; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; 25 APRIL 1998; IA SUPERNOVAE; LIGHT CURVES; INFRARED OBSERVATIONS; OPTICAL PHOTOMETRY; NEBULAR SPECTRA; IB SUPERNOVAE; 2002AP AB Ultraviolet, optical, and near-infrared photometry and optical spectroscopy of the broad-lined Type Ic supernova (SN) 2009bb are presented, following the flux evolution from -10 to +285 days past B-band maximum. Thanks to the very early discovery, it is possible to place tight constraints on the SN explosion epoch. The expansion velocities measured from near maximum spectra are found to be only slightly smaller than those measured from spectra of the prototype broad-lined SN 1998bw associated with GRB 980425. Fitting an analytical model to the pseudobolometric light curve of SN 2009bb suggests that 4.1 +/- 1.9M(circle dot) of material was ejected with 0.22 +/- 0.06 M-circle dot of it being Ni-56. The resulting kinetic energy is 1.8 +/- 0.7 x 10(52) erg. This, together with an absolute peak magnitude of M-B = -18.36 +/- 0.44, places SN 2009bb on the energetic and luminous end of the broad-lined Type Ic (SN Ic) sequence. Detection of helium in the early time optical spectra accompanied with strong radio emission and high metallicity of its environment makes SN 2009bb a peculiar object. Similar to the case for gamma-ray bursts (GRBs), we find that the bulk explosion parameters of SN 2009bb cannot account for the copious energy coupled to relativistic ejecta, and conclude that another energy reservoir (a central engine) is required to power the radio emission. Nevertheless, the analysis of the SN 2009bb nebular spectrum suggests that the failed GRB detection is not imputable to a large angle between the line-of-sight and the GRB beamed radiation. Therefore, if a GRB was produced during the SN 2009bb explosion, it was below the threshold of the current generation of gamma-ray instruments. C1 [Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Pignata, Giuliano; Anderson, J. P.; Folatelli, Gaston; Foerster, Francisco; Hamuy, Mario; Maza, Jose] Univ Chile, Dept Astron, Santiago, Chile. [Stritzinger, Maximilian; Phillips, M. M.; Morrell, Nidia; Boldt, Luis; Campillay, Abdo; Contreras, Carlos; Gonzalez, Sergio; Krzeminski, Wojtek; Roth, Miguel; Salgado, Francisco] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, Maximilian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Stritzinger, Maximilian] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Soderberg, Alicia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Mazzali, Paolo] Scuola Normale Super Pisa, I-56127 Pisa, Italy. [Mazzali, Paolo] INAF Oss Astron Padova, I-35122 Padua, Italy. [Contreras, Carlos] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Levesque, Emily M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Rest, Armin] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Crain, J. Adam; Foster, Andrew C.; Haislip, Joshua B.; Ivarsen, Kevin M.; LaCluyze, Aaron P.; Nysewander, Melissa C.; Reichart, Daniel E.] Univ N Carolina, Chapel Hill, NC 27599 USA. RP Pignata, G (reprint author), Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile. RI Folatelli, Gaston/A-4484-2011; Hamuy, Mario/G-7541-2016; Maza, Jose/I-5722-2016; OI Maza, Jose/0000-0003-2068-1328; stritzinger, maximilian/0000-0002-5571-1833 FU Comite Mixto ESO-Gobierno de Chile; FONDECYT [11090421, 1060808]; Programa Bicentenario de Ciencia y Tecnologia de CONICYT [P06-045-F]; Centro de Astrofisica FONDAP [15010003]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; Danish NSF; National Science Foundation (NSF) [AST-0306969] FX A special thanks to the Gemini-South staff for their efforts in obtaining data for our spectroscopic program. G.P. acknowledges support by the Proyecto FONDECYT 11090421 and from Comite Mixto ESO-Gobierno de Chile. M.H. acknowledges support from FONDECYT through grant 1060808. G.P., M.H., and J.M. acknowledge support from the Millennium Center for Supernova Science through grant P06-045-F funded by "Programa Bicentenario de Ciencia y Tecnologia de CONICYT," "Programa Iniciativa Cientifica Milenio de MIDEPLAN." G.P., M.H., and J.M. acknowledge partial support from Centro de Astrofisica FONDAP 15010003 and by Fondecyt through grant 1060808 from the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). The Dark Cosmology Centre is funded by the Danish NSF. This material is based upon work supported by the National Science Foundation (NSF) under grant AST-0306969. This paper is based on observations obtained at the Gemini Observatory, Cerro Pachon, Chile (Gemini Programs GS-2009A-Q-17 and GS-2009A-Q-43). We have made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 75 TC 37 Z9 37 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 FEB 10 PY 2011 VL 728 IS 1 AR 14 DI 10.1088/0004-637X/728/1/14 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500014 ER PT J AU Testa, P Reale, F Landi, E DeLuca, EE Kashyap, V AF Testa, Paola Reale, Fabio Landi, Enrico DeLuca, Edward E. Kashyap, Vinay TI TEMPERATURE DISTRIBUTION OF A NON-FLARING ACTIVE REGION FROM SIMULTANEOUS HINODE XRT AND EIS OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: abundances; Sun: activity; Sun: corona; Sun: UV radiation; Sun: X-rays; gamma rays; techniques: spectroscopic ID ULTRAVIOLET IMAGING SPECTROMETER; X-RAY TELESCOPE; EMISSION-LINES; CORONAL LOOPS; DENSITY STRUCTURE; ATOMIC DATABASE; PLASMA TEMPERATURE; SOLAR CORONA; QUIET-SUN; FUNDAMENTAL LIMITATIONS AB We analyze coordinated Hinode X-ray Telescope (XRT) and Extreme Ultraviolet Imaging Spectrometer (EIS) observations of a non-flaring active region to investigate the thermal properties of coronal plasma taking advantage of the complementary diagnostics provided by the two instruments. In particular, we want to explore the presence of hot plasma in non-flaring regions. Independent temperature analyses from the XRT multi-filter data set, and the EIS spectra, including the instrument entire wavelength range, provide a cross-check of the different temperature diagnostics techniques applicable to broadband and spectral data, respectively, and insights into cross-calibration of the two instruments. The emission measure distributions, (EM(T)), we derive from the two data sets have similar width and peak temperature, but show a systematic shift of the absolute values, the EIS (EM(T)) being smaller than the XRT (EM(T)) by approximately a factor two. We explore possible causes of this discrepancy, and we discuss the influence of the assumptions for the plasma element abundances. Specifically, we find that the disagreement between the results from the two instruments is significantly mitigated by assuming chemical composition closer to the solar photospheric composition rather than the often adopted "coronal" composition. We find that the data do not provide conclusive evidence on the high temperature (log T (K) greater than or similar to 6.5) tail of the plasma temperature distribution, however, suggesting its presence to a level in agreement with recent findings for other non-flaring regions. C1 [Testa, Paola; DeLuca, Edward E.; Kashyap, Vinay] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Reale, Fabio] Univ Palermo, Sez Astron, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy. [Reale, Fabio] INAF Osservatario Astron Palermo, I-90134 Palermo, Italy. [Landi, Enrico] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Testa, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu RI Landi, Enrico/H-4493-2011; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Reale, Fabio/0000-0002-1820-4824 FU NASA [NNM07AB07C]; Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI) [I/015/07/0]; [NNH06CD24C]; [NNH09AL49I] FX We thank P. Grigis and J. Drake for useful discussions. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and the NSC (Norway). P. T. and E. E. D. were supported by NASA contract NNM07AB07C to the Smithsonian Astrophysical Observatory. F. R. acknowledges support from Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI), contract I/015/07/0. The work of Enrico Landi is supported by NNH06CD24C, NNH09AL49I, and other NASA grants. NR 56 TC 36 Z9 36 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 30 DI 10.1088/0004-637X/728/1/30 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500030 ER PT J AU Wake, DA Whitaker, KE Labbe, I van Dokkum, PG Franx, M Quadri, R Brammer, G Kriek, M Lundgren, BF Marchesini, D Muzzin, A AF Wake, David A. Whitaker, Katherine E. Labbe, Ivo van Dokkum, Pieter G. Franx, Marijn Quadri, Ryan Brammer, Gabriel Kriek, Mariska Lundgren, Britt F. Marchesini, Danilo Muzzin, Adam TI GALAXY CLUSTERING IN THE NEWFIRM MEDIUM BAND SURVEY: THE RELATIONSHIP BETWEEN STELLAR MASS AND DARK MATTER HALO MASS AT 1 < z < 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; galaxies: halos; large-scale structure of universe ID DIGITAL SKY SURVEY; DISTANT RED GALAXIES; VLT DEEP SURVEY; LARGE-SCALE STRUCTURE; LYMAN-BREAK GALAXIES; K-SELECTED GALAXIES; INFRARED SPECTROSCOPIC SURVEY; STAR-FORMING GALAXIES; GOODS-MUSIC SAMPLE; OCCUPATION DISTRIBUTION AB We present an analysis of the clustering of galaxies as a function of their stellar mass at 1 < z < 2 using data from the NEWFIRM Medium Band Survey (NMBS). The precise photometric redshifts and stellar masses that the NMBS produces allow us to define a series of stellar mass limited samples of galaxies more massive than 7 x 10(9) M-circle dot, 1 x 10(10) M-circle dot, and 3 x 10(10) M-circle dot in three redshift intervals centered on z = 1.1, 1.5, and 1.9, respectively. In each redshift interval, we show that there exists a strong dependence of clustering strength on the stellar mass limit of the sample, with more massive galaxies showing a higher clustering amplitude on all scales. We further interpret our clustering measurements in the ACDM cosmological context using the halo model of galaxy clustering. We show that the typical halo mass of both central and satellite galaxies increases with stellar mass, whereas the satellite fraction decreases with stellar mass, qualitatively the same as is seen at z < 1. We see little evidence of any redshift dependence in the relationship between stellar mass and halo mass over our narrow redshift range. However, when we compare our measurements with similar ones at z similar or equal to 0, we see clear evidence for a change in this relation. If we assume a universal baryon fraction, the ratio of stellar mass to halo mass reveals the fraction of baryons that have been converted to stars. We see that the peak in this star formation efficiency for central galaxies shifts to higher halo masses at higher redshift, moving from similar or equal to 7 x 10(11) h(-1) M-circle dot at z similar or equal to 0 to similar or equal to 3 x 10(12) h(-1) M-circle dot at z similar or equal to 1.5, revealing evidence of "halo downsizing." Finally, we show that for highly biased galaxy populations at z > 1 there may be a discrepancy between the space density and clustering predicted by the halo model and the measured clustering and space density. This could imply that there is a problem with one or more ingredient of the halo model at these redshifts, for instance, the halo bias relation may not yet be precisely calibrated at high halo masses or galaxies may not be distributed within halos following a Navarro-Frenk-White profile. C1 [Wake, David A.; Whitaker, Katherine E.; van Dokkum, Pieter G.; Brammer, Gabriel; Lundgren, Britt F.; Muzzin, Adam] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Labbe, Ivo; Quadri, Ryan] Carnegie Observ, Pasadena, CA 91101 USA. [Franx, Marijn; Quadri, Ryan] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Brammer, Gabriel] European So Observ, Santiago 19, Chile. [Kriek, Mariska] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Wake, DA (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA. FU NSF [AST-0449678, AST-0807974] FX D.A.W. thanks Ravi Sheth, Zheng Zheng, Michael Brown, Carlton Baugh, Richard Bower, Scott Croom, Darren Croton, and Frank van den Bosch for helpful discussions on this work. Ron Probst and the NEWFIRM team are thanked for their work on the instrument and help during the observations. We used the HyperLeda database (http://leda.univ-lyon1.fr). This paper is partly based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. We thank the CARS team for providing us with their reduced CFHT mosaics. Support from NSF grants AST-0449678 and AST-0807974 is gratefully acknowledged. NR 132 TC 89 Z9 89 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 FEB 10 PY 2011 VL 728 IS 1 AR 46 DI 10.1088/0004-637X/728/1/46 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500046 ER PT J AU Yan, RB Ho, LC Newman, JA Coil, AL Willmer, CNA Laird, ES Georgakakis, A Aird, J Barmby, P Bundy, K Cooper, MC Davis, M Faber, SM Fang, TT Griffith, RL Koekemoer, AM Koo, DC Nandra, K Park, SQ Sarajedini, VL Weiner, BJ Willner, SP AF Yan, Renbin Ho, Luis C. Newman, Jeffrey A. Coil, Alison L. Willmer, Christopher N. A. Laird, Elise S. Georgakakis, Antonis Aird, James Barmby, Pauline Bundy, Kevin Cooper, Michael C. Davis, Marc Faber, S. M. Fang, Taotao Griffith, Roger L. Koekemoer, Anton M. Koo, David C. Nandra, Kirpal Park, Shinae Q. Sarajedini, Vicki L. Weiner, Benjamin J. Willner, S. P. TI AEGIS: DEMOGRAPHICS OF X-RAY AND OPTICALLY SELECTED ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: fundamental parameters; galaxies: nuclei; galaxies: Seyfert; galaxies: statistics ID DIGITAL SKY SURVEY; GALAXY REDSHIFT SURVEY; STAR-FORMING GALAXIES; EMISSION-LINE GALAXIES; SEYFERT 2 GALAXIES; FORMATION RATE INDICATOR; EXTENDED GROTH STRIP; 2-10 KEV LUMINOSITY; DEEP FIELD-SOUTH; HOST GALAXIES AB We develop a new diagnostic method to classify galaxies into active galactic nucleus (AGN) hosts, star-forming galaxies, and absorption-dominated galaxies by combining the [OIII]/H beta ratio with rest-frame U-B color. This can be used to robustly select AGNs in galaxy samples at intermediate redshifts (z < 1). We compare the result of this optical AGN selection with X-ray selection using a sample of 3150 galaxies with 0.3 < z < 0.8 and I-AB < 22, selected from the DEEP2 Galaxy Redshift Survey and the All-wavelength Extended Groth Strip International Survey. Among the 146 X-ray sources in this sample, 58% are classified optically as emission-line AGNs, the rest as star-forming galaxies or absorption-dominated galaxies. The latter are also known as "X-ray bright, optically normal galaxies" (XBONGs). Analysis of the relationship between optical emission lines and X-ray properties shows that the completeness of optical AGN selection suffers from dependence on the star formation rate and the quality of observed spectra. It also shows that XBONGs do not appear to be a physically distinct population from other X-ray detected, emission-line AGNs. On the other hand, X-ray AGN selection also has strong bias. About 2/3 of all emission-line AGNs at L-bol > 10(44) erg s(-1) in our sample are not detected in our 200 ks Chandra images, most likely due to moderate or heavy absorption by gas near the AGN. The 2-7 keV detection rate of Seyfert 2s at z similar to 0.6 suggests that their column density distribution and Compton-thick fraction are similar to that of local Seyferts. Multiple sample selection techniques are needed to obtain as complete a sample as possible. C1 [Yan, Renbin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Coil, Alison L.; Aird, James] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA. [Coil, Alison L.; Aird, James] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Laird, Elise S.; Nandra, Kirpal] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Georgakakis, Antonis] Natl Observ Athens, V Paulou 11532, Greece. [Georgakakis, Antonis] Natl Observ Athens, I Metaxa 11532, Greece. [Barmby, Pauline] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Bundy, Kevin; Davis, Marc] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA. [Davis, Marc] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Faber, S. M.; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Griffith, Roger L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Park, Shinae Q.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sarajedini, Vicki L.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Yan, RB (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM yan@astro.utoronto.ca RI Georgakakis, Antonis/K-4457-2013; Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Weiner, Benjamin/0000-0001-6065-7483; Georgakakis, Antonis/0000-0002-3514-2442; Koekemoer, Anton/0000-0002-6610-2048 FU NSF [AST00-71198, AST00-71048, AST05-07483, AST05-07428, AST08-07630, AST08-08133]; NASA [G05-6141A, GO8-9129A]; STFC; Alfred P. Sloan Foundation; National Aeronautics and Space Administration; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; University of Chicago; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; University of Pittsburgh; Princeton University; United States Naval Observatory; University of Washington FX This study makes use of data from AEGIS, a multiwavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA, and other telescopes and supported in part by the NSF, NASA, and the STFC. The AEGIS Web site is http://aegis.ucolick.org. The DEEP2 Web site is http://deep.berkeley.edu/.; The project was supported in part by the NSF Grants AST00-71198, AST00-71048, AST05-07483, AST05-07428, AST08-07630, AST08-08133, and NASA Chandra Grants G05-6141A and GO8-9129A. This research made use of the NASA Astrophysics Data System, and employed open-source software written and maintained by David Schlegel, Douglas Finkbeiner, and others.; Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, the University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. NR 108 TC 49 Z9 49 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 38 DI 10.1088/0004-637X/728/1/38 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500038 ER PT J AU ZuHone, JA AF ZuHone, J. A. TI A PARAMETER SPACE EXPLORATION OF GALAXY CLUSTER MERGERS. I. GAS MIXING AND THE GENERATION OF CLUSTER ENTROPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; hydrodynamics; methods: numerical; X-rays: galaxies: clusters ID X-RAY-CLUSTERS; ANISOTROPIC THERMAL CONDUCTION; MATTER VELOCITY ANISOTROPY; DARK-MATTER; COOLING FLOWS; INTRACLUSTER MEDIUM; HYDRODYNAMIC SIMULATIONS; NUMERICAL SIMULATIONS; MASS-DISTRIBUTION; MERGING CLUSTERS AB We present a high-resolution set of adiabatic binary galaxy cluster merger simulations using FLASH. These are the highest resolution simulations to date of such mergers using an adaptive mesh refinement grid-based code with Eulerian hydrodynamics. In this first paper in a series, we investigate the effects of merging on the entropy of the hot intracluster gas, specifically with regard to the ability of merging to heat and disrupt cluster "cool cores." We find, in line with recent works, that the effect of fluid instabilities that are well resolved in grid-based codes is to significantly mix the gases of the two clusters and to significantly increase the entropy of the gas of the final merger remnant. This result is characteristic of mergers over a range of initial mass ratio and impact parameter. In line with this, we find that the kinetic energy associated with random motions is higher in our merger remnants which have high-entropy floors, indicating that the motions have efficiently mixed the gas and heated the cluster core with gas of initially high entropy. We examine the implications of this result for the maintenance of high-entropy floors in the centers of galaxy clusters and the derivation of the properties of dark matter from the thermal properties of the X-ray-emitting gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP ZuHone, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Chandra grant [GO8-9128X]; ASC/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago FX J.A.Z. is grateful to Don Lamb, Paul Ricker, Maxim Markevitch, Ryan Johnson, Eric Hallman, Ian Parrish, and Andrey Kravtsov for discussions and advice. Calculations were performed using the computational resources of Argonne National Laboratory and Lawrence Livermore National Laboratory. J.A.Z. is supported under Chandra grant GO8-9128X. The software used in this work was in part developed by the DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago. NR 98 TC 28 Z9 28 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2011 VL 728 IS 1 AR 54 DI 10.1088/0004-637X/728/1/54 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712GY UT WOS:000286655500054 ER PT J AU Li, ZY Garcia, MR Forman, WR Jones, C Kraft, RP Lal, DV Murray, SS Wang, QD AF Li, Zhiyuan Garcia, Michael R. Forman, William R. Jones, Christine Kraft, Ralph P. Lal, Dharam V. Murray, Stephen S. Wang, Q. Daniel TI THE MURMUR OF THE HIDDEN MONSTER: CHANDRA'S DECADAL VIEW OF THE SUPERMASSIVE BLACK HOLE IN M31 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (M31); galaxies: nuclei; X-rays: galaxies ID SAGITTARIUS-A-ASTERISK; NUCLEAR RADIO-SOURCE; X-RAY; NEARBY GALAXIES; GALACTIC-CENTER; DOMINATED ACCRETION; FUNDAMENTAL PLANE; XMM-NEWTON; FLARES; VARIABILITY AB The Andromeda galaxy (M31) hosts a central supermassive black hole (SMBH), known as M31*, which is remarkable for its mass (similar to 10(8) M-circle dot) and extreme radiative quiescence. Over the past decade, the Chandra X-Ray Observatory has pointed to the center of M31 similar to 100 times and accumulated a total exposure of similar to 900 ks. Based on these observations, we present an X-ray study of a highly variable source that we associate with M31* based on positional coincidence. We find that M31* remained in a quiescent state from late 1999 to 2005, exhibiting an average 0.5-8 keV luminosity less than or similar to 10(36) erg s(-1), or only similar to 10(-10) of its Eddington luminosity. We report the discovery of an outburst that occurred on 2006 January 6 during which M31* radiated at similar to 4.3 x 10(37) erg s(-1). After the outburst, M31* entered a more active state that apparently lasts to the present, which is characterized by frequent flux variability around an average luminosity of similar to 4.8 x 10(36) erg s(-1). These flux variations are similar to the X-ray flares found in the SMBH of our Galaxy (Sgr A*), making M31* the second SMBH known to exhibit recurrent flares. Future coordinated X-ray/radio observations will provide useful constraints on the physical origin of the flaring emission and help rule out a possible stellar origin of the X-ray source. C1 [Li, Zhiyuan; Garcia, Michael R.; Forman, William R.; Jones, Christine; Kraft, Ralph P.; Lal, Dharam V.; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21205 USA. [Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Li, ZY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zyli@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 FU SAO [GO9-0100X, GO0-11098] FX We are grateful to Feng Yuan for valuable discussions. Z.L. thanks Jun Lin and Jeffrey McClintock for useful comments, and the Chandra calibration team, in particular, Jennifer Posson-Brown, Frank Primini, and Aneta Siemiginowska, for suggestions on the usage of HRC data and Sherpa. This work is supported by SAO grants GO9-0100X and GO0-11098. NR 38 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2011 VL 728 IS 1 AR L10 DI 10.1088/2041-8205/728/1/L10 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 711WV UT WOS:000286623000010 ER PT J AU Snyder, GF Hopkins, PF Hernquist, L AF Snyder, Gregory F. Hopkins, Philip F. Hernquist, Lars TI RELATION BETWEEN GLOBULAR CLUSTERS AND SUPERMASSIVE BLACK HOLES IN ELLIPTICALS AS A MANIFESTATION OF THE BLACK HOLE FUNDAMENTAL PLANE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE black hole physics; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation ID EARLY-TYPE GALAXIES; MERGER REMNANTS; GALACTIC NUCLEI; EXTRA LIGHT; INTRINSIC SCATTER; HOST GALAXIES; SYSTEMS; MASS; DISSIPATION; QUASARS AB We analyze the relation between the mass of the central supermassive black hole (M-BH) and the number of globular clusters (N-GC) in elliptical galaxies and bulges as a ramification of the black hole fundamental plane, the theoretically predicted and observed multi-variable correlation between M-BH and bulge binding energy. Although the tightness of the M-BH-N-GC correlation suggests an unlikely causal link between supermassive black holes and globular clusters (GCs), such a correspondence can exhibit small scatter even if the physical relationship is indirect. We show that the relatively small scatter of the M-BH-N-GC relation owes to the mutual residual correlation of M-BH and N-GC with stellar mass when the velocity dispersion is held fixed. Thus, present observations lend evidence for feedback-regulated models in which the bulge binding energy is most important; they do not necessarily imply any "special" connection between GCs and M-BH. This raises the question of why N-GC traces the formation of ellipticals and bulges sufficiently well to be correlated with binding energy. C1 [Snyder, Gregory F.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Snyder, GF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 47 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2011 VL 728 IS 1 AR L24 DI 10.1088/2041-8205/728/1/L24 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 711WV UT WOS:000286623000024 ER PT J AU Irwin, RP Craddock, RA Howard, AD Flemming, HL AF Irwin, Rossman P., III Craddock, Robert A. Howard, Alan D. Flemming, Holly L. TI Topographic influences on development of Martian valley networks SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID EARLY MARS; AQUEOUS SEDIMENTATION; MARGARITIFER SINUS; FLUVIAL PROCESSES; DRAINAGE BASINS; EVOLUTION; CHANNELS; SURFACE; ORIGIN; PRECIPITATION AB Some morphometric differences between terrestrial and Martian valley networks may reflect the precursor topography on Mars, particularly impact basins or tectonic slopes. To evaluate these possible influences, we mapped highland watersheds in nine study areas that sample a range of geographic and topographic settings. We collected data including latitude, longitude, watershed length, divide and terminal elevations, watershed relief and slope, slope orientation, and qualitative descriptors including whether a drainage basin was open or closed. The longest valley networks and most overflowed basins occur on preexisting intercrater slopes of 0.1-1 degrees, particularly on north facing slopes associated with the crustal dichotomy. The control of watershed length by earlier Noachian topographic features, which the relict networks did not significantly modify, suggests that the Early to Middle Noachian geomorphic environment was nominally much drier than the later Noachian to Hesperian transition. The distribution of fluvial valleys and likely orographic effects created by the crustal dichotomy suggest that evaporation from the northern lowlands was an important source of atmospheric humidity over short time scales. Much of the highland plateau consists of smaller enclosed watersheds, which (along with cooler temperatures) detained surface water at high elevations, lengthening or impeding the global water cycle. Ponding and evaporation may have partly offset a continentality effect of the highland landmass. Prolonged modification of the intercrater geomorphic surface prior to incision of valley networks included substantial weathering, reduction of relief, and gravity-driven sediment transport, indicating a long-term role for surface water in a transport-limited, arid to hyperarid Noachian paleoclimate. C1 [Irwin, Rossman P., III] Planetary Sci Inst, Tucson, AZ USA. [Craddock, Robert A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Flemming, Holly L.] MDA Informat Syst Inc, Gaithersburg, MD 20878 USA. RP Irwin, RP (reprint author), Planetary Sci Inst, Tucson, AZ USA. EM irwin@psi.edu RI Craddock, Robert/B-3884-2013; OI Howard, Alan/0000-0002-5423-1600 NR 65 TC 18 Z9 18 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 10 PY 2011 VL 116 AR E02005 DI 10.1029/2010JE003620 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 721AV UT WOS:000287324700001 ER PT J AU Capak, PL Riechers, D Scoville, NZ Carilli, C Cox, P Neri, R Robertson, B Salvato, M Schinnerer, E Yan, L Wilson, GW Yun, M Civano, F Elvis, M Karim, A Mobasher, B Staguhn, JG AF Capak, Peter L. Riechers, Dominik Scoville, Nick Z. Carilli, Chris Cox, Pierre Neri, Roberto Robertson, Brant Salvato, Mara Schinnerer, Eva Yan, Lin Wilson, Grant W. Yun, Min Civano, Francesca Elvis, Martin Karim, Alexander Mobasher, Bahram Staguhn, Johannes G. TI A massive protocluster of galaxies at a redshift of z approximate to 5.3 SO NATURE LA English DT Article ID LYMAN-BREAK GALAXIES; SOURCE CATALOG; MOLECULAR GAS; SUBMILLIMETER GALAXIES; COSMOS SURVEY; EVOLUTION; QUASARS; Z-SIMILAR-TO-6; POPULATION; HISTORY AB Massive clusters of galaxies have been found that date from as early as 3.9 billion years(1) (3.9 Gyr; z = 1.62) after the Big Bang, containing stars that formed at even earlier epochs(2,3). Cosmological simulations using the current cold dark matter model predict that these systems should descend from 'protoclusters'-early overdensities of massive galaxies that merge hierarchically to form a cluster(4,5). These protocluster regions themselves are built up hierarchically and so are expected to contain extremely massive galaxies that can be observed as luminous quasars and starbursts(4-6). Observational evidence for this picture, however, is sparse because high-redshift protoclusters are rare and difficult to observe(6,7). Here we report a protocluster region that dates from 1 Gyr (z = 55.3) after the Big Bang. This cluster of massive galaxies extends over more than 13 megaparsecs and contains a luminous quasar as well as a system rich in molecular gas(8). These massive galaxies place a lower limit of more than 4 x 10(11) solar masses of dark and luminous matter in this region, consistent with that expected from cosmological simulations for the earliest galaxy clusters(4,5,7). C1 [Capak, Peter L.; Yan, Lin] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Riechers, Dominik; Scoville, Nick Z.; Robertson, Brant] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Carilli, Chris] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Cox, Pierre; Neri, Roberto] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Salvato, Mara] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Schinnerer, Eva; Karim, Alexander] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Wilson, Grant W.; Yun, Min] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Civano, Francesca; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Staguhn, Johannes G.] Johns Hopkins Univ, Lab Observat Cosmol, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Capak, PL (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM capak@astro.caltech.edu OI Schinnerer, Eva/0000-0002-3933-7677 FU NASA; NSF FX These results are based on observations with: the W. M. Keck Observatory, the IRAM Plateau de Bure Interferometer, the IRAM 30-m telescope with the GISMO 2-mm camera, the Chandra X-ray Observatory, the Subaru Telescope, the Hubble Space Telescope, the Canada-France-Hawaii Telescope with WIRCam and MegaPrime, the United Kingdom Infrared Telescope, the Spitzer Space Telescope, the Smithsonian Submillimeter Array Telescope, the James Clerk Maxwell Telescope with the AzTEC 1.1 mm camera, and the National Radio Astronomy Observatory's Very Large Array. D. R. and B. R. acknowledge support from NASA through Hubble Fellowship grants awarded by the Space Telescope Science Institute. P. L. C. and N.Z.S. acknowledge grant support from NASA. G. W. W., M.Y. and J.G.S. acknowledge grant support from the NSF. NR 28 TC 123 Z9 124 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 10 PY 2011 VL 470 IS 7333 BP 233 EP 235 DI 10.1038/nature09681 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 718RQ UT WOS:000287144200038 PM 21228776 ER PT J AU Cardenas, M Grajales, A Sierra, R Rojas, A Gonzalez-Almario, A Vargas, A Marin, M Fermin, G Lagos, LE Grunwald, NJ Bernal, A Salazar, C Restrepo, S AF Cardenas, Martha Grajales, Alejandro Sierra, Roberto Rojas, Alejandro Gonzalez-Almario, Adriana Vargas, Angela Marin, Mauricio Fermin, Gustavo Lagos, Luz E. Gruenwald, Niklaus J. Bernal, Adriana Salazar, Camilo Restrepo, Silvia TI Genetic diversity of Phytophthora infestans in the Northern Andean region SO BMC GENETICS LA English DT Article ID LATE BLIGHT; POPULATION-STRUCTURE; CENTRAL MEXICO; PHYLOGENETIC ANALYSIS; MAXIMUM-LIKELIHOOD; STATISTICAL-METHOD; CULTIVATED POTATO; SOLANACEOUS HOSTS; DNA POLYMORPHISM; EFFECTOR AVR3A AB Background: Phytophthora infestans (Mont.) de Bary, the causal agent of potato late blight, is responsible for tremendous crop losses worldwide. Countries in the northern part of the Andes dedicate a large proportion of the highlands to the production of potato, and more recently, solanaceous fruits such as cape gooseberry (Physalis peruviana) and tree tomato (Solanum betaceum), all of which are hosts of this oomycete. In the Andean region, P. infestans populations have been well characterized in Ecuador and Peru, but are poorly understood in Colombia and Venezuela. To understand the P. infestans population structure in the Northern part of the Andes, four nuclear regions (ITS, Ras, beta-tubulin and Avr3a) and one mitochondrial (Cox1) region were analyzed in isolates of P. infestans sampled from different hosts in Colombia and Venezuela. Results: Low genetic diversity was found within this sample of P. infestans isolates from crops within several regions of Colombia and Venezuela, revealing the presence of clonal populations of the pathogen in this region. We detected low frequency heterozygotes, and their distribution patterns might be a consequence of a high migration rate among populations with poor effective gene flow. Consistent genetic differentiation exists among isolates from different regions. Conclusions: The results here suggest that in the Northern Andean region P. infestans is a clonal population with some within-clone variation. P. infestans populations in Venezuela reflect historic isolation that is being reinforced by a recent self-sufficiency of potato seeds. In summary, the P. infestans population is mainly shaped by migration and probably by the appearance of variants of key effectors such as Avr3a. C1 [Cardenas, Martha; Grajales, Alejandro; Sierra, Roberto; Rojas, Alejandro; Gonzalez-Almario, Adriana; Vargas, Angela; Bernal, Adriana; Restrepo, Silvia] Univ Los Andes, Bogota, Colombia. [Marin, Mauricio] Univ Nacl Colombia, Medellin, Antioquia, Colombia. [Fermin, Gustavo] Univ Los Andes, Merida, Venezuela. [Lagos, Luz E.] Univ Narino, Pasto, Narino, Colombia. [Gruenwald, Niklaus J.] ARS, USDA, Corvallis, OR USA. [Salazar, Camilo] Smithsonian Trop Res Inst, Panama City, Panama. [Salazar, Camilo] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. RP Cardenas, M (reprint author), Univ Los Andes, Bogota, Colombia. EM martcard@unlandes.edu.co RI Salazar, camilo/A-1647-2010; Grunwald, Niklaus/K-6041-2013; Rojas, J Alejandro/D-9273-2016; OI Salazar, camilo/0000-0001-9217-6588; Grunwald, Niklaus/0000-0003-1656-7602; Rojas, J Alejandro/0000-0001-5492-5963; Marin, Mauricio/0000-0001-7123-2747; Restrepo, Silvia/0000-0001-9016-1040; Sierra, Roberto/0000-0002-8657-1781 FU Facultad de Ciencias of the Universidad de Los Andes; FONACIT [2004000490-26140]; CDCHT-ULA [C-1260-04-01-B]; USDA Agricultural Research Service [5358-22000-034-00 D] FX In Colombia this work was financed by the Facultad de Ciencias of the Universidad de Los Andes. In Venezuela, the study was financed by FONACIT (Grant 2004000490-26140) and CDCHT-ULA (Grant C-1260-04-01-B). NJG was supported by funds from USDA Agricultural Research Service CRIS Project 5358-22000-034-00 D. NR 51 TC 14 Z9 19 U1 1 U2 17 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2156 J9 BMC GENET JI BMC Genet. PD FEB 9 PY 2011 VL 12 AR 23 DI 10.1186/1471-2156-12-23 PG 13 WC Genetics & Heredity SC Genetics & Heredity GA 730GZ UT WOS:000288023100001 PM 21303555 ER PT J AU Mah, CL AF Mah, Christopher L. TI Taxonomy of high-latitude Goniasteridae (Subantarctic & Antarctic): one new genus, and three new species with an overview and key to taxa SO ZOOTAXA LA English DT Article DE Goniasteridae; Asteroidea; Antarctic; subantarctic; Southern Ocean; taxonomy; New Zealand ID OCEAN ACIDIFICATION; ASTEROIDEA; ECHINODERMATA; TEMPERATURE; SYSTEMATICS; PHYLOGENY; INCREASE AB A review of high-latitude Goniasteridae south of 50 degrees S is presented, including a key to species, figures and taxonomic descriptions of all species with a brief taxonomic summary for all genera. Nineteen species in 11 genera are reviewed. Eratosaster jenae nov. gen and sp., Chitonaster trangae nov. sp., and Pillsburiaster calvus nov. sp. are described. Several taxa, including Chitonaster, have not been reviewed since their initial description and revision of the group has clarified taxonomic boundaries between species. The genus Pentoplia is a junior synonym of Chitonaster. Rarely encountered species, synonyms, and range extensions are reported for multiple species. C1 Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Mah, CL (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, MRC-163,POB 37012, Washington, DC 20560 USA. EM mahch@si.edu FU OPP Antarctic [0631245]; USARP [ANT-0646308] FX Thanks to Kate Neil, National Institute of Water and Atmosphere (NIWA) in Wellington, New Zealand and Tim O'Hara, Museum Victoria for photography and specimen assistance. I am grateful to the following for their specimen and collections-based assistance: Jennifer Hammock, Trang Ngyuen, and the personnel of the United States Antarctic Research Program, Christina Piotrowski-California Academy of Sciences, Susan Lockhart-US AMLR (NOAA), Paul Greenhall, USNM, and Marc Eleaume, Nadia Ameziane, and Lenaig Hemery for assistance at the Museum national d'Histoire naturelle in Paris France. Funding was provided by an OPP Antarctic postdoctoral fellowship (0631245) and USARP (ANT-0646308) contracts. NR 42 TC 3 Z9 3 U1 1 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 FEB 7 PY 2011 IS 2759 BP 1 EP 48 PG 48 WC Zoology SC Zoology GA 716NM UT WOS:000286980700001 ER PT J AU Solomon, SE Lopes, CT Mueller, UG Rodrigues, A Sosa-Calvo, J Schultz, TR Vasconcelos, HL AF Solomon, Scott E. Lopes, Caue T. Mueller, Ulrich G. Rodrigues, Andre Sosa-Calvo, Jeffrey Schultz, Ted R. Vasconcelos, Heraldo L. TI Nesting biology and fungiculture of the fungus-growing ant, Mycetagroicus cerradensis: New light on the origin of higher-attine agriculture SO JOURNAL OF INSECT SCIENCE LA English DT Article DE Attini; Cerrado; evolutionary transitions; Leucocoprinus; molecular systematics; nest architecture ID BRAZILIAN CERRADO; FORMICIDAE; SYMBIOSIS; ARCHITECTURE; HYMENOPTERA; COEVOLUTION; GENUS; EMERY AB The genus Mycetagroicus is perhaps the least known of all fungus-growing ant genera, having been first described in 2001 from museum specimens. A recent molecular phylogenetic analysis of the fungus-growing ants demonstrated that Mycetagroicus is the sister to all higher attine ants (Trachymyrmex, Sericomyrmex, Acromyrmex, Pseudoatta, and Atta), making it of extreme importance for understanding the transition between lower and higher attine agriculture. Four nests of Mycetagroicus cerradensis near Uberlandia, Minas Gerais, Brazil were excavated, and fungus chambers for one were located at a depth of 3.5 meters. Based on its lack of gongylidia (hyphal-tip swellings typical of higher attine cultivars), and a phylogenetic analysis of the ITS rDNA gene region, M. cerradensis cultivates a lower attine fungus in Clade 2 of lower attine (G3) fungi. This finding refines a previous estimate for the origin of higher attine agriculture, an event that can now be dated at approximately 21-25 mya in the ancestor of extant species of Trachymyrmex and Sericomyrmex. C1 [Lopes, Caue T.; Vasconcelos, Heraldo L.] Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. [Mueller, Ulrich G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Rodrigues, Andre] State Univ Sao Paulo, Ctr Study Social Insects CEIS, BR-13506900 Rio Claro, SP, Brazil. [Sosa-Calvo, Jeffrey] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. [Solomon, Scott E.; Sosa-Calvo, Jeffrey; Schultz, Ted R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Solomon, SE (reprint author), Rice Univ, Dept Ecol & Evolutionary Biol, 6100 Main St,MS 170, Houston, TX 77005 USA. EM ses4@rice.edu; cauelopes@gmail.com; umueller@mail.utexas.edu; andrer@rc.unesp.br; sossajef@si.edu; schultzt@si.edu; heraldo@umuarama.ufu.br RI Rodrigues, Andre/B-8148-2012; Vasconcelos, Heraldo/C-3353-2013 OI Rodrigues, Andre/0000-0002-4164-9362; Vasconcelos, Heraldo/0000-0001-6969-7131 FU NSF [07012333, DEB-0639879, DEB-0110073, DEB-0431330, DEB-0949689]; Smithsonian Scholarly Studies Program; Smithsonian USS Restricted Endowment FX We would especially like to thank C.R.F. Brandao (Museu de Zoologia, Universidade de Sao Paulo) for the loan of material used in this study. We would also like to thank M. Bacci Jr. (Universidade Estadual Paulista, Rio Claro, SP) for his support and assistance for fieldwork in Brazil, S. Brady for providing dates for the origin of higher attine agriculture, A.S. Mikheyev for supplying the phylogram used in the left panel of Figure 2, and two anonymous reviewers for their helpful suggestions. This work was conducted under collecting permit Number 14789-1 issued by the Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais Renovaveis (IBAMA) and the Instituto Chico Mendes de Conservacao da Biodiversidade (ICMBio). This project was funded by NSF International Research Fellowship (IRFP) 07012333 to SES; NSF Grant DEB-0639879 to UGM; NSF Integrated Research Challenges in Environmental Biology (IRCEB) Grant DEB-0110073 to UGM, C. R. Currie, and TRS; NSF Assembling the Tree of Life (AToL) Grant DEB-0431330 to P. S. Ward, B. L. Fisher, S. G. Brady, and TRS; NSF DEB-0949689 to TRS, UGM, N.J. Mehdiabadi, C. W. Mitter, and A.S. Mikheyev; a Smithsonian Scholarly Studies Program grant to TRS and S.G. Brady; and a Smithsonian USS Restricted Endowment Grant to TRS. NR 37 TC 7 Z9 7 U1 0 U2 8 PU UNIV ARIZONA PI TUCSON PA LIBRARY C327, TUCSON, AZ 85721 USA SN 1536-2442 J9 J INSECT SCI JI J Insect Sci. PD FEB 4 PY 2011 VL 11 AR 12 PG 14 WC Entomology SC Entomology GA 717IK UT WOS:000287036700002 PM 21526926 ER PT J AU Carter, JA Fabrycky, DC Ragozzine, D Holman, MJ Quinn, SN Latham, DW Buchhave, LA Van Cleve, J Cochran, WD Cote, MT Endl, M Ford, EB Haas, MR Jenkins, JM Koch, DG Li, J Lissauer, JJ MacQueen, PJ Middour, CK Orosz, JA Rowe, JF Steffen, JH Welsh, WF AF Carter, Joshua A. Fabrycky, Daniel C. Ragozzine, Darin Holman, Matthew J. Quinn, Samuel N. Latham, David W. Buchhave, Lars A. Van Cleve, Jeffrey Cochran, William D. Cote, Miles T. Endl, Michael Ford, Eric B. Haas, Michael R. Jenkins, Jon M. Koch, David G. Li, Jie Lissauer, Jack J. MacQueen, Phillip J. Middour, Christopher K. Orosz, Jerome A. Rowe, Jason F. Steffen, Jason H. Welsh, William F. TI KOI-126: A Triply Eclipsing Hierarchical Triple with Two Low-Mass Stars SO SCIENCE LA English DT Article ID BINARY CM DRACONIS; MAGNETIC ACTIVITY; MAIN-SEQUENCE; EVOLUTION; MODELS; SCIENCE; SYSTEMS; RADII AB The Kepler spacecraft has been monitoring the light from 150,000 stars in its primary quest to detect transiting exoplanets. Here, we report on the detection of an eclipsing stellar hierarchical triple, identified in the Kepler photometry. KOI-126 [A, (B, C)], is composed of a low-mass binary [masses M(B) = 0.2413 +/- 0.0030 solar mass (M(circle dot)), M(C) = 0.2127 +/- 0.0026 M(circle dot); radii R(B) = 0.2543 +/- 0.0014 solar radius (R(circle dot)), R(C) = 0.2318 +/- 0.0013 R(circle dot); orbital period P(1) = 1.76713 +/- 0.00019 days] on an eccentric orbit about a third star (mass M(A) = 1.347 +/- 0.032 M(circle dot); radius R(A) = 2.0254 +/- 0.0098 R(circle dot); period of orbit around the low-mass binary P(2) = 33.9214 +/- 0.0013 days; eccentricity of that orbit e(2) = 0.3043 +/- 0.0024). The low-mass pair probe the poorly sampled fully convective stellar domain offering a crucial benchmark for theoretical stellar models. C1 [Carter, Joshua A.; Ragozzine, Darin; Holman, Matthew J.; Quinn, Samuel N.; Latham, David W.; Buchhave, Lars A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Van Cleve, Jeffrey; Cote, Miles T.; Haas, Michael R.; Jenkins, Jon M.; Koch, David G.; Li, Jie; Lissauer, Jack J.; Middour, Christopher K.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Austin, TX 78712 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Van Cleve, Jeffrey; Jenkins, Jon M.; Li, Jie; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Lissauer, Jack J.] Stanford Univ, Stanford, CA 94305 USA. [Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Middour, Christopher K.] Orbital Sci Corp, Dulles, VA 20166 USA. RP Carter, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jacarter@cfa.harvard.edu RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; OI Buchhave, Lars A./0000-0003-1605-5666; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [HF-51267.01-A, HF-51272.01-A, NAS 5-26555] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. J.A.C. and D. C. F. are Hubble Fellows and acknowledge support for this work by NASA through Hubble Fellowship grants HF-51267.01-A and HF-51272.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA under contract NAS 5-26555. J.A.C. is grateful for helpful discussions with P. Podsiadlowski, S. Rappaport, G. Torres, A. Levine, J. Winn, S. Seager, and T. Dupuy. J. F. R. is a NASA Postdoctoral Program Fellow. NR 26 TC 106 Z9 107 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 FEB 4 PY 2011 VL 331 IS 6017 BP 562 EP 565 DI 10.1126/science.1201274 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 715ZE UT WOS:000286933600047 PM 21224439 ER PT J AU Lissauer, JJ Fabrycky, DC Ford, EB Borucki, WJ Fressin, F Marcy, GW Orosz, JA Rowe, JF Torres, G Welsh, WF Batalha, NM Bryson, ST Buchhave, LA Caldwell, DA Carter, JA Charbonneau, D Christiansen, JL Cochran, W Desert, JM Dunham, EW Fanelli, MN Fortney, JJ Gautier, TN Geary, JC Gilliland, RL Haas, MR Hall, JR Holman, MJ Koch, DG Latham, DW Lopez, E McCauliff, S Miller, N Morehead, RC Quintana, EV Ragozzine, D Sasselov, D Short, DR Steffen, JH AF Lissauer, Jack J. Fabrycky, Daniel C. Ford, Eric B. Borucki, William J. Fressin, Francois Marcy, Geoffrey W. Orosz, Jerome A. Rowe, Jason F. Torres, Guillermo Welsh, William F. Batalha, Natalie M. Bryson, Stephen T. Buchhave, Lars A. Caldwell, Douglas A. Carter, Joshua A. Charbonneau, David Christiansen, Jessie L. Cochran, WilliamD. Desert, Jean-Michel Dunham, Edward W. Fanelli, Michael N. Fortney, Jonathan J. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Haas, Michael R. Hall, Jennifer R. Holman, Matthew J. Koch, David G. Latham, David W. Lopez, Eric McCauliff, Sean Miller, Neil Morehead, Robert C. Quintana, Elisa V. Ragozzine, Darin Sasselov, Dimitar Short, Donald R. Steffen, Jason H. TI A closely packed system of low-mass, low-density planets transiting Kepler-11 SO NATURE LA English DT Article ID EXTRASOLAR PLANETS; SUPER-EARTHS; STARS; PERFORMANCE; EVAPORATION; ISOCHRONES; DYNAMICS; NEPTUNES; JUPITERS; SCIENCE AB When an extrasolar planet passes in front of (transits) its star, its radius can be measured from the decrease in starlight and its orbital period from the time between transits. Multiple planets transiting the same star reveal much more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and orbital shapes, and the fraction of transiting planets observed as multiples has implications for the planarity of planetary systems. But few stars have more than one known transiting planet, and none has more than three. Here we report Kepler spacecraft observations of a single Sun-like star, which we call Kepler-11, that reveal six transiting planets, five with orbital periods between 10 and 47 days and a sixth planet with a longer period. The five inner planets are among the smallest for which mass and size have both been measured, and these measurements imply substantial envelopes of light gases. The degree of coplanarity and proximity of the planetary orbits imply energy dissipation near the end of planet formation. C1 [Lissauer, Jack J.; Rowe, Jason F.; Caldwell, Douglas A.; Christiansen, Jessie L.; Quintana, Elisa V.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.; Lopez, Eric; Miller, Neil] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Ford, Eric B.; Morehead, Robert C.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Fressin, Francois; Torres, Guillermo; Carter, Joshua A.; Charbonneau, David; Desert, Jean-Michel; Geary, John C.; Holman, Matthew J.; Latham, David W.; Ragozzine, Darin; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Orosz, Jerome A.; Welsh, William F.; Short, Donald R.] San Diego State Univ, San Diego, CA 92182 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Cochran, WilliamD.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Fanelli, Michael N.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hall, Jennifer R.; McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. EM jack.lissauer@nasa.gov; fabrycky@ucolick.org RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA [HF-51272.01-A, HF-51267.01-A]; STScl [NAS 5-26555] FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. We thank the many people who gave so generously of their time to make the Kepler mission a success. A. Dobrovolskis, T. J. Lee and D. Queloz provided constructive comments on the manuscript. D.C.F. and J.A.C. acknowledge NASA support through Hubble Fellowship grants HF-51272.01-A and HF-51267.01-A, respectively, awarded by STScl, operated by AURA under contract NAS 5-26555. NR 35 TC 338 Z9 338 U1 2 U2 20 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 3 PY 2011 VL 470 IS 7332 BP 53 EP 58 DI 10.1038/nature09760 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 715LQ UT WOS:000286886400032 PM 21293371 ER PT J AU Hummon, MT Tscherbul, TV Klos, J Lu, HI Tsikata, E Campbell, WC Dalgarno, A Doyle, JM AF Hummon, Matthew T. Tscherbul, Timur V. Klos, Jacek Lu, Hsin-I Tsikata, Edem Campbell, Wesley C. Dalgarno, Alexander Doyle, John M. TI Cold N plus NH Collisions in a Magnetic Trap SO PHYSICAL REVIEW LETTERS LA English DT Article ID MOLECULES; ATOMS AB We present an experimental and theoretical study of atom-molecule collisions in a mixture of cold, trapped N atoms and NH molecules at a temperature of similar to 600 mK. We measure a small N + NH trap loss rate coefficient of k(loss)((N+NH)) = 9(5)(3) x 10(-13) cm(3) s(-1). Accurate quantum scattering calculations based on ab initio interaction potentials are in agreement with experiment and indicate the magnetic dipole interaction to be the dominant loss mechanism. Our theory further indicates the ratio of N + NH elastic-to-inelastic collisions remains large (> 100) into the mK regime. C1 [Hummon, Matthew T.; Tsikata, Edem; Campbell, Wesley C.; Doyle, John M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Hummon, Matthew T.; Tscherbul, Timur V.; Lu, Hsin-I; Tsikata, Edem; Campbell, Wesley C.; Dalgarno, Alexander; Doyle, John M.] Harvard MIT, Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, Timur V.; Dalgarno, Alexander] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Klos, Jacek] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Lu, Hsin-I] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Hummon, MT (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM matt@cua.harvard.edu RI Campbell, Wesley/F-6813-2010; Klos, Jacek/A-6457-2008; Tscherbul, Timur/K-3286-2014; OI Klos, Jacek/0000-0002-7407-303X; Tscherbul, Timur/0000-0001-5689-040X; HUMMON, MATTHEW/0000-0002-3020-0500 FU Department of Energy [DE-FG02-02ER15316]; Air Force Office of Scientific Research [FA9550-07-1-0492]; DOE Office of Basic Energy Science; NSF FX This work was supported by the Department of Energy, under Grant No. DE-FG02-02ER15316 and by the Air Force Office of Scientific Research, under Grant No. FA9550-07-1-0492. T.V. Tand A.D acknowledge support from the DOE Office of Basic Energy Science and NSF to the Harvard-MIT CUA and ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 32 TC 41 Z9 41 U1 0 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 FEB 2 PY 2011 VL 106 IS 5 AR 053201 DI 10.1103/PhysRevLett.106.053201 PG 4 WC Physics, Multidisciplinary SC Physics GA 715JG UT WOS:000286879900004 PM 21405394 ER PT J AU Trac, H Gnedin, NY AF Trac, Hy Gnedin, Nickolay Y. TI Computer Simulations of Cosmic Reionization SO ADVANCED SCIENCE LETTERS LA English DT Review DE Cosmology: Theory; Large-Scale Structure of Universe; Galaxies: Formation; Intergalactic Medium; Methods: Numerical; Radiative Transfer ID SMOOTHED PARTICLE HYDRODYNAMICS; LY-ALPHA EMITTERS; LARGE-SCALE STRUCTURE; COSMOLOGICAL RADIATIVE-TRANSFER; UV LUMINOSITY FUNCTIONS; 21 CM SIGNAL; HYDROGEN REIONIZATION; HIGH-REDSHIFT; Z-SIMILAR-TO-6 QUASARS; INTERGALACTIC MEDIUM AB The cosmic reionization of hydrogen was the last major phase transition in the evolution of the universe, which drastically changed the ionization and thermal conditions in the cosmic gas. To the best of our knowledge today, this process was driven by the ultra-violet radiation from young, star-forming galaxies and from first quasars. We review the current observational constraints on cosmic reionization, as well as the dominant physical effects that control the ionization of intergalactic gas. We then focus on numerical modeling of this process with computer simulations. Over the past decade, significant progress has been made in solving the radiative transfer of ionizing photons from many sources through the highly inhomogeneous distribution of cosmic gas in the expanding universe. With modern simulations, we have finally converged on a general picture for the reionization process, but many unsolved problems still remain in this young and exciting field of numerical cosmology. C1 [Gnedin, Nickolay Y.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Trac, Hy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gnedin, Nickolay Y.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gnedin, Nickolay Y.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. RP Gnedin, NY (reprint author), Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA. RI Trac, Hy/N-8838-2014 OI Trac, Hy/0000-0001-6778-3861 FU Institute for Theory and Computation; DOE at Fermi lab FX We thank Alexandre Amblard, Xiaohui Fan, Ilian Iliev, Mario Santos, Volker Springel, and Oliver Zahn for kind permission to use their figures in this review. Hy Trac is supported by an Institute for Theory and Computation Fellowship. Nickolay Y. Gnedin is supported in part by the DOE at Fermi lab. NR 95 TC 36 Z9 36 U1 1 U2 1 PU AMER SCIENTIFIC PUBLISHERS PI VALENCIA PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA SN 1936-6612 J9 ADV SCI LETT JI Adv. Sci. Lett. PD FEB PY 2011 VL 4 IS 2 BP 228 EP 243 DI 10.1166/asl.2011.1214 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 774UA UT WOS:000291410900004 ER PT J AU Krayesky, DM Norris, JN West, JA Fredericq, S AF Krayesky, David M. Norris, James N. West, John A. Fredericq, Suzanne TI The Caloglossa leprieurii complex (Delesseriaceae, Rhodophyta) in the Americas: the elucidation of overlooked species based on molecular and morphological evidence SO CRYPTOGAMIE ALGOLOGIE LA English DT Article DE Atlantic Ocean; Caloglossa; Ceramiales; Delesseriaceae; Gulf of Mexico; LSU rDNA; rbcL; Rhodophyta; systematics ID RED ALGAE; NOV; CERAMIACEAE; BOTRYOCLADIA; CHLOROPHYTA; APOMEIOTICA; PHYLOGENIES; SEQUENCES; TAXONOMY; PACIFIC AB The red algal genus Caloglossa (Delesseriaceae, Ceramiales) in the New World is represented by Caloglossa leprieurii sensu Into. The earliest name for any species in the genus, other than the basionym Delesseria leprieurii, is Apiarium apiculum. On the basis of comparative morphological data, and rbcL and LSU rDN A sequence analyses, the C. leprieurii complex in the New World is found to include four species: C. leprieurii, C. apomeiotica, C. apicula comb. nov., and C. ruetzleri sp. nov. The four species can be distinguished by subtle vegetative characters, including rhizoid morphology, the degree of constriction at the thallus nodes, presence or absence of adventitious branches, number of cell rows cut off from the first axial cell of the main axis, and the position of the cystocarp on the blades. A dichotomous key highlights the diagnostic vegetative characters to separate species of the C. leprieurii complex that occur in the Americas. Caloglossa leprieurii is a tropical species from the Caribbean Sea, the Indian Ocean and the tropical eastern Pacific Ocean. Caloglossa ruetzleri is apparently restricted to the Caribbean Sea and the Gulf of Mexico, C. apomeiotica to the eastern Pacific and southern Atlantic Oceans, and C. apicula the Western Atlantic Ocean, Gulf of Mexico and Indian Ocean. C1 [Krayesky, David M.] Slippery Rock Univ, Dept Biol, Slippery Rock, PA 16057 USA. [Norris, James N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [West, John A.] Univ Melbourne, Sch Bot, Parkville, Vic 3010, Australia. [Fredericq, Suzanne] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. RP Krayesky, DM (reprint author), Slippery Rock Univ, Dept Biol, Slippery Rock, PA 16057 USA. EM david.krayesky@sru.edu FU The National Science Foundation [DEB PEET 0328491, DEB 091905, DEB 0936216, OISE 0819205] FX The National Science Foundation Grants DEB PEET 0328491, DEB 091905, DEB 0936216 and OISE 0819205 supported parts of this study. We also would like to thank Juan Lopez-Bautista for material of C. leprieurii from French Guyana, Klaus Ruetzler for providing logistical support in Smithsonian Marine Field Laboratory, Carrie Bow Cay, Belize, all collectors cited in Table 1, and Michael J. Wynne who provided loans of herbarium material from MICH as well as many helpful comments to improve the manuscript. In addition, we would also like to thank Chris Puttock, Mitsunobu Kamiya, and Giuseppe C. Zuccarello for their helpful remarks with this manuscript. This research represents Caribbean Coral Reef Ecosystem Program of the National Museum of Natural History Contribution No. CCRE-863. NR 56 TC 6 Z9 7 U1 0 U2 3 PU ADAC-CRYPTOGAMIE PI PARIS PA 12 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0181-1568 J9 CRYPTOGAMIE ALGOL JI Cryptogam. Algol. PD FEB PY 2011 VL 32 IS 1 BP 37 EP 62 PG 26 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 752QD UT WOS:000289706500004 ER PT J AU Fredericq, S Krayesky, D Schmidt, W Gabriel, D Norris, JN AF Fredericq, S. Krayesky, D. Schmidt, W. Gabriel, D. Norris, J. N. TI NEW INSIGHTS INTO THE SYSTEMATICS OF THE RED ALGAL FAMILY PEYSSONNELIACEAE (PEYSSONNELIALES) SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Fredericq, S.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Krayesky, D.] Slippery Rock Univ, Dept Biol, Slippery Rock, PA 16057 USA. [Schmidt, W.] Univ Louisiana Lafayette, Dept Biol, Lafayette, Portugal. [Norris, J. N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Biol, Washington, DC 20560 USA. EM slf9209@louisiana.edu; david.krayesky@sru.edu; wes4500@louisiana.edu NR 0 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2011 VL 47 SU 1 SI SI BP 7 EP 7 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 721NJ UT WOS:000287361300015 ER PT J AU Schmidt, W Fredericq, S Wysor, B Norris, JN AF Schmidt, W. Fredericq, S. Wysor, B. Norris, J. N. TI THE RED ALGAL GENUS CHAMPIA IN THE GULF OF MEXICO AND THE CARIBBEAN SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Schmidt, W.; Fredericq, S.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Wysor, B.] Roger Williams Univ, Dept Biol & Marine Biol, Bristol, RI 02809 USA. [Norris, J. N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Biol, Washington, DC 20560 USA. EM wes4500@louisiana.edu; slf9209@louisiana.edu; bwysor@rwu.edu NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2011 VL 47 SU 1 SI SI BP 11 EP 11 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 721NJ UT WOS:000287361300022 ER PT J AU Laughinghouse, HD Kangas, PC Adey, WH AF Laughinghouse, H. D. Kangas, P. C. Adey, W. H. TI ALGAL SPECIES DIVERSITY IN TWO EXPERIMENTAL ALGAL PRODUCTION SYSTEMS IN SOUTHEASTERN PENNSYLVANIA SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Adey, W. H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Kangas, P. C.] Univ Maryland, Environm Sci & Technol Dept, College Pk, MD 20742 USA. EM hdliv@hotmail.com RI Adey, Walter/G-2858-2011 NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2011 VL 47 SU 1 SI SI BP 27 EP 28 PG 2 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 721NJ UT WOS:000287361300058 ER PT J AU Krayesky, DM Norris, JN West, JA Wysor, B Fredericq, S AF Krayesky, D. M. Norris, J. N. West, J. A. Wysor, B. Fredericq, S. TI A UNIQUE NEW SPECIES OF CALOGLOSSA (DELESSERIACEAE, RHODOPHYTA) FROM PEDRO MIGUEL LOCKS, MIRAFLORES LAKE, PANAMA, CENTRAL AMERICA SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Krayesky, D. M.] Slippery Rock Univ, Slippery Rock, PA 16057 USA. [Norris, J. N.] Smithsonian Inst, Washington, DC 20560 USA. [West, J. A.] Univ Melbourne, Melbourne, Vic 3010, Australia. [Wysor, B.] Roger Williams Univ, Bristol, RI 02809 USA. [Fredericq, S.] Univ Louisiana Lafayette, Lafayette, LA 70503 USA. EM david.krayesky@sru.edu; NORRISJ@si.edu; jwest@unimelb.edu.au; bwysor@rwu.edu; slf9209@louisiana.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2011 VL 47 SU 1 SI SI BP 44 EP 44 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 721NJ UT WOS:000287361300094 ER PT J AU Liebhold, P AF Liebhold, Peter TI The Vault SO PUBLIC HISTORIAN LA English DT Art Exhibit Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Liebhold, P (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS & DIGITAL PUBLISHING DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FEB PY 2011 VL 33 IS 1 BP 83 EP 86 DI 10.1525/tph.2011.33.1.83 PG 4 WC History SC History GA 731XR UT WOS:000288144400009 ER PT J AU Blanco, JM Long, JA Gee, G Wildt, DE Donoghue, AM AF Blanco, Juan M. Long, Julie A. Gee, George Wildt, David E. Donoghue, Ann M. TI Comparative cryopreservation of avian spermatozoa: Benefits of non-permeating osmoprotectants and ATP on turkey and crane sperm cryosurvival SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Poultry sperm; DMA; Trehalose; Sucrose; Betaine hydrochloride ID EXTRACELLULAR ADENOSINE 5'-TRIPHOSPHATE; COTURNIX-JAPONICA SPERMATOZOA; FERTILIZING ABILITY; GLYCINE BETAINE; FOWL SPERMATOZOA; RAM SPERMATOZOA; COOLING RATE; BULL SPERM; TREHALOSE; MOTILITY AB A comparative approach was used to evaluate the cryosurvival of turkey and crane sperm frozen in a dimethylacetamide (DMA) cryodiluent supplemented with osmoprotectants and ATP. A range (6-26%) of DMA concentrations was used alone or in combination with ATP (30,60 or 118 mM) or one of the following osmoprotectants: (1) sucrose (turkey, 8.0%; crane, 5.0%); (2) 5.0% sucrose and 5.0% trehalose; or (3) betaine hydrochloride (0.1, 0.2 or 0.4 mM). The viability of thawed sperm was assessed using the nigrosin-eosin stain and sperm motility was determined using the hanging-drop technique. For semen frozen only with DMA, post-thaw sperm motility was greatest (P < 0.05) for the 6.0%, 10.0% and 18% concentrations, regardless of species. Turkey sperm frozen with the sucrose/trehalose combination had greater (P < 0.05) post-thaw motility for all DMA treatments compared to DMA alone. The lowest concentration of the osmoprotectant betaine hydrochloride substantially improved turkey sperm viability post-thaw in all treatments compared to DMA alone (P < 0.05). The post-thaw motility of crane sperm was improved (P< 0.05) with a combination of 18.0%, 24.0% or 26.0% DMA and 30 mM ATP. Moreover, in the presence of osmoprotectants, crane sperm motility decreased as the osmoprotectant concentration increased. The lowest concentration of ATP also improved crane sperm viability post-thaw, especially for DMA concentrations 18% or greater. The combination of sucrose and trehalose improved (P < 0.05) crane sperm viability only with 6% and 10% DMA. These data affirm that there are avian-specific differences in sperm survival after cryopreservation and suggest that post-thaw survival can be enhanced by including species-based osmoprotectant/ATP combinations in a cryodiluent where DMA is the cryoprotectant. Published by Elsevier B.V. C1 [Blanco, Juan M.; Long, Julie A.] ARS, USDA, ANRI, ABBL, Beltsville, MD 20705 USA. [Blanco, Juan M.] Aquila Fdn, Toledo, Spain. [Blanco, Juan M.] CERI, Ctr Studies Iberian Raptors, Toledo, Spain. [Gee, George] US Fish & Wildlife Serv, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Wildt, David E.] Smithsonians Natl Zool Pk, Conservat & Res Ctr, Ctr Species Survival, Front Royal, VA 22630 USA. [Donoghue, Ann M.] ARS, USDA, PPPSRU, Fayetteville, AR 72701 USA. RP Long, JA (reprint author), ARS, USDA, ANRI, ABBL, Beltsville, MD 20705 USA. EM julie.long@ars.usda.gov RI Wilkinson, Stuart/C-2802-2013 FU USDA [SP 33]; Patuxent Wildlife Research Center, USGS; Junta de Comunidades de Castilla-La Mancha; Smithsonian Institution/British Airways partnership; Smithsonian Women's Committee; Aquila Foundation FX This study was supported by the USDA Foreign Agricultural Services Project #SP 33; The Patuxent Wildlife Research Center, USGS; The Junta de Comunidades de Castilla-La Mancha, the Smithsonian Institution/British Airways partnership; The Smithsonian Women's Committee; and the Aquila Foundation. NR 48 TC 23 Z9 23 U1 0 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD FEB PY 2011 VL 123 IS 3-4 BP 242 EP 248 DI 10.1016/j.anireprosci.2010.12.005 PG 7 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 738GG UT WOS:000288627700015 PM 21277718 ER PT J AU Gagnon, PR Bruna, EM Rubim, P Darrigo, MR Littell, RC Uriarte, M Kress, WJ AF Gagnon, Paul R. Bruna, Emilio M. Rubim, Paulo Darrigo, Maria Rosa Littell, Ramon C. Uriarte, Maria Kress, W. John TI Growth of an understory herb is chronically reduced in Amazonian forest fragments SO BIOLOGICAL CONSERVATION LA English DT Article DE Habitat fragmentation; Heliconia acuminata; Plant demography; Relative growth rate; Reproductive output; Vital rates ID TROPICAL RAIN-FOREST; HABITAT FRAGMENTATION; PLANT-POPULATIONS; HELICONIA-ACUMINATA; TREE COMMUNITIES; BRAZILIAN AMAZON; EDGE; VEGETATION; RESPONSES; RECRUITMENT AB The biotic and abiotic changes associated with habitat fragmentation have been shown to have major consequences for plant recruitment and survivorship. However, few studies have quantified the growth of plants that persist in fragments. Over the course of a decade, we measured annual growth of 5200 individuals of the common understory herb Heliconia acuminata (Heliconiaceae) in an experimentally fragmented Amazonian forest. We tested (A) whether annual growth rates were lower in fragments than in continuous forest, and (B) whether cumulative growth rates of plants that survived the entire period were lower in fragments. While mean annual growth rates were often lower in fragments, differences were not significant in any year. After 10 years, however, the cumulative effect was that plants in fragments were significantly smaller. This had a clear demographic consequence - plants in fragments produced fewer inflorescences than plants in continuous forest. Our results demonstrate that chronic reduced individual growth may be an important mechanism contributing to reduced population viability in fragmented forests, and that negative demographic consequences of fragmentation for plants can take years to manifest themselves. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Gagnon, Paul R.; Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Gagnon, Paul R.; Bruna, Emilio M.] INPA PDBFF, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Bruna, Emilio M.; Rubim, Paulo; Darrigo, Maria Rosa; Uriarte, Maria] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. [Littell, Ramon C.] Univ Florida, Dept Stat, Gainesville, FL 32611 USA. [Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Kress, W. John] Smithsonian Inst, NMNH Dept Bot, Washington, DC 20013 USA. RP Gagnon, PR (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, POB 110430, Gainesville, FL 32611 USA. EM pgagnon@ufl.edu RI Bruna, Emilio/H-2769-2012; Uriarte, Maria/L-8944-2013 OI Bruna, Emilio/0000-0003-3381-8477; FU US National Science Foundation [DEB-0614149, DEB-0614339, DEB-0309819, DBI-0109226, INT 98-06351]; University of Florida FX We thank Kathleen Kiernan for suggestions with analyses and Heather Passmore and three anonymous reviewers for comments on the manuscript. We also thank the many technicians and students who helped conduct the censuses and the logistical support of the BDFFP and its staff. Financial support was provided by the US National Science Foundation (awards DEB-0614149, DEB-0614339, DEB-0309819, DBI-0109226, and INT 98-06351) and the University of Florida. This is publication number 566 in the BDFFP Technical Series. NR 60 TC 9 Z9 9 U1 0 U2 26 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD FEB PY 2011 VL 144 IS 2 BP 830 EP 835 DI 10.1016/j.biocon.2010.11.015 PG 6 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 728TJ UT WOS:000287897100023 ER PT J AU Fisher, R Radford, BT Knowlton, N Brainard, RE Michaelis, FB Caley, MJ AF Fisher, Rebecca Radford, Ben T. Knowlton, Nancy Brainard, Russell E. Michaelis, Frances B. Caley, M. Julian TI Global mismatch between research effort and conservation needs of tropical coral reefs SO CONSERVATION LETTERS LA English DT Article DE Biological conservation; biological knowledge; Coral Triangle; coral reefs; geocoding; global conservation; global research; Google Maps (TM); scientific literature; Web of Science ID CLIMATE-CHANGE; BIODIVERSITY HOTSPOTS; MARINE BIODIVERSITY; ECOSYSTEMS; RESILIENCE; PRIORITIES; OCEAN AB Tropical coral reefs are highly diverse and globally threatened. Management to ensure their persistence requires sound biological knowledge in regions where coral reef biodiversity and/or the threats to it are greatest. This paper uses a novel text analysis approach and Google Maps (TM) to examine the spatial coverage of scientific papers on coral reefs listed in Web of Science (R). Results show that research is highly clumped spatially, positively related to per capita gross domestic product, negatively related to coral species richness, and unrelated to threats to coral reefs globally; indicating a serious mismatch between conservation needs and the knowledge required for effective management. Greater research effort alone cannot guarantee better conservation outcomes, but given some regions of the world (e.g., Central Indo-Pacific) remain severely understudied, priority allocation of resources to fill such knowledge gaps should support greater adaptive management capacity through the development of an improved knowledge base for reef managers. C1 [Fisher, Rebecca; Radford, Ben T.] UWA Oceans Inst M096, Australian Inst Marine Sci, Crawley, WA 6009, Australia. [Radford, Ben T.] Univ Western Australia M004, Sch Earth & Environm, Crawley, WA 6009, Australia. [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20013 USA. [Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. [Brainard, Russell E.] Natl Marine Fisheries Serv, Coral Reef Ecosyst Div, Pacific Islands Fisheries Sci Ctr, NOAA, Honolulu, HI 96814 USA. [Michaelis, Frances B.; Caley, M. Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia. RP Fisher, R (reprint author), UWA Oceans Inst M096, Australian Inst Marine Sci, 35 Stirling Hwy, Crawley, WA 6009, Australia. EM r.fisher@aims.gov.au RI Fisher, Rebecca/C-5459-2011; OI Fisher, Rebecca/0000-0001-5148-6731 FU BHP Billiton through CReefs Australia (CReefs, Census of Marine Life) FX Funded by BHP Billiton through CReefs Australia (CReefs, Census of Marine Life). J. Ruxton assisted with compiling the literature database, M. Case assisted with geographic analyses and R. O'Leary provided statistical advice. S. Wilson, S. Kininmonth, M. Case, and M. Puotinen provided comments on the manuscript. R. F., M. J. C, N.K., and R. B. conceived the study, F. B. M. provided global context, B. R. assisted with geocoding and analyses, R. F. and M. J. C. led the writing of the manuscript; all authors contributed to writing and commenting on drafts. We thank P. Armsworth and two anonymous reviewers for their comments. NR 32 TC 29 Z9 29 U1 2 U2 37 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-263X J9 CONSERV LETT JI Conserv. Lett. PD FEB PY 2011 VL 4 IS 1 BP 64 EP 72 DI 10.1111/j.1755-263X.2010.00146.x PG 9 WC Biodiversity Conservation SC Biodiversity & Conservation GA 716PW UT WOS:000286986900008 ER PT J AU Pavicic, M Megill, ND Aravind, PK Waegell, M AF Pavicic, Mladen Megill, Norman D. Aravind, P. K. Waegell, Mordecai TI New class of 4-dim Kochen-Specker sets SO JOURNAL OF MATHEMATICAL PHYSICS LA English DT Article ID THEOREM; VECTORS; CONTEXTUALITY AB We find a new highly symmetrical and very numerous class (millions of nonisomorphic sets) of 4-dim Kochen-Specker (KS) vector sets. Due to the nature of their geometrical symmetries, they cannot be obtained from previously known ones. We generate the sets from a single set of 60 orthogonal spin vectors and 75 of their tetrads (which we obtained from the 600-cell) by means of our newly developed stripping technique. We also consider critical KS subsets and analyze their geometry. The algorithms and programs for the generation of our KS sets are presented. (C) 2011 American Institute of Physics. [doi:10.1063/1.3549586] C1 [Pavicic, Mladen] Harvard Univ, Dept Phys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Univ Zagreb, Zagreb 41000, Croatia. [Megill, Norman D.] Boston Informat Grp, Lexington, MA 02420 USA. [Aravind, P. K.; Waegell, Mordecai] Worcester Polytech Inst, Dept Phys, Worcester, MA 01609 USA. RP Pavicic, M (reprint author), Harvard Univ, Dept Phys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. EM pavicic@grad.hr; nm@alum.mit.edu; paravind@wpi.edu; caiw@wpi.edu FU US National Science Foundation; Ministry of Science, Education, and Sport of Croatia [082-0982562-3160] FX One of us (M.P.) would like to thank his host Hossein Sadeghpour for a support during his stay at ITAMP. Supported by the US National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics (ITAMP) at Harvard University and Smithsonian Astrophysical Observatory and Ministry of Science, Education, and Sport of Croatia through the project No. 082-0982562-3160. Computational support was provided by the cluster Isabella of the University Computing Centre of the University of Zagreb and by the Croatian National Grid Infrastructure. NR 33 TC 1 Z9 1 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0022-2488 J9 J MATH PHYS JI J. Math. Phys. PD FEB PY 2011 VL 52 IS 2 AR 022104 DI 10.1063/1.3549586 PG 9 WC Physics, Mathematical SC Physics GA 727OW UT WOS:000287811800004 ER PT J AU Diaz-Marrero, AR Porras, G Aragon, Z de la Rosa, JM Dorta, E Cueto, M D'Croz, L Mate, J Darias, J AF Diaz-Marrero, Ana R. Porras, Gina Aragon, Zulma de la Rosa, Jose M. Dorta, Enrique Cueto, Mercedes D'Croz, Luis Mate, Juan Darias, Jose TI Carijodienone from the Octocoral Carijoa multiflora. A Spiropregnane-Based Steroid SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID T76 SCENEDESMUS QUADRICAUDA; SOFT CORAL; TELESTO-RIISEI; ELYSIAPYRONES; BIOSYNTHESIS; PUNAGLANDINS; PREGNANES; CULTURES; CHAIN AB Two new steroids (1 and 2) and the known pregna-1,4,20-trien-3-one (3) have been isolated from the Pacific octocoral Carijoa multiflora. Compound 1 possesses a novel spiropregnane-based steroidal skeleton. The photochemical transformation of 3 into 1. allowed the assignment of the absolute configuration at C-10 of 1. The antibacterial activities of compounds 1 and 3 were evaluated against a panel of bacterial strains. C1 [Diaz-Marrero, Ana R.; Porras, Gina; Aragon, Zulma; de la Rosa, Jose M.; Dorta, Enrique; Cueto, Mercedes; Darias, Jose] CSIC, Inst Prod Nat & Agrobiol, Tenerife 38206, Spain. [D'Croz, Luis] Univ Panama, Dept Biol Marina & Limnol, Panama City, Panama. [Mate, Juan] Smithsonian Trop Res Inst, Balboa, Panama. RP Diaz-Marrero, AR (reprint author), CSIC, Inst Prod Nat & Agrobiol, Ave Astrofis F Sanchez 3, Tenerife 38206, Spain. EM ardiaz@ipna.csic.es RI Diaz-Marrero, Ana/L-2899-2014; Cueto, MERCEDES/L-3185-2014 OI Diaz-Marrero, Ana/0000-0002-8886-7519; Cueto, MERCEDES/0000-0002-9112-6877 FU Ministerio de Ciencia e Innovacion [BIO2007-61745, SAF2009-08039, SAF2010-16858]; JAE-Doc (CSIC) FX This work was supported by the Ministerio de Ciencia e Innovacion (BIO2007-61745, SAF2009-08039, SAF2010-16858). A.R.D.-M. acknowledges financial support from Programs JAE-Doc (CSIC). The STRI provided support and facilities for field work The authors thank J. del Rosario for technical support and Dr. A. J. Herrera for assistance in completion of the photochemical reaction. The Government of Panama granted permission for the collection of the samples. NR 26 TC 14 Z9 14 U1 0 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD FEB PY 2011 VL 74 IS 2 BP 292 EP 295 DI 10.1021/np1007608 PG 4 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 725IB UT WOS:000287637300028 PM 21235217 ER PT J AU Welten, KC Caffee, MW Hillegonds, DJ McCoy, TJ Masarik, J Nishiizumi, K AF Welten, K. C. Caffee, M. W. Hillegonds, D. J. McCoy, T. J. Masarik, J. Nishiizumi, K. TI Cosmogenic radionuclides in L5 and LL5 chondrites from Queen Alexandra Range, Antarctica: Identification of a large L/LL5 chondrite shower with a preatmospheric mass of approximately 50,000 kg SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID TRACE-ELEMENT CONTENT; COSMIC-RAY PARTICLES; EXPOSURE HISTORY; PRODUCTION-RATES; FRONTIER MOUNTAIN; TERRESTRIAL AGES; IRON-METEORITES; AMS STANDARDS; STONY METEORITES; STREWN FIELD AB The collection of approximately 3300 meteorites from the Queen Alexandra Range (QUE) area, Antarctica, is dominated by more than 2000 chondrites classified as either L5 or LL5. Based on concentrations of the cosmogenic radionuclides 10Be, 26Al, 36Cl, and 41Ca in the metal and stone fraction of 16 QUE L5 or LL5 chondrites, we conclude that 13 meteorites belong to a single meteorite shower, QUE 90201, with a large preatmospheric size and a terrestrial age of 125 kyr. Members of this shower have properties typical of L (e.g., pyroxene composition) and LL chondrites (e.g., metal abundance and composition), as well as properties intermediate between the L and LL groups (e.g., olivine composition), and is thus best described as an L/LL5 chondrite. Based on comparison with model calculations, the measured radionuclide concentrations in the metal and stone fractions of QUE 90201 indicate irradiation in an object with a preatmospheric radius of approximately 150 cm, representing one of the largest chondrites known so far. Based on the abundance of small L5 and LL5 chondrites at QUE and their distinct mass distribution, we conclude that the QUE 90201 shower includes up to 2000 fragments with a total recovered mass of 60-70 kg, < 1% of the preatmospheric mass of approximately 50,000 kg. The mass distribution of the QUE 90201 shower suggests that the meteoroid experienced catastrophic atmospheric fragmentation(s), either because it was a fragile object or it had a high entry velocity. C1 [Welten, K. C.; Nishiizumi, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Caffee, M. W.; Hillegonds, D. J.] Lawrence Livermore Natl Lab, Ctr Accelerator Mass Spectrometry, Livermore, CA 94550 USA. [Caffee, M. W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [McCoy, T. J.] Smithsonian Inst, US Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Masarik, J.] Comenius Univ, Dept Nucl Phys, SK-84248 Bratislava, Slovakia. RP Welten, KC (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM kcwelten@berkeley.edu RI Caffee, Marc/K-7025-2015 OI Caffee, Marc/0000-0002-6846-8967 FU NASA [NAG5-4992, NAG5-9777]; LLNL-CAMS FX This work was supported, in part, by NASA grants NAG5-4992 (K. C. W. and K. N.), NAG5-9777 (T. J. M.), and a LLNL-CAMS grant. We thank the National Science Foundation for supporting the Antarctic Search for Meteorites (ANSMET) and the Meteorite Working Group for providing samples. We also are grateful to Bob Finkel for assistance with the AMS measurements at LLNL. AMS measurements at LLNL were performed under the auspices of the U.S. DOE by LLNL under contract W-7405-ENG-48. We thank Bernard Lavielle and Ingo Leya for valuable comments that improved this article, and Tim Jull for editorial handling. NR 78 TC 13 Z9 13 U1 1 U2 10 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD FEB PY 2011 VL 46 IS 2 DI 10.1111/j.1945-5100.2010.01142.x PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 723DU UT WOS:000287487300002 ER PT J AU Koch, PM Raffin, P Huang, YD Chen, MT Han, CC Lin, KY Altamirano, P Granet, C Ho, PTP Huang, CWL Kesteven, M Li, CT Liao, YW Liu, GC Nishioka, H Ong, CL Oshiro, P Umetsu, K Wang, FC Wu, JHP AF Koch, Patrick M. Raffin, Philippe Huang, Yau-De Chen, Ming-Tang Han, Chih-Chiang Lin, Kai-Yang Altamirano, Pablo Granet, Christophe Ho, Paul T. P. Huang, Chih-Wei L. Kesteven, Michael Li, Chao-Te Liao, Yu-Wei Liu, Guo-Chin Nishioka, Hiroaki Ong, Ching-Long Oshiro, Peter Umetsu, Keiichi Wang, Fu-Cheng Wu, Jiun-Huei Proty TI 1.2 m Shielded Cassegrain Antenna for Close-Packed Radio Interferometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MICROWAVE BACKGROUND ANISOTROPY; MASSIVE GALAXY CLUSTERS; AMIBA; DESIGN; ARRAY; PERFORMANCE; TELESCOPE; REDUCTION; COSMOLOGY; REFLECTOR AB Interferometric millimeter observations of the cosmic microwave background and clusters of galaxies with arcminute resolutions require antenna arrays with short spacings. Having all antennas co-mounted on a single steerable platform sets limits to the overall weight. A 25 kg lightweight novel carbon-fiber design for a 1.2 m diameter Cassegrain antenna is presented. The finite element analysis predicts excellent structural behavior under gravity, wind, and thermal load. The primary- and secondary-minor surfaces are aluminum-coated with a thin TiO(2) top layer for protection. A low beam sidelobe level is achieved with a Gaussian feed-illumination pattern with edge taper, designed based on feed-horn antenna simulations and verified in a far-field beam-pattern measurement. A shielding baffle reduces interantenna coupling to below similar to - 135 dB. The overall antenna efficiency, including a series of efficiency factors, is estimated to be around 60%, with major losses coming from the feed spillover and secondary blocking. With this new antenna, a detection rate of about 50 clusters yr(-1) is anticipated in a 13-element array operation. C1 [Koch, Patrick M.; Raffin, Philippe; Huang, Yau-De; Chen, Ming-Tang; Han, Chih-Chiang; Lin, Kai-Yang; Altamirano, Pablo; Ho, Paul T. P.; Li, Chao-Te; Liao, Yu-Wei; Liu, Guo-Chin; Nishioka, Hiroaki; Oshiro, Peter; Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Granet, Christophe] CSIRO ICT Ctr, Epping, NSW 1710, Australia. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huang, Chih-Wei L.; Liao, Yu-Wei; Wang, Fu-Cheng; Wu, Jiun-Huei Proty] Natl Taiwan Univ, Dept Phys, Inst Astrophys, Taipei 10617, Taiwan. [Huang, Chih-Wei L.; Liao, Yu-Wei; Wang, Fu-Cheng; Wu, Jiun-Huei Proty] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Kesteven, Michael] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, Taipei County, Taiwan. [Ong, Ching-Long] CoTec Inc, Taichung, Taiwan. RP Koch, PM (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM pmkoch@asiaa.sinica.edu.tw OI WU, JIUN-HUEI/0000-0001-9608-7662 FU Ministry of Education; National Science Council as part of the Cosmology and Particle Astrophysics initiative; Academia Sinica FX Capital and operational funding for the Array for Microwave Background Anisotropy came from the Ministry of Education and the National Science Council as part of the Cosmology and Particle Astrophysics initiative. Matching operational funding also came in the form of an Academia Sinica Key Project. P. M. K. acknowledges Shiang-Yu Wang for advising and consulting on mirror coatings. NR 45 TC 2 Z9 3 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD FEB PY 2011 VL 123 IS 900 BP 198 EP 212 DI 10.1086/658675 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 728WI UT WOS:000287904800008 ER PT J AU Vencl, FV Trillo, PA Geeta, R AF Vencl, Fredric V. Trillo, Paula A. Geeta, R. TI Functional interactions among tortoise beetle larval defenses reveal trait suites and escalation SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Failure-time analysis; Shield; Gregariousness; Maternal care; Bayesian; Character reconstruction; Cassidinae; Splits analysis ID PHYLOGENETIC ANALYSIS; ADAPTIVE RADIATION; PLANT DEFENSE; PHYTOPHAGOUS INSECTS; REPELLENT DEFENSES; SHIELD DEFENSE; EVOLUTION; PREDATION; DIVERSIFICATION; GREGARIOUSNESS AB Whereas the "escape-and-radiate" plant-herbivore scenario predicts that reciprocating cycles of defense-counter defense foster the evolution of traits with increasing efficacy that accumulate during clade diversification, coevolutionary models of herbivore responses to their enemies remain unexplored. Quantitative information is scarce about how defensive traits perform, interact and become functionally integrated. Moreover, there are few studies that have combined performance and phylogenetic information to detect patterns of trait assembly and trends in defense efficacy. Using field demonstrations of effectiveness and phylogenetic reconstructions, we evaluated patterns of trait precedence and suite assembly by comparing the larval defenses of two beetles, Acromis sparsa and Chelymorpha alternans, which both feed on the leaf surfaces of the same plant, have shields containing host-derived deterrent chemicals and form aggregations. Additionally, female A. sparsa guard their larvae. Using an ecologically relevant bioassay, we quantified the extent to which: (1) gregariousness, size, maternal care and shields affected survival; (2) defenses interacted, and; (3) derived traits and suites outperformed ancestral ones. Regression models ranked traits revealing synergistic interactions. Shields interacted with gregariousness to form the strongest suite. Maternal care contributed to overall higher survival in A. sparsa, an advantage lost after female removal. Phylogenetic reconstruction revealed a sequence of trait accumulation and suite formation. The combined performance-phylogenetic approach revealed: (1) multi-trait interactions amplified effectiveness; (2) a sequence of novel trait origins was followed by suite assembly, and; (3) an incremental trend in defense efficacy congruent with escalation. Multi-trait interactions fostered suite assembly that likely conferred the advantage of enhanced survival in the precarious leaf surface adaptive zone. C1 [Vencl, Fredric V.; Geeta, R.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Trillo, Paula A.] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. [Vencl, Fredric V.] Smithsonian Trop Res Inst, Panama City, Panama. [Geeta, R.] Univ Delhi, Dept Bot, Delhi 110007, India. RP Vencl, FV (reprint author), SUNY Stony Brook, Stony Brook, NY 11794 USA. EM fvencl@life.bio.sunysb.edu; alextrillo@hotmail.com; rgeeta53@gmail.com FU US National Science Foundation [DEB 108213]; Doctoral Dissertation Improvement Grant [IOS-0508906]; Smithsonian Predoctoral Fellowship FX We thank E. Leigh, D. Emlen, F. James Rohlf, A. Ehmer, L. Maroja and D. Windsor for many thoughtful comments during the revision process. We are also grateful to A. Murgas, S. van Bael, and the students of the STRI Gigante field ecology course for collecting and bioassays help. Experiments, sample exportation, and specimen collection were done under permits issued by the Authoridad Nacional del Ambiente de Panama (ANAM). This is contribution #1157 from the Department of Ecology and Evolution at Stony Brook University. This research was supported by the US National Science Foundation DEB 108213 to F. Vencl and by a Doctoral Dissertation Improvement Grant IOS-0508906 and a Smithsonian Predoctoral Fellowship to P. Trillo. NR 67 TC 5 Z9 5 U1 3 U2 17 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 FEB PY 2011 VL 65 IS 2 BP 227 EP 239 DI 10.1007/s00265-010-1031-z PG 13 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 707WR UT WOS:000286322200011 ER PT J AU Jones, PL Page, RA Hartbauer, M Siemers, BM AF Jones, Patricia L. Page, Rachel A. Hartbauer, Manfred Siemers, Bjoern M. TI Behavioral evidence for eavesdropping on prey song in two Palearctic sibling bat species SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Advertisement call; Eavesdropping; Bat; Orthoptera; Sensory ecology; Niche partitioning; Myotis myotis; Myotis blythii oxygnathus; Tettigonia cantans; Tettigonia viridissima ID MOUSE-EARED BATS; MYOTIS-MYOTIS; TETTIGONIA-VIRIDISSIMA; NEOTROPICAL KATYDIDS; TRACHOPS-CIRRHOSUS; FORAGING STRATEGY; FEEDING-BEHAVIOR; PREDATION; ECHOLOCATION; BLYTHII AB Eavesdropping on prey communication signals has never before been reported for a Palearctic bat species. In this study, we investigated whether lesser and greater mouse-eared bats, Myotis blythii oxygnathus and Myotis myotis, find tettigoniid bushcrickets (Tettigoniidae) by eavesdropping on their mate-attraction song. Tettigoniids are known to be the most important prey item for M. blythii oxygnathus, while carabid beetles and other epigaeic arthropods are the most important prey for its sibling species, M. myotis, in many places in Europe. M. myotis locates walking beetles by listening for their rustling sounds. We compared these two species' response to four acoustic prey cues: calling song of two tettigoniid species, the rustling sound made by walking carabid beetles, and a control tone. Individuals of both bat species attacked the speaker playing tettigoniid song, which clearly indicates that both species eavesdrop on prey-generated advertisement signals. There were, however, species differences in response. M. blythii oxygnathus exhibited stronger predatory responses to the calling song of two species of tettigoniid than to the beetle rustling sound or the control. M. myotis, in contrast, exhibited stronger predatory responses to the beetle rustling and to one tettigoniid species but not the other tettigoniid or the control. Our study (1) for the first time demonstrates eavesdropping on prey communication signals for Palearctic bats and (2) gives preliminary evidence for sensory niche partitioning between these two sympatric sibling bat species. C1 [Jones, Patricia L.; Page, Rachel A.; Siemers, Bjoern M.] Max Planck Inst Ornithol, Sensory Ecol Grp, D-82319 Seewiesen, Germany. [Jones, Patricia L.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Page, Rachel A.] Smithsonian Trop Res Inst, Panama City, Panama. [Hartbauer, Manfred] Karl Franzens Univ Graz, Dept Zool, A-8010 Graz, Austria. RP Siemers, BM (reprint author), Max Planck Inst Ornithol, Sensory Ecol Grp, Eberhard Gwinner Str 11, D-82319 Seewiesen, Germany. EM siemers@orn.mpg.de FU Max Planck Society; Alexander von Humboldt Foundation; National Science Foundation; Directorate of the Rusenski Lom Nature Park; Bulgarian Bat Research and Protection Group FX We are grateful to David Bethel, Ivailo Borissov, Tess Driessens, Stefan Greif, Antonia Hubancheva, Markus Schuller, and Sara Troxell for help and company during fieldwork, bat husbandry, and experiments. We thank Maike Schuchmann for assistance in amplitude measurements, Viktoria Grossauer for the evaluation of tettigoniid song parameters, and Leonie Baier for help with figure preparation. We thank the responsible Bulgarian authorities (MOEW-Sofia and RIOSV-Ruse) for granting us permission to conduct this research and the Directorate of the Rusenski Lom Nature Park (director Milko Belberov) as well as the Bulgarian Bat Research and Protection Group for cooperation and support. We are grateful to two anonymous reviewers for their insightful comments on the manuscript. This study was funded by the Max Planck Society (BMS), an Alexander von Humboldt Foundation Postdoctoral Research Fellowship (RAP), and a National Science Foundation Graduate Research Fellowship (PLJ). NR 54 TC 13 Z9 13 U1 0 U2 29 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 FEB PY 2011 VL 65 IS 2 BP 333 EP 340 DI 10.1007/s00265-010-1050-9 PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 707WR UT WOS:000286322200022 ER PT J AU Baugh, AT Ryan, MJ AF Baugh, Alexander T. Ryan, Michael J. TI The relative value of call embellishment in tungara frogs SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Advertisement calls; Individual differences; Mate choice; Phonotaxis; Physalaemus; Sexual selection ID SEXUAL SELECTION; PHYSALAEMUS-PUSTULOSUS; LOCALIZATION PERFORMANCE; SENSORY EXPLOITATION; BARN SWALLOW; FEMALE; ADVERTISEMENT; SIGNALS; MANIPULATION; PREFERENCES AB Facultative traits that have evolved under sexual selection, such as the acoustic ornaments present in the advertisement signals of male tA(0)ngara frogs (Physalaemus pustulosus), offer a unique opportunity to examine selection for trait exaggeration with a focus on individual differences amongst signalers. By contrast, many studies of mate choice use experimental designs that obscure the inter-individual variation amongst signalers available for selection to act on-through the use of "typical" or average signals from the population. Here, we use dichotomous female phonotaxis choice tests to determine how the value of male call embellishment varies across 20 individual males frogs recorded from the wild-a sample which captures the acoustic diversity present in the population. We tested 20 females for each male call pair (i.e., 400 females). The results show widespread preference amongst females for ornamented calls ("whine-chucks") over simple calls ("whines"), yet also demonstrate substantial variation in the relative benefits for individual male frogs-some males enjoy appreciable benefits by using ornaments while others (30% of males in this study) do not. We also show that the relative amplitude of the chuck to the whine correlates positively with the value of call elaborations across these 20 males. Finally, by manipulating the relative amplitude of whines and chucks using both natural and synthetic calls, we demonstrate directly that this single call parameter is key to determining the relative value of call elaborations across males. C1 [Baugh, Alexander T.] Max Planck Inst Ornithol Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. [Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Baugh, AT (reprint author), Max Planck Inst Ornithol Migrat & Immunoecol, Schlossallee 2, D-78315 Radolfzell am Bodensee, Germany. EM abaugh@orn.mpg.de OI Baugh, Alexander/0000-0003-2032-892X FU National Science Foundation [IOB 0544096]; Homer Lindsay Bruce Endowed Fellowship FX We thank X. Bernal, A. Lea, L. Ziegler, A. Dapper, and N. Lessios for assistance with data collection and the staff at the Smithsonian Tropical Research Institute for logistical support. The suggestions of two anonymous reviewers significantly improved this manuscript. Autoridad Nacional del Ambiente approved scientific permits in the Republic of Panama. Animal use was approved by the IACUC (#06041701) at The University of Texas at Austin. This work was supported by the National Science Foundation (grant number IOB 0544096 to M. Ryan). The Homer Lindsay Bruce Endowed Fellowship supported A. Baugh. NR 34 TC 1 Z9 1 U1 1 U2 9 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 FEB PY 2011 VL 65 IS 2 BP 359 EP 367 DI 10.1007/s00265-010-1053-6 PG 9 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 707WR UT WOS:000286322200025 ER PT J AU Hirsch, BT AF Hirsch, Ben T. TI Within-group spatial position in ring-tailed coatis: balancing predation, feeding competition, and social competition SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Coati; Social foraging; Spatial position; Nasua; Predation; Dominance; Feeding competition ID BROWN CAPUCHIN MONKEYS; MACAQUES MACACA-FASCICULARIS; CONSENSUS DECISION-MAKING; CEBUS-APELLA; FORAGING GROUPS; NASUA-NASUA; ATLANTIC FOREST; ANIMAL GROUPS; ARGENTINA; RISK AB A variety of factors can influence an individual's choice of within-group spatial position. For terrestrial social animals, predation, feeding success, and social competition are thought to be three of the most important variables. The relative importance of these three factors was investigated in groups of ring-tailed coatis (Nasua nasua) in IguazA(0), Argentina. Different age/sex classes responded differently to these three variables. Coatis were found in close proximity to their own age/sex class more often than random, and three out of four age/sex classes were found to exhibit within-group spatial position preferences which differed from random. Juveniles were located more often at the front edge and were rarely found at the back of the group. Juveniles appeared to choose spatial locations based on feeding success and not predation avoidance. Since juveniles are the most susceptible to predation and presumably have less prior knowledge of food source location, these results have important implications in relation to predator-sensitive foraging and models of democratic group leadership. Subadults were subordinate to adult females, and their relationships were characterized by high levels of aggression. This aggression was especially common during the first half of the coati year (Nov-April), and subadults were more peripheralized during this time period. Subadults likely chose spatial positions to avoid aggression and were actively excluded from the center of the group by adult females. In the IguazA(0) coati groups, it appeared that food acquisition and social agonism were the major determinants driving spatial choice, while predation played little or no role. This paper demonstrates that within-group spatial structure can be a complex process shaped by differences in body size and nutritional requirements, food patch size and depletion rate, and social dominance status. How and why these factors interact is important to understanding the costs and benefits of sociality and emergent properties of animal group formation. C1 [Hirsch, Ben T.] Smithsonian Trop Res Inst, Dpo aa 340029898, Barro Colorado, Panama. [Hirsch, Ben T.] New York State Museum & Sci Serv, Albany, NY 12230 USA. RP Hirsch, BT (reprint author), Smithsonian Trop Res Inst, Unit 9100,Box 0948, Dpo aa 340029898, Barro Colorado, Panama. EM hirschb@si.edu FU National Science Fund [BCS-0314525] FX I would like to thank Yamil Di Blanco, Santiago Escobar, Carolina Ferrari, Fermino Silva, and Mauro Tammone for help and assistance during the course of the field work. I would also like to thank Viviana Munoz for her veterinary assistance. I am particularly grateful to Charles Janson for the immeasurable amount of advice he gave me during all aspects of this project and letting me borrow several pieces of much needed field equipment. I am also very thankful for the consistently helpful comments and advice from Mario Di Bitetti. This paper has benefited tremendously thanks to comments by Matt Gompper, Charles Janson, Andreas Koenig, Diane Doran-Sheehy, and two anonymous reviewers. I thank the APN for permission to carry out work in Iguazu. This study was funded in part by a National Science Fund grant (BCS-0314525). NR 40 TC 20 Z9 20 U1 10 U2 67 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 FEB PY 2011 VL 65 IS 2 BP 391 EP 399 DI 10.1007/s00265-010-1056-3 PG 9 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 707WR UT WOS:000286322200028 ER PT J AU Mascaro, J Schnitzer, SA AF Mascaro, Joseph Schnitzer, Stefan A. TI Dominance by the introduced tree Rhamnus cathartica (common buckthorn) may limit aboveground carbon storage in Southern Wisconsin forests SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Allometric regression; Aboveground biomass; Buckthorn; Carbon; Exotic-dominated ecosystems; New forests; Novel ecosystems; Succession ID GRASS INVASION; NATIVE SHRUBS; HAWAII; ECOPHYSIOLOGY; CONSEQUENCES; ECOSYSTEMS; SUCCESSION; DYNAMICS; BIOMASS; PLANTS AB Many ecosystems are now dominated by introduced species, and because dominant species drive ecosystem properties, these changes lead to increased uncertainty in estimates of carbon storage and cycling. We examined aboveground biomass in forests dominated by the introduced tree Rhamnus cathartica (common buckthorn) relative to forests dominated by native species, and measured aboveground biomass increment over a three-year period (2005-2008). Three of the four lowest biomass levels occurred in R. cathartica-dominated forests, and biomass in these forest types was stored primarily in trees 10-20 cm DBH. By contrast, forests dominated by native trees (including those with R. cathartica understories) had the six highest biomass levels, and biomass was stored primarily in trees >50 cm DBH. On average, forests dominated by R. cathartica stored half as much aboveground biomass (14.6 +/- 3.3 kg/m(2)) as forests dominated by native tree species (28.9 +/- 8.3 kg/m(2)). R. cathartica-dominated forests also had half the aboveground biomass increment of native-dominated forests (0.28 vs. 0.60 kg/m(2)/year). Although known anecdotally as a fast-growing species, R. cathartica growth rates declined with increasing size. Between 2005 and 2008, R. cathartica individuals <10 cm DBH grew faster than native species: however, R. cathartica individuals >10 cm DBH grew consistently slower than native species. Overall, our findings indicate that intrinsic size limitations on R. cathartica will lead to lower biomass stocks in forests where it acts as a canopy dominant relative to forests dominated by native tree species. (C) 2010 Elsevier B.V. All rights reserved. C1 [Mascaro, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94035 USA. [Mascaro, Joseph; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. [Mascaro, Joseph; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA. RP Mascaro, J (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94035 USA. EM jmascaro@stanford.edu OI Schnitzer, Stefan/0000-0002-2715-9455 FU Applied Ecological Services, Inc.; Friends of the Pheasant Branch Conservancy; NSF; UWM FX We thank the cities of Middleton, Madison, Brookfield, and Milwaukee. WI, as well as the WI Department of Natural Resources, University of Wisconsin - Madison Arboretum, Indian Mound Camp, and County of Milwaukee for site access. Several persons assisted in field work for this study, including R. Londre, S. Rutishauser, B. Jensen, M. Kaeske, L. Ingwell, and S. Servek. R. F. Hughes and C. Litton provided advice on allometry. Two anonymous reviewers provided comments that improved this manuscript. J. Mascaro was supported by a grant from Applied Ecological Services, Inc., a generous donation from the Friends of the Pheasant Branch Conservancy, a NSF Graduate Research Fellowship, and a UWM Golda Meir Library Scholar Award. NR 28 TC 4 Z9 4 U1 2 U2 31 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD FEB 1 PY 2011 VL 261 IS 3 BP 545 EP 550 DI 10.1016/j.foreco.2010.11.005 PG 6 WC Forestry SC Forestry GA 721DO UT WOS:000287333000023 ER PT J AU Plath, M Mody, K Potvin, C Dorn, S AF Plath, Mirco Mody, Karsten Potvin, Catherine Dorn, Silvia TI Establishment of native tropical timber trees in monoculture and mixed-species plantations: Small-scale effects on tree performance and insect herbivory SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Anacardium excelsum; Cedrela odorata; Insect herbivory; Pasture reforestation; Soil characteristics; Tabebuia rosea ID COSTA-RICA; ABOVEGROUND BIOMASS; HYPSIPYLA-GRANDELLA; SOIL INSECTICIDES; FOREST; DIVERSITY; GROWTH; PURE; PRODUCTIVITY; BIODIVERSITY AB Plantations of native timber species established on former pasture are a potential strategy to reduce the logging pressure on remnant natural forests in the tropics. Such plantations may help to mitigate or reverse the negative impacts of land degradation, and they may contribute to the long-term livelihood of livestock farmers. Planting native trees is, however, perceived as a risky activity due to limited knowledge of their performance and due to marked losses of newly established seedlings attributed to insect pests. Our study focuses on the small-scale effects of environmental heterogeneity, tree diversity and insecticide treatment on the performance of three native Central American timber species two years after establishment, and on damage inflicted by insect herbivores. Growth, survival and herbivore leaf damage were quantified for Anacardium excelsum (Anacardiaceae). Cedrela odorata (Meliaceae) and Tabebuia rosea (Bignoniaceae) planted in an experiment in Panama as (1) monocultures, (2) mixed stands, and (3) mixed stands protected by insecticides. Our study revealed that small-scale effects can have a substantial impact on the success of timber trees planted on former pasture. Growth performance and survival of the three species was strongly affected by small-scale environmental heterogeneity, which was expressed as significant differences in growth and survival among different plantation plots at the same study site. Establishment of trees in mixed stands did not have significant effects on tree survival and growth compared to pure stands, although it reduced herbivore pressure in one of the studied tree species. All tree species grew best and suffered lowest leaf damage when protected by insecticides, indicating a general influence of insect herbivory on growth of newly established trees. In contrast to growth performance, survival was not significantly affected by different management practices or herbivory. The large variability among plots in tree survival and growth, and also in the effects of management practices such as planting design and insecticide treatment, emphasizes the importance of small-scale environmental heterogeneity on tree survival and growth. (C) 2010 Elsevier B.V. All rights reserved. C1 [Plath, Mirco; Mody, Karsten; Dorn, Silvia] Swiss Fed Inst Technol, Inst Plant Anim & Agroecosyst Sci, CH-8092 Zurich, Switzerland. [Potvin, Catherine] Smithsonian Trop Res Inst, Panama City, Panama. RP Mody, K (reprint author), Swiss Fed Inst Technol, Inst Plant Anim & Agroecosyst Sci, Schmelzbergstr 9 LFO, CH-8092 Zurich, Switzerland. EM karsten.mody@ipw.agrl.ethz.ch FU Panamanian National Environmental Authority (ANAM); ETH North-South Centre FX We acknowledge the support by the Smithsonian Tropical Research Institute in administration and logistics. The Native Species Reforestation Project (PRORENA) provided the tree seedlings. We thank the University of Panama, in particular Hector Barrios, for infrastructure and reliable support. The Panamanian National Environmental Authority (ANAM) granted research, collecting and export permits. We are grateful to Wolfgang Einhauser-Treyer, Philipps-University Marburg, Germany, and the Machine Learning Laboratory of the ETH Zurich, Switzerland, for the development of the leaf herbivory software. The ETH Grassland Science group provided technical equipment for chemical analyses. We thank Jose Monteza and all local assistants in Sardinilla for help with fieldwork, as well as Andreas Muller, Jake Alexander and an anonymous referee for useful comments on the manuscript. This study has been supported by a grant of the ETH North-South Centre to S.D. and K.M. NR 82 TC 24 Z9 25 U1 5 U2 49 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD FEB 1 PY 2011 VL 261 IS 3 BP 741 EP 750 DI 10.1016/j.foreco.2010.12.004 PG 10 WC Forestry SC Forestry GA 721DO UT WOS:000287333000043 ER PT J AU Hershler, R Liu, HP Landye, JJ AF Hershler, Robert Liu, Hsiu-Ping Landye, J. Jerry TI TWO NEW GENERA AND FOUR NEW SPECIES OF FRESHWATER COCHLIOPID GASTROPODS (RISSOOIDEA) FROM NORTHEASTERN MEXICO SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID MITOCHONDRIAL-DNA SEQUENCES; NORTH-AMERICAN SOUTHWEST; PHYLOGENETIC-RELATIONSHIPS; HYDROBIIDAE GASTROPODA; AQUATIC GASTROPODS; TRYONIA; BIOGEOGRAPHY; BASIN; GENUS; PROSOBRANCHIA AB We describe four new species of cochliopid snails from thermal springs in northeastern Mexico (Chihuahua, Coahuila and Durango States). Two of these are placed in Pseudotryonia and represent the first Mexican records for this genus. They are diagnosed by unique or unique combinations of shell and anatomical characters, are well differentiated genetically from both each other and other congeners (mtCOI sequence divergence >= 2.0%) and were resolved as sister species within the Pseudotryonia clade in our molecular phylogenetic analyses. The other two species resemble Ipnobius, Pseudotryonia and Tryonia in having a thin, narrow shell, penis ornamented with a small number of glandular papillae and ovoviviparous reproductive mode, but are well differentiated (from these and each other) by other morphological/anatomical characters and mtCOI sequences (8.6-12.5% and 5.2-12.1% divergence, respectively) and consequently are placed in new monotypic genera (Chorrobius and Minckleyella). Chorrobius and Minckleyella formed a clade with Ipnobius, Mexipyrgus and Tryonia in all of our molecular phylogenetic analyses. Chorrobius was consistently delineated as a divergent lineage within this clade, but its relationships were otherwise unresolved. Minckleyella was nested within Tryonia in most of the trees and was sister to this genus in the others; despite this finding we erected a new genus for this snail because of its highly distinctive anatomical features and large genetic divergence relative to Tryonia (5.2 +/- 0.6%). Each of the four new species is endemic to highly disturbed single springs or local spring systems and may require protection. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll, Dept Biol, Denver, CO 80217 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. EM hershlerr@si.edu FU National Science Foundation [GB-6477x]; Smithsonian Biodiversity program FX J.J.L.'s early collections were made under the auspices of a National Science Foundation grant to W.L. Minckley (GB-6477x) and a collecting permit from the Secretaria de Industria y Comercio (# 5803). More recent fieldwork was supported by awards (to R.H.) from the Smithsonian Biodiversity program; collecting permits were provided by La Secretaria de Relaciones Exteriores (DAN 01874, 03358) and facilitated by Angelica Narvaez (U.S. Embassy Mexico City, Office of Environment, Science and Technology Affairs). We thank Andrew Simons and Jonathan Slaght (BellMNH) for loan of material under their care. Darrell Wong assisted with fieldwork, Yolanda Villacampa measured shells and prepared scanning electron micrographs, and Karolyn Darrow inked the anatomical drawings. This work was completed as part of the author's employment with the US federal government (Smithsonian Institution). NR 38 TC 3 Z9 4 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 J9 J MOLLUS STUD JI J. Molluscan Stud. PD FEB PY 2011 VL 77 BP 8 EP 23 DI 10.1093/mollus/eyq033 PN 1 PG 16 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 719RF UT WOS:000287225700002 ER PT J AU Janiszewska, K Stolarski, J Benzerara, K Meibom, A Mazur, M Kitahara, MV Cairns, SD AF Janiszewska, Katarzyna Stolarski, Jaroslaw Benzerara, Karim Meibom, Anders Mazur, Maciej Kitahara, Marcelo V. Cairns, Stephen D. TI A Unique Skeletal Microstructure of the Deep-Sea Micrabaciid Scleractinian Corals SO JOURNAL OF MORPHOLOGY LA English DT Article DE azooxanthellate scleractinian corals; biomineralization; microstructure; nanostructure ID GENUS ACROPORA SCLERACTINIA; GROWTH; BIOMINERALIZATION; PHYLOGENY; EVIDENCES; PROTEINS; FIBERS; NACRE; SCALE AB Micrabaciids are solitary, exclusively azooxanthellate deep-sea corals belonging to one of the deepest-living (up to 5,000 m) scleractinian representatives. All modern micrabaciid taxa (genera: Letepsammia, Rhombopsammia, Stephanophyllia, Leptopenus) have a porous and often very fragile skeleton consisting of two main microstructural components known also from other scleractinians: rapid accretion deposits and thickening deposits. However, at the microstructural level, the skeletal organization of the micrabaciids is distinctly different from that of other scleractinians. Rapid accretion deposits consist of alternations of superimposed "microcrystalline" (micrometer-sized aggregates of nodular nanodomains) and fibrous zones. In contrast to all shallow-water and sympatric deep-water corals so far described, the thickening deposits of micrabaciids are composed of irregular meshwork of short (1-2 mu m) and extremely thin (ca. 100-300 am) fibers organized into small, chip-like bundles (ca. 1-2 mu m thick). Longer axes of fiber bundles are usually subparallel to the skeletal surfaces and oriented variably in this plane. The unique microstructural organization of the micrabaciid skeleton is consistent with their monophyletic status based on macromorphological and molecular data, and points to a diversity of organic matrix-mediated biomineralization strategies in Scleractinia. J. Morphol. 272:191-203, 2011. (C) 2010 Wiley-Liss, Inc. C1 [Janiszewska, Katarzyna; Stolarski, Jaroslaw] Inst Paleobiol, PL-00818 Warsaw, Poland. [Benzerara, Karim] CNRS, UMR 7590, Inst Mineral & Phys Milieux Condenses, F-75015 Paris, France. [Benzerara, Karim] Univ Paris 06, IPGP, F-75015 Paris, France. [Benzerara, Karim] Univ Paris 07, IPGP, F-75015 Paris, France. [Meibom, Anders] Museum Natl Hist Nat, LMCM, UMR 7202, F-75005 Paris, France. [Mazur, Maciej] Univ Warsaw, Dept Chem, Lab Electrochem, PL-02093 Warsaw, Poland. [Kitahara, Marcelo V.] James Cook Univ, ARC Ctr Excellence Coral Reefs Studies, Townsville, Qld 4811, Australia. [Kitahara, Marcelo V.] James Cook Univ, Coral Genom Grp, Townsville, Qld 4811, Australia. [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Stolarski, J (reprint author), Inst Paleobiol, Twarda 51-55, PL-00818 Warsaw, Poland. EM stolacy@twarda.pan.pl RI Kitahara, Marcelo/D-5560-2011; Benzerara, Karim/J-1532-2016; IMPMC, Geobio/F-8819-2016 OI Benzerara, Karim/0000-0002-0553-0137; FU Polish Ministry of Science and Higher Education [N307-015733]; Museum d'Histoire Naturelle in Paris; European Research Council [246749]; Region Ile-de-France [SESAME 2000 E 1435 (JEOL JEM-2100F)]; INSU-CNRS; INP-CNRS; University Pierre et Marie Curie-Paris 6 FX Contract grant sponsor: Polish Ministry of Science and Higher Education; Contract grant number: project N307-015733; Contract grant sponsor: Museum d'Histoire Naturelle in Paris; Contract grant sponsor: European Research Council Advanced Grant; Contract grant number: 246749 (BIOCARB); Contract grant sponsor: Region Ile-de-France; Contract grant number: SESAME 2000 E 1435 (JEOL JEM-2100F); Contract grant sponsors: INSU-CNRS, INP-CNRS and University Pierre et Marie Curie-Paris 6. NR 51 TC 17 Z9 17 U1 0 U2 6 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD FEB PY 2011 VL 272 IS 2 BP 191 EP 203 DI 10.1002/jmor.10906 PG 13 WC Anatomy & Morphology SC Anatomy & Morphology GA 717PX UT WOS:000287061000006 PM 21210490 ER PT J AU Uribe, MC Grier, HJ AF Uribe, Mari Carmen Grier, Harry J. TI Oogenesis of Microlecithal Oocytes in the Viviparous Teleost Heterandria formosa SO JOURNAL OF MORPHOLOGY LA English DT Article DE oogenesis; microlecithal oocyte; viviparity; poeciliids; Heterandria formosa ID POECILIID FISHES; OVARIAN-FOLLICLE; LEAST KILLIFISH; LEBISTES RETICULATUS; GERMINAL EPITHELIUM; GROWTH; MATURATION; GAMBUSIA; EVOLUTION; PLACENTA AB Viviparous teleosts exhibit two patterns of embryonic nutrition: lecithotrophy (when nutrients are derived from yolk that is deposited in the oocyte during oogenesis) and matrotrophy (when nutrients are derived from the maternal blood stream during gestation). Nutrients contained in oocytes of matrotrophic species are not sufficient to support embryonic development until term. The smallest oocytes formed among the viviparous poeciliid fish occur in the least killifish, Heterandria formosa, these having diameters of only 400 pm. Accordingly, H. formosa presents the highest level of matrotrophy among poeciliids. This study provides histological details occurring during development of its microlecithal oocytes. Five stages occur during oogenesis: oogonial proliferation, chromatin nucleolus, primary growth (previtellogenesis), secondary growth (vitellogenesis), and oocyte maturation. H. formosa, as in all viviparous poeciliids, has intrafollicular fertilization and gestation. Therefore, there is no ovulation stage. The full-grown oocyte of H. formosa contains a large oil globule, which occupies most of the cell volume. The oocyte periphery contains the germinal vesicle, and ooplasm that includes cortical alveoli, small oil droplets and only a few yolk globules. The follicular cell layer is initially composed of a single layer of squamous cells during early previtellogenesis, but these become columnar during early vitellogenesis. They are pseudostratified during late vitellogenesis and reduce their height becoming almost squamous in full-grown oocytes. The microlecithal oocytes of H. formosa represent an extreme in fish oogenesis typified by scarce yolk deposition, a characteristic directly related to matrotrophy. J. Morphol. 272:241-257, 2011. (C) 2010 Wiley-Liss, Inc. C1 [Uribe, Mari Carmen] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Biol Comparada, Mexico City 04510, DF, Mexico. [Grier, Harry J.] Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. [Grier, Harry J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. RP Uribe, MC (reprint author), Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Biol Comparada, Ciudad Univ,Insurgentes 3000, Mexico City 04510, DF, Mexico. EM uribearanzabal@yahoo.com.mx NR 52 TC 11 Z9 12 U1 1 U2 6 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD FEB PY 2011 VL 272 IS 2 BP 241 EP 257 DI 10.1002/jmor.10912 PG 17 WC Anatomy & Morphology SC Anatomy & Morphology GA 717PX UT WOS:000287061000009 PM 21210493 ER PT J AU Thiele, KR Funk, VA Iwatsuki, K Morat, P Peng, CI Raven, PH Sarukhan, J Seberg, O AF Thiele, Kevin R. Funk, Vicki A. Iwatsuki, Kunio Morat, Philippe Peng, Ching-I Raven, Peter H. Sarukhan, Jose Seberg, Ole TI The controversy over the retypification of Acacia Mill. with an Australian type: A pragmatic view SO TAXON LA English DT Editorial Material DE Acacia; botanical nomenclature; conservation of names; International Botanical Congress; International Code of Botanical Nomenclature ID NOMENCLATURE SECTION; MIMOSOIDEAE; LEGUMINOSAE AB The conservation of Acacia with an Australian type has been perhaps the most controversial issue to have been dealt with under the International Code of Botanical Nomenclature in many years. Before, during and since the vote on the matter at the Seventeenth International Botanical Congress in Vienna, strong opinions have been expressed in print, on the web and in the popular media. Opponents of the Vienna decision are currently focusing on details of the process by which the vote was conducted, rather than on the merits or otherwise of the original proposal. They have signalled an intention to challenge and to try to overturn the Vienna decision at the Melbourne Congress. We are a group of taxonomists, from a range of backgrounds and with a range of opinions on the original proposal, who believe that the Vienna process was fundamentally sound, and that continuance of this argument in its current form is damaging to the international nomenclatural consensus. We provide this paper as, we hope, an objective, non-partisan summary of the issue and conclude with the recommendation that the international taxonomic community should accept the retypification of Acacia and move on. C1 [Thiele, Kevin R.] Western Australia Herbarium, Bentley Dc, WA 6983, Australia. Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA. Univ Tokyo, Bot Gardens, Bunkyo Ku, Tokyo 1120001, Japan. Museum Natl Hist Nat, Dept Systemat & Evolut, Herbier Plantes Vasculaires, UMS 0602, Paris, France. Acad Sinica, Herbarium, Biodivers Res Ctr, Taipei 115, Taiwan. Missouri Bot Garden, St Louis, MO 63166 USA. Comis Nacl Conocimiento & Uso Biodiversidad CONAB, Mexico City 14010, DF, Mexico. Nat Hist Museum Denmark, Bot Garden & Museum, DK-1307 Copenhagen K, Denmark. RP Thiele, KR (reprint author), Western Australia Herbarium, Locked Bag 104, Bentley Dc, WA 6983, Australia. EM kevin.thiele@dec.wa.gov.au RI Seberg, Ole/A-5111-2013 OI Seberg, Ole/0000-0001-9675-4090 NR 20 TC 16 Z9 18 U1 3 U2 8 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD FEB PY 2011 VL 60 IS 1 BP 194 EP 198 PG 5 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 725FS UT WOS:000287631200017 ER PT J AU Anderson, GE Gaensler, BM Kaplan, DL Posselt, B Slane, PO Murray, SS Mauerhan, JC Benjamin, RA Brogan, CL Chakrabarty, D Drake, JJ Drew, JE Grindlay, JE Hong, J Lazio, TJW Lee, JC Steeghs, DTH van Kerkwijk, MH AF Anderson, Gemma E. Gaensler, B. M. Kaplan, David L. Posselt, Bettina Slane, Patrick O. Murray, Stephen S. Mauerhan, Jon C. Benjamin, Robert A. Brogan, Crystal L. Chakrabarty, Deepto Drake, Jeremy J. Drew, Janet E. Grindlay, Jonathan E. Hong, Jaesub Lazio, T. Joseph W. Lee, Julia C. Steeghs, Danny T. H. van Kerkwijk, Marten H. TI IDENTIFICATION OF A POPULATION OF X-RAY-EMITTING MASSIVE STARS IN THE GALACTIC PLANE SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: winds, outflows; stars: Wolf-Rayet; supergiants; X-rays: binaries; X-rays: individual (AX J163252-4746, AX J184738-0156, AX J144701-5919, AX J144547-5931); X-rays: stars ID H-II REGIONS; CARINA OB1 ASSOCIATION; RADIO-EMISSION MODELS; WIND BINARY-SYSTEMS; COLLIDING WINDS; NONTHERMAL EMISSION; SOURCE CATALOG; VIITH CATALOG; INNER GALAXY; HOT STARS AB We present X-ray, infrared, optical, and radio observations of four previously unidentified Galactic plane X-ray sources: AX J163252-4746, AX J184738-0156, AX J144701-5919, and AX J144547-5931. Detection of each source with the Chandra X-ray Observatory has provided sub-arcsecond localizations, which we use to identify bright infrared counterparts to all four objects. Infrared and optical spectroscopy of these counterparts demonstrate that all four X-ray sources are extremely massive stars, with spectral classifications: Ofpe/WN9 (AX J163252-4746), WN7 (AX J184738-0156 = WR121a), WN7-8h (AX J144701-5919), and OIf(+) (AX J144547-5931). AX J163252-4746 and AX J184738-0156 are both luminous, hard, X-ray emitters with strong Fe XXV emission lines in their X-ray spectra at similar to 6.7 keV. The multi-wavelength properties of AX J163252-4746 and AX J184738-0156 are not consistent with isolated massive stars or accretion onto a compact companion; we conclude that their X-ray emission is most likely generated in a colliding-wind binary (CWB) system. For both AX J144701-5919 and AX J144547-5931, the X-ray emission is an order of magnitude less luminous and with a softer spectrum. These properties are consistent with a CWB interpretation for these two sources also, but other mechanisms for the generation of X-rays cannot be excluded. There are many other as yet unidentified X-ray sources in the Galactic plane, with X-ray properties similar to those seen for AX J163252-4746, AX J184738-0156, AX J144701-5919, and AX J144547-5931. This may indicate a substantial population of X-ray-emitting massive stars and CWBs in the Milky Way. C1 [Anderson, Gemma E.; Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys A29, Sydney, NSW 2006, Australia. [Kaplan, David L.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Posselt, Bettina; Slane, Patrick O.; Murray, Stephen S.; Drake, Jeremy J.; Grindlay, Jonathan E.; Hong, Jaesub; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mauerhan, Jon C.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Benjamin, Robert A.] Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA. [Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Chakrabarty, Deepto] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Drew, Janet E.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Lazio, T. Joseph W.] USN, Res Lab, Washington, DC 20375 USA. [Steeghs, Danny T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [van Kerkwijk, Marten H.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Anderson, GE (reprint author), Univ Sydney, Sydney Inst Astron, Sch Phys A29, Sydney, NSW 2006, Australia. EM g.anderson@physics.usyd.edu.au RI Steeghs, Danny/C-5468-2009; Gaensler, Bryan/F-8655-2010; Lee, Julia/G-2381-2015; OI Steeghs, Danny/0000-0003-0771-4746; Lee, Julia/0000-0002-7336-3588; Anderson, Gemma/0000-0001-6544-8007; Posselt, Bettina/0000-0003-2317-9747; Gaensler, Bryan/0000-0002-3382-9558; Drew, Janet/0000-0003-1192-7082 FU Australian Postgraduate Award; Australian Research Council [FF0561298]; NASA, STScI [51230.01-A, NAS 5-26555]; NASA [NAS8-03060, NAS8-39073, GO9-0155X]; STFC; NRL; Commonwealth of Australia for operation; NFS FX Special thanks goes to Michael Muno for his encouragement, expertise, and participation in this project. We also thank Sean Farrell, Stan Owocki, and Nathan Smith for their advice and help with this research and the referee for his or her constructive response and suggestions. G. E. A acknowledges the support of an Australian Postgraduate Award. B. M. G. acknowledges the support of a Federation Fellowship from the Australian Research Council through grant FF0561298. D. L. K. was supported by NASA through Hubble Fellowship grant 51230.01-A awarded by the STScI, which is operated by AURA, for NASA, under contract NAS 5-26555. P.O.S. acknowledges partial support from NASA Contract NAS8-03060. D. T. H. S. acknowledges an STFC Advanced Fellowship. J.J.D was supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC). Basic research in radio astronomy at the NRL is supported by 6.1 Base funding. Support for this work was also provided by NASA through Chandra Award Number GO9-0155X issued by the CXC, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. This research makes use of data obtained with the Chandra X-ray Observatory, and software provided by the CXC in the application packages CIAO and Sherpa. OSIRIS is a collaborative project between Ohio State University and CTIO. Observing time on the 6.5m Clay and Baade Magellan Telescopes, located at Las Campanas Observatory, was allocated through the Harvard-Smithsonian Center for Astrophysics. The ATCA, part of the Australia Telescope, is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This publication makes use of data products from the second catalogue of serendipitous X-ray sources (2XMMi) from the European Space Agency's (ESA) XMM-Newton observatory. These data were accessed through the Leicester Database and Archive Service at Leicester University, UK. 2MASS is a joint project of the University of Massachusetts and the IPAC/Caltech, funded by the NASA and NFS. GLIMPSE survey data are part of the Spitzer Legacy Program. The Spitzer Space Telescope is operated by the JPL/Caltech under a contract with NASA. This research has made use of NASA's Astrophysics Data System. NR 88 TC 14 Z9 14 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2011 VL 727 IS 2 AR 105 DI 10.1088/0004-637X/727/2/105 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000044 ER PT J AU Chan, CK AF Chan, Chi-Kwan TI A CLASS OF PHYSICALLY MOTIVATED CLOSURES FOR RADIATION HYDRODYNAMICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; radiative transfer ID FLUX-LIMITED DIFFUSION; VARIABLE EDDINGTON FACTOR; LATTICE BOLTZMANN METHOD; PLANE-PARALLEL FLOW; BLACK-HOLES; SPHERICAL ACCRETION; MOMENT METHOD; EQUATIONS; APPROXIMATION; ALGORITHMS AB Radiative transfer and radiation hydrodynamics use the relativistic Boltzmann equation to describe the kinetics of photons. It is difficult to solve the six-dimensional time-dependent transfer equation unless the problem is highly symmetric or in equilibrium. When the radiation field is smooth, it is natural to take angular moments of the transfer equation to reduce the degrees of freedom. However, low order moment equations contain terms that depend on higher order moments. To close the system of moment equations, approximations are made to truncate this hierarchy. Popular closures used in astrophysics include flux-limited diffusion and the M-1 closure, which are rather ad hoc and do not necessarily capture the correct physics. In this paper, we propose a new class of closures for radiative transfer and radiation hydrodynamics. We start from a different perspective and highlight the consistency of a fully relativistic formalism. We present a generic framework to approximate radiative transfer based on relativistic Grad's moment method. We then derive a 14-field method that minimizes unphysical photon self-interaction. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Chan, CK (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM ckchan@cfa.harvard.edu FU ITC FX This work is originally motivated by Feryal Ozel and Dimitrios Psaltis. It is a pleasure to thank Ramesh Narayan for his intuitions on resolving many technical difficulties. The author thanks Chris Fryer, Avi Loeb, George Rybicki, and Dimitri Mihalas for helpful comments on moment methods. The PiTP 2009 lectures by Jim Stone and Mike Norman are extremely useful. The author is grateful for discussions with Martin Pessah, Mark Dijkstra, Hy Trac, Mike Sekora, Sukanya Chakrabarti, Robert Marcus, and Alexander Tchekhovskoy. The author is currently supported by an ITC fellowship. NR 64 TC 1 Z9 1 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2011 VL 727 IS 2 AR 67 DI 10.1088/0004-637X/727/2/67 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000006 ER PT J AU Wilson, CD Warren, BE Irwin, J Knapen, JH Israel, FP Serjeant, S Attewell, D Bendo, GJ Brinks, E Butner, HM Clements, DL Leech, J Matthews, HE Muhle, S Mortier, AMJ Parkin, TJ Petitpas, G Tan, BK Tilanus, RPJ Usero, A Vaccari, M van der Werf, P Wiegert, T Zhu, M AF Wilson, C. D. Warren, B. E. Irwin, J. Knapen, J. H. Israel, F. P. Serjeant, S. Attewell, D. Bendo, G. J. Brinks, E. Butner, H. M. Clements, D. L. Leech, J. Matthews, H. E. Muhle, S. Mortier, A. M. J. Parkin, T. J. Petitpas, G. Tan, B. K. Tilanus, R. P. J. Usero, A. Vaccari, M. van der Werf, P. Wiegert, T. Zhu, M. TI The JCMT Nearby Galaxies Legacy Survey - IV. Velocity dispersions in the molecular interstellar medium in spiral galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: molecules; galaxies: ISM; galaxies: kinematics and dynamics; galaxies: spiral ID MASSIVE DISK GALAXIES; STAR-FORMATION; GALACTIC DISK; VIRGO CLUSTER; H-I; GRAVITATIONAL-INSTABILITY; SUBMILLIMETER GALAXIES; SOLAR NEIGHBORHOOD; DWARF GALAXIES; SMALLER CLOUDS AB An analysis of large-area CO J = 3-2 maps from the James Clerk Maxwell Telescope for 12 nearby spiral galaxies reveals low velocity dispersions in the molecular component of the interstellar medium. The three lowest luminosity galaxies show a relatively flat velocity dispersion as a function of radius while the remaining nine galaxies show a central peak with a radial fall-off within 0.2-0.4r(25). Correcting for the average contribution due to the internal velocity dispersions of a population of giant molecular clouds, the average cloud-cloud velocity dispersion across the galactic discs is 6.1 +/- 1.0 km s-1 (standard deviation of 2.9 km s-1), in reasonable agreement with previous measurements for the Galaxy and M33. The cloud-cloud velocity dispersion derived from the CO data is on average two times smaller than the H i velocity dispersion measured in the same galaxies. The low cloud-cloud velocity dispersion implies that the molecular gas is the critical component determining the stability of the galactic disc against gravitational collapse, especially in those regions of the disc which are H-2 dominated. The cloud-cloud velocity dispersion shows a significant positive correlation with both the far-infrared luminosity, which traces the star formation activity, and the K-band absolute magnitude, which traces the total stellar mass. For three galaxies in the Virgo cluster, smoothing the data to a resolution of 4.5 kpc (to match the typical resolution of high-redshift CO observations) increases the measured velocity dispersion by roughly a factor of 2, comparable to the dispersion measured recently in a normal galaxy at z = 1. This comparison suggests that the mass and star formation rate surface densities may be similar in galaxies from z = 0 to 1 and that the high star formation rates seen at z = 1 may be partly due to the presence of physically larger molecular gas discs. C1 [Wilson, C. D.; Warren, B. E.; Attewell, D.; Parkin, T. J.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Irwin, J.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Knapen, J. H.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Knapen, J. H.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Israel, F. P.; van der Werf, P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Bendo, G. J.; Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Brinks, E.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Butner, H. M.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Leech, J.; Tan, B. K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Matthews, H. E.] Natl Res Council Canada, Herzberg Inst Astrophys, DRAO, Penticton, BC V2A 69J, Canada. [Muhle, S.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Mortier, A. M. J.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tilanus, R. P. J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Usero, A.] OAN, Observ Madrid, E-28014 Madrid, Spain. [Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Wiegert, T.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Zhu, M.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Wilson, CD (reprint author), McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. EM wilson@physics.mcmaster.ca RI Vaccari, Mattia/R-3431-2016; OI Vaccari, Mattia/0000-0002-6748-0577; Butner, Harold/0000-0003-4899-2064; Brinks, Elias/0000-0002-7758-9699 FU NSERC (Canada); UK Science & Technology Facilities Council; National Aeronautics and Space Administration; National Research Council (Canada) FX We thank the anonymous referee for a referee report which spurred us to re-examine our data processing choices and resulted in a significant improvement in the paper. The James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research and the National Research Council of Canada. The research of JI and CDW is supported by grants from NSERC (Canada). AU has been supported through a Post-Doctoral Research Assistantship from the UK Science & Technology Facilities Council. Travel support for BEW and TW was supplied by the National Research Council (Canada). We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr) and thank R.N. Henriksen for useful discussions. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 80 TC 20 Z9 20 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 410 IS 3 BP 1409 EP 1422 DI 10.1111/j.1365-2966.2010.17646.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703TN UT WOS:000286004300002 ER PT J AU Murphy, KR AF Murphy, Kathleen R. TI A Note on Determining the Extent of the Water Raman Peak in Fluorescence Spectroscopy SO APPLIED SPECTROSCOPY LA English DT Article DE Fluorescence spectroscopy; Intensity standardization; Calibration; MATLAB program; Water Raman peak; Instrumentation ID ORGANIC-MATTER; CALIBRATION AB A method is proposed for automatically determining the upper and lower boundaries of the Raman scatter peak in fluorescence spectroscopy from empirical data. Accurate peak boundaries are needed to calculate accurate Raman peak areas, used for normalizing fluorescence signals to produce data in units that are comparable between instruments. Comparisons of Raman peak boundaries across nine individual instruments (FluoroMax 3 (FM3) fluorometers from HORIBA Jobin Yvon and Cary Eclipse (CE) fluorometers from Varian Inc.) at the excitation wavelength lambda(ex) = 350 nm reveal consistent results. At 350 nm excitation, the Raman peak was confined by the emission wavelengths of 382-418 nm, with boundaries determined for the FM3 fluorometers deviating by no more than 0.5 nm and 1.5 nm with respect to the start and end of the peak, and CE fluorometers deviating by up to 1.5 nm and 2 nm, respectively. Peak width was a function of fluorometer type and excitation wavelength. For the FM3 instruments, widths increased from approximately 30 nm at lambda(ex) = 300 nm to 40 nm at lambda(ex) = 380 nm, while for the CE instruments, peaks were approximately 5-8 nm narrower. Code for implementing the procedure in MATLAB, which allows for the adjustment of input parameters to compensate for noisy data, is provided in the Supplemental Material (available online). C1 [Murphy, Kathleen R.] Univ New S Wales, Sch Civil & Environm Engn, Sydney, NSW 2052, Australia. [Murphy, Kathleen R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Murphy, KR (reprint author), Univ New S Wales, Sch Civil & Environm Engn, Sydney, NSW 2052, Australia. EM krm@unsw.edu.au RI Murphy, Kathleen/B-8217-2009 OI Murphy, Kathleen/0000-0001-5715-3604 FU US Geological Survey; NASA [NNH04AA62I] FX The author thanks participants in the 2008 AGU Chapman Conference on Organic Matter Fluorescence, convened by A. Baker and P. Coble and funded by the US Geological Survey, and NASA Grant NNH04AA62I, for providing the data described in this paper. NR 6 TC 3 Z9 3 U1 2 U2 31 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 5320 SPECTRUM DRIVE SUITE C, FREDERICK, MD 21703 USA SN 0003-7028 J9 APPL SPECTROSC JI Appl. Spectrosc. PD FEB PY 2011 VL 65 IS 2 BP 233 EP 236 DI 10.1366/10-06136 PG 4 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 710XE UT WOS:000286549500016 ER PT J AU Wilson, AG Arcese, P Chan, YL Patten, MA AF Wilson, Amy G. Arcese, Peter Chan, Yvonne L. Patten, Michael A. TI Micro-spatial genetic structure in song sparrows (Melospiza melodia) SO CONSERVATION GENETICS LA English DT Article DE Spatial autocorrelation; Genetic structure; Isolation by distance; Islands ID MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; AUTOCORRELATION ANALYSIS; PACIFIC COAST; DIFFERENTIATION MEASURE; ALEXANDER ARCHIPELAGO; WILDLIFE MANAGEMENT; CERVUS-ELAPHUS; FLOW; CONSERVATION AB The spatial genetic structure of populations is strongly influenced by current and historical patterns of gene flow and drift, which in the simplest case, is limited by geographic distance. We examined the microspatial genetic structure within 33 populations of song sparrows (Melospiza melodia) which included eight subspecies located across coastal areas in southern British Columbia (BC) and California. We also examined the effect of water barriers and local density estimates on genetic structuring. Across both regions, positive genetic structure was detectable at distances of less than 10 km. Genetic divergence was highest in Californian subspecies, perhaps due to reduced gene flow across sub-specific contact zones. In BC, populations distributed across islands displayed greater genetic structuring over similar spatial scales than those across mainland sites, supporting the prediction that water barriers reduce gene flow in this species. Our results confirm both the expectation for fine-scale genetic structure in these generally sedentary subspecies, and the role of landscape features in generating geographic variation in genetic structure. C1 [Wilson, Amy G.; Arcese, Peter] Univ British Columbia, Ctr Appl Conservat Res, Vancouver, BC V6T 1Z4, Canada. [Wilson, Amy G.] Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Chan, Yvonne L.] Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. [Patten, Michael A.] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73019 USA. RP Wilson, AG (reprint author), Univ British Columbia, Ctr Appl Conservat Res, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM asg.wilson@gmail.com RI Chan, Yvonne/A-3383-2009 FU NSERC; American Ornithologists Union Bleitz Grant; Friends of Ecological Reserves FX We thank S. Wilson, A. Marr, L.F. Keller, J.M.N Smith, C. Begus, C. Ritland, A. Miscampbell, H. Yueh, W. Easton, and J. Hope for assistance on various aspects of this study. Site access was provided by the Tsawout and Tseycum Bands, A. and H. Brumbaum, T. and M. Boyle, Parks Canada, Canadian Wildlife Service, Nature Trust, Powell River Municipality, and Sooke Municipal District. We gratefully acknowledge financial support from NSERC, American Ornithologists Union Bleitz Grant and the Friends of Ecological Reserves. All work was conducted under permits of the UBC Animal Care Committee and Environment Canada. This manuscript benefitted from comments made by V. Friesen, E. Taylor, D. Irwin, S. Aitken, K. Cheng, S. Wilson and two anonymous reviewers. NR 81 TC 11 Z9 11 U1 0 U2 30 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PD FEB PY 2011 VL 12 IS 1 BP 213 EP 222 DI 10.1007/s10592-010-0134-4 PG 10 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 703IP UT WOS:000285971900019 ER PT J AU Lee, TS Nagamine, K Hernquist, L Springel, V AF Lee, T. S. Nagamine, K. Hernquist, L. Springel, V. TI Cross-correlation between damped Ly alpha systems and Lyman break galaxies in cosmological SPH simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: formation; quasars: absorption lines; galaxies: star formation; cosmology: theory ID PARTICLE HYDRODYNAMICS SIMULATIONS; HIGH-REDSHIFT GALAXIES; DARK-MATTER UNIVERSE; STAR-FORMATION; STELLAR POPULATIONS; LARGE-SCALE; ABSORBERS; Z-SIMILAR-TO-3; EVOLUTION; ABSORPTION AB We calculate the cross-correlation function (CCF) between damped Ly alpha systems (DLAs) and Lyman break galaxies (LBGs) using cosmological hydrodynamic simulations at z = 3. We compute the CCF with two different methods. First, we assume that there is one DLA in each dark matter halo if its DLA cross-section is non-zero. In our second approach we weight the pair count by the DLA cross-section of each halo, yielding a cross-section-weighted CCF. We also compute the angular CCF for direct comparison with observations. Finally, we calculate the autocorrelation functions of LBGs and DLAs, and their bias against the dark matter distribution. For these different approaches, we consistently find that there is good agreement between our simulations and observational measurements by Cooke et al. and Adelberger et al.. Our results thus confirm that the spatial distribution of LBGs and DLAs can be well described within the framework of the concordance Lambda cold dark matter model. We find that the correlation strengths of LBGs and DLAs are consistent with the actual observations, and in the case of LBGs it is higher than would be predicted by low-mass galaxy merger models. C1 [Lee, T. S.; Nagamine, K.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Hernquist, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, V.] Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Lee, TS (reprint author), Univ Nevada, Dept Phys & Astron, 4505 Maryland Pkwy, Las Vegas, NV 89154 USA. EM tslee@physics.unlv.edu; kn@physics.unlv.edu FU National Aeronautics and Space Administration [NNX08AE57A]; UNLV FX This work is supported in part by the National Aeronautics and Space Administration under Grant/Cooperative Agreement No. NNX08AE57A issued by the Nevada NASA EPSCoR programme and the President's Infrastructure Award at UNLV. KN is grateful for the hospitality of the Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, where part of this work was done. The simulations were performed at the Institute of Theory and Computation at Harvard-Smithsonian Center for Astrophysics, and the analysis was performed at the UNLV Cosmology Computing Cluster. NR 53 TC 4 Z9 4 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 411 IS 1 BP 54 EP 64 DI 10.1111/j.1365-2966.2010.17668.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710QF UT WOS:000286525600019 ER PT J AU Gallo, LC Miniutti, G Miller, JM Brenneman, LW Fabian, AC Guainazzi, M Reynolds, CS AF Gallo, L. C. Miniutti, G. Miller, J. M. Brenneman, L. W. Fabian, A. C. Guainazzi, M. Reynolds, C. S. TI Multi-epoch X-ray observations of the Seyfert 1.2 galaxy Mrk 79: bulk motion of the illuminating X-ray source SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: Mrk 79; galaxies: individual: UGC3973; galaxies: nuclei; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; XMM-NEWTON OBSERVATIONS; IRON L LINE; PLASMA DIAGNOSTICS; ACCRETION DISCS; REFLECTION; EMISSION; VARIABILITY; REVERBERATION AB Multi-epoch X-ray spectroscopy (0.3-25 keV) of the Seyfert 1.2 galaxy Mrk 79 (UGC3973) spanning nearly 8 yr and a factor of 3 in broad-band flux are analysed. The data are obtained at seven epochs with either XMM-Newton or Suzaku. Comparison with contemporaneous RXTE monitoring indicates that all flux states of Mrk 79 are represented by the data. The spectra are fitted in a self-consistent manner adopting a power law and ionized reflection to describe the broad-band continuum. Modification of the spectra by a distant photoionized medium, seen predominantly in emission, is also included. Under the assumption that the inner disc is at the innermost stable circular orbit, our blurred reflection models give a spin of a = 0.7 +/- 0.1. The reflection component in each spectrum is weaker than that predicted by simple reflection models. If the illuminating X-ray emission is produced by flares above the disc that move at mildly relativistic velocities, however, diminished reflection is expected. Light bending due to strong gravity near black holes can influence how the illuminating and reflected fluxes are observed; variations in Mrk 79 do not suggest that light bending is important in this source. C1 [Gallo, L. C.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Miniutti, G.] LAEFF, Ctr Astrobiol CSIC INTA, Dept Astrofis, E-28691 Madrid, Spain. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Brenneman, L. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Guainazzi, M.] ESA, European Space Astron Ctr, E-28080 Madrid, Spain. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, C. S.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA. RP Gallo, LC (reprint author), St Marys Univ, Dept Phys & Astron, 923 Robie St, Halifax, NS B3H 3C3, Canada. EM lgallo@ap.smu.ca RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009 OI Miniutti, Giovanni/0000-0003-0707-4531; FU ESA; USA (NASA) FX The XMM-Newton project is an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). Thanks to Damien Robertson for alphaox measurements and Phil Uttley for the RXTE light curve. NR 59 TC 30 Z9 30 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 FEB PY 2011 VL 411 IS 1 BP 607 EP 619 DI 10.1111/j.1365-2966.2010.17705.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710QF UT WOS:000286525600065 ER PT J AU Siwak, M Rucinski, SM Matthews, JM Pojmanski, G Kuschnig, R Guenther, DB Moffat, AFJ Sasselov, D Weiss, WW AF Siwak, Michal Rucinski, Slavek M. Matthews, Jaymie M. Pojmanski, Grzegorz Kuschnig, Rainer Guenther, David B. Moffat, Anthony F. J. Sasselov, Dimitar Weiss, Werner W. TI Analysis of variability of TW Hya as observed by MOST and ASAS in 2009 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: individual: TW Hya; stars: rotation ID MAGNETIC NEUTRON-STARS; MAGNETOSPHERIC ACCRETION MODELS; QUASI-PERIODIC OSCILLATIONS; TAURI STARS; YOUNG STARS; DISK; HYDRAE; SIMULATIONS; PHOTOMETRY; ROTATION AB As a continuation of our previous studies in 2007 and 2008, new photometric observations of the T Tauri star TW Hya obtained by the MOST satellite and the All Sky Automated Survey (ASAS) project over 40 d in 2009 with temporal resolution of 0.2 d are presented. A wavelet analysis of the combined MOST-ASAS data provides a rich picture of coherent, intermittent, variable-period oscillations, similarly as discovered in the 2008 data. The periods (1.3-10 d) and systematic period shortening on time-scales of weeks can be interpreted within the model of magnetorotationally controlled accretion processes in the inner accretion disc around the star. Within this model and depending on the assumed visibility of plasma parcels causing the oscillations, the observed shortest oscillation period may indicate the stellar rotation period of 1.3 or 2.6 d, synchronized with the disc at 4.5 or 7.1 R-circle dot, respectively. C1 [Siwak, Michal; Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Pojmanski, Grzegorz] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, David B.] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Moffat, Anthony F. J.] Univ Montreal, Ctr Rech Astrophys Quebec, Montreal, PQ H3C 3J7, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Siwak, M (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM siwak@astro.utoronto.ca FU Natural Sciences and Engineering Research Council of Canada; Canadian Space Agency; Austrian Space Agency; Austrian Science Fund FX The Natural Sciences and Engineering Research Council of Canada supports the research of DBG, JMM, AFJM and SMR. Additional support for AFJM comes from FQRNT (Quebec). RK is supported by the Canadian Space Agency and WWW is supported by the Austrian Space Agency and the Austrian Science Fund. NR 28 TC 11 Z9 11 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 FEB PY 2011 VL 410 IS 4 BP 2725 EP 2729 DI 10.1111/j.1365-2966.2010.17649.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706IG UT WOS:000286211000054 ER PT J AU Penner, K Pope, A Chapin, EL Greve, TR Bertoldi, F Brodwin, M Chary, RR Conselice, CJ Coppin, K Giavalisco, M Hughes, DH Ivison, RJ Perera, T Scott, D Scott, K Wilson, G AF Penner, Kyle Pope, Alexandra Chapin, Edward L. Greve, Thomas R. Bertoldi, Frank Brodwin, Mark Chary, Ranga-Ram Conselice, Christopher J. Coppin, Kristen Giavalisco, Mauro Hughes, David H. Ivison, Rob J. Perera, Thushara Scott, Douglas Scott, Kimberly Wilson, Grant TI Origins of the extragalactic background at 1 mm from a combined analysis of the AzTEC and MAMBO data in GOODS-N SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; galaxies: evolution; galaxies: high-redshift; submillimetre: diffuse background ID STAR-FORMATION HISTORY; SCUBA SUPER-MAP; SUBMILLIMETER GALAXIES; FIELD; UNIVERSE; SPITZER; LIGHT; BLAST; HALF AB We present a study of the cosmic infrared background, which is a measure of the dust-obscured activity in all galaxies in the Universe. We venture to isolate the galaxies responsible for the background at 1 mm; with spectroscopic and photometric redshifts we constrain the redshift distribution of these galaxies. We create a deep 1.16 mm map (sigma similar to 0.5 mJy) by combining the AzTEC 1.1 mm and MAMBO 1.2 mm data sets in the Great Observatories Origins Deep Survey North (GOODS-N) region. This combined map contains 41 secure detections, 13 of which are new. By averaging the 1.16 mm flux densities of individually undetected galaxies with 24 mu m flux densities > 25 mu Jy, we resolve 31-45 per cent of the 1.16 mm background. Repeating our analysis on the SCUBA 850 mu m map, we resolve a higher percentage (40-64 per cent) of the 850 mu m background. A majority of the background resolved (attributed to individual galaxies) at both wavelengths comes from galaxies at z > 1.3. If the ratio of the resolved submillimetre to millimetre background is applied to a reasonable scenario for the origins of the unresolved submillimetre background, 60-88 per cent of the total 1.16 mm background comes from galaxies at z > 1.3. C1 [Penner, Kyle] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Pope, Alexandra] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Chapin, Edward L.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Greve, Thomas R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Greve, Thomas R.] Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Bertoldi, Frank] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chary, Ranga-Ram] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Coppin, Kristen] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Giavalisco, Mauro; Wilson, Grant] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Hughes, David H.] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico. [Ivison, Rob J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, Rob J.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Perera, Thushara] Illinois Wesleyan Univ, Dept Phys, Bloomington, IL 61701 USA. [Scott, Kimberly] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Penner, K (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM kpenner@as.arizona.edu RI Conselice, Christopher/B-4348-2013; Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Scott, Douglas/0000-0002-6878-9840; Conselice, Christopher/0000-0003-1949-7638; /0000-0002-0729-2988 FU NASA; DNRF; IDA; W. M. Keck Foundation; UK Science and Technology Facilities Council (STFC) FX We thank the referee for their helpful comments. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. AP acknowledges support provided by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Dark Cosmology Centre is funded by the DNRF. TRG acknowledges support from IDA. Support for MB was provided by the W. M. Keck Foundation. KC acknowledges the UK Science and Technology Facilities Council (STFC) for a fellowship. NR 25 TC 20 Z9 20 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 410 IS 4 BP 2749 EP 2759 DI 10.1111/j.1365-2966.2010.17650.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706IG UT WOS:000286211000057 ER PT J AU Schmidt, T Calabrese, JM Grodzycki, M Paulick, M Pearce, MC Rau, F von Borell, E AF Schmidt, Tatjana Calabrese, Justin M. Grodzycki, Mario Paulick, Marleen Pearce, Michael C. Rau, Franziska von Borell, Eberhard TI Impact of single-sex and mixed-sex group housing of boars vaccinated against GnRF or physically castrated on body lesions, feeding behaviour and weight gain SO APPLIED ANIMAL BEHAVIOUR SCIENCE LA English DT Article DE GnRF vaccination; Castration; Feeding behaviour; Aggression; Mixed-sex housing; Welfare ID SURGICAL-CASTRATION; FINISHING PIGS; GROWTH-PERFORMANCE; ANIMAL-WELFARE; TAINT; SOWS AB Physical castration of male piglets is common practice in many countries for the control of boar taint. A vaccine against GnRF (Improvac (R)) is licensed in Europe as an alternative to this painful procedure. Vaccinated pigs are known to behave like entire males up to the second vaccination, exhibiting more aggressive behaviour towards each other, which is of welfare concern. Previous studies showed that feeding behaviour is influenced by the level of competition and therefore possibly also by agonistic interactions in pig groups. The aim of this study was to evaluate if mixed-sex or single-sex housing as well as the castration method would influence skin lesions, feeding behaviour and weight gain. A total of 160 pigs were raised in four treatment groups (in four replicates): (1) single-sex physical castrates (C, n = 10 per pen), (2) single-sex vaccinates (V, n = 10), (3) physical castrates (CF, n = 5) housed with females (FC, n = 5), and (4) vaccinates (VF, n = 5) housed with females (FV, n = 5). The fattening time started at 11 wks and vaccinations were applied at 12 and 23 wks of age. Data were analyzed as repeated mixed models with Tukey HSD tests. A shorter feeding duration (FDV, P<0.001) and lower feed intake (Fly, P=0.009) per visit of V compared to C pigs, before the second vaccination (wk 20 of age), could be a consequence of more aggressive interactions at the feeder. This is confirmed by higher shoulder lesion scores in V pigs before effective castration (period 3, P=0.036). This disadvantage is not apparent in VF groups, in which shoulder lesions were not higher and FIV/FDV were not lower compared to C and CF pigs. Feeding duration (FDD) and intake (FID) per day were lower for V (P<0.001/P<0.001), as well as for VF pigs (P=0.005/P=0.013) in wk 20 compared to C pigs. However, ADG did not differ between treatments before the second vaccination. Considerable changes occurred after the second vaccination, with a higher FID for V (P<0.001) and a higher ADG for V (P<0.001) and VF pigs (P<0.001) than for C pigs; the other feeding parameters and lesion scores did not differ between treatments anymore. Although lesions were mostly superficial scratches and not severe wounds, it seems likely that agonistic interactions impair welfare. Our results suggest that for welfare improvement the second vaccination should be applied earlier in the fattening phase and GnRF-vaccinated males should be raised together with females to reduce agonistic interactions. (C) 2010 Elsevier B.V. All rights reserved. C1 [Schmidt, Tatjana] Univ Halle Wittenberg, Inst Agr & Nutr Nutr Sci Anim Husb & Ecol, D-06120 Halle, Saale, Germany. [Calabrese, Justin M.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Calabrese, Justin M.] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04318 Leipzig, Germany. [Grodzycki, Mario] Pfizer Anim Hlth, D-10785 Berlin, Germany. [Pearce, Michael C.] Pfizer Anim Hlth, Vet Med Res & Dev, Sandwich CT13 9NJ, Kent, England. RP Schmidt, T (reprint author), Univ Halle Wittenberg, Inst Agr & Nutr Nutr Sci Anim Husb & Ecol, Theodor Lieser Str 11, D-06120 Halle, Saale, Germany. EM tatjana.schmidt@landw.uni-halle; eberhard.vonborell@landw.uni-halle.de RI Calabrese, Justin/B-9131-2012 FU Pfizer FX We thank Pfizer for providing financial support and Dr. Steve Wilson and Jim Allison for helpful comments on the manuscript. We also thank Heidrun Nitzer, Manuela Zuhl and the staff of the State Institute for Agriculture in Saxony Anhalt, especially Dr. Manfred Weber for excellent collaboration and animal management as well as Dr. Herwig Maurer and Gerald Wischer for help with the database management. NR 29 TC 10 Z9 10 U1 3 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1591 J9 APPL ANIM BEHAV SCI JI Appl. Anim. Behav. Sci. PD FEB PY 2011 VL 130 IS 1-2 BP 42 EP 52 DI 10.1016/j.applanim.2010.11.019 PG 11 WC Agriculture, Dairy & Animal Science; Behavioral Sciences; Veterinary Sciences SC Agriculture; Behavioral Sciences; Veterinary Sciences GA 724ZN UT WOS:000287615100005 ER PT J AU Barmby, P Marengo, M Evans, NR Bono, G Huelsman, D Su, KYL Welch, DL Fazio, GG AF Barmby, P. Marengo, M. Evans, N. R. Bono, G. Huelsman, D. Su, K. Y. L. Welch, D. L. Fazio, G. G. TI GALACTIC CEPHEIDS WITH SPITZER. II. SEARCH FOR EXTENDED INFRARED EMISSION SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; stars: mass-loss; stars: variables: Cepheids ID LARGE-MAGELLANIC-CLOUD; PERIOD-LUMINOSITY RELATIONS; BAADE-WESSELINK DISTANCES; PHASE-DEPENDENT VARIATION; HUBBLE-SPACE-TELESCOPE; TESTING MASS-LOSS; RS-PUPPIS; CLASSICAL CEPHEIDS; FUNDAMENTAL PARAMETERS; DELTA CEPHEI AB A deep and detailed examination of 29 classical Cepheids with the Spitzer Space Telescope has revealed three stars with strong nearby extended emission detected in multiple bands which appears to be physically associated with the stars. RS Pup was already known to possess extended infrared emission, while the extended emission around the other two stars (S Mus and delta Cep) is newly discovered in our observations. Four other stars (GH Lup, l Car, T Mon, and X Cyg) show tentative evidence for extended infrared emission. An unusual elongated extended object next to SZ Tau appears to be a background or foreground object in a chance alignment with the Cepheid. The inferred mass-loss rate upper limits for S Mus and d Cep are in the range from 10(-9) to 10(-8) M-circle dot yr(-1), with the upper limit for RS Pup as high as 10(-6) M-circle dot yr(-1). Mass loss during post-main-sequence evolution has been proposed as a resolution to the discrepancy between pulsational and dynamical masses of Cepheid variable stars: dust in the lost material would make itself known by the presence of an infrared bright nebula or unresolved infrared excess. The observed frequency of infrared circumstellar emission (< 24%) and the mass-loss rate we estimate for our sources show that dusty mass loss can only account for part of the Cepheid mass-loss discrepancy. Nevertheless, our direct evidence that mass loss is active during the Cepheid phase is an important confirmation that these processes need to be included in evolutionary and pulsation models of these stars and should be taken into account in the calibration of the Cepheid distance scale. C1 [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Barmby, P.; Marengo, M.; Evans, N. R.; Huelsman, D.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Bono, G.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Bono, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Huelsman, D.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. RP Barmby, P (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Su, Kate/0000-0002-3532-5580 FU NASA [1407]; Natural Sciences and Engineering Research Council of Canada; Ontario Early Researcher Award; Chandra X-Ray Center [NAS8-03060]; National Science Foundation REU; Department of Defense [0754568]; Smithsonian Institution FX The authors thank H. Neilson for useful conversations and L. D. Matthews for assistance with computing the projected space velocity of l Car. We thank the referee for helpful comments. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through an award issued by JPL/Caltech. P. B. and D. L. W. acknowledge research support through Discovery Grants from the Natural Sciences and Engineering Research Council of Canada; P. B. also acknowledges support from an Ontario Early Researcher Award. N.R.E. acknowledges support from the Chandra X-Ray Center Grant NAS8-03060. D. H. was supported in part by the National Science Foundation REU and Department of Defense ASSURE programs under grant no. 0754568 and by the Smithsonian Institution. NR 70 TC 22 Z9 22 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2011 VL 141 IS 2 AR 42 DI 10.1088/0004-6256/141/2/42 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706AW UT WOS:000286186100014 ER PT J AU Matthews, LD Libert, Y Gerard, E Le Bertre, T Johnson, MC Dame, TM AF Matthews, L. D. Libert, Y. Gerard, E. Le Bertre, T. Johnson, M. C. Dame, T. M. TI HI OBSERVATIONS OF THE ASYMPTOTIC GIANT BRANCH STAR X HERCULIS: DISCOVERY OF AN EXTENDED CIRCUMSTELLAR WAKE SUPERPOSED ON A COMPACT HIGH-VELOCITY CLOUD SO ASTRONOMICAL JOURNAL LA English DT Article DE radio lines: stars; stars: AGB and post-AGB; stars: individual (X Her); stars: winds, outflows ID MASS-LOSS RATES; INTERSTELLAR-MEDIUM; PLANETARY-NEBULAE; SEMIREGULAR VARIABLES; ATOMIC-HYDROGEN; GALACTIC-CENTER; EVOLVED STARS; LOSS HISTORY; MILKY-WAY; CO AB We report Hi 21 cm line observations of the asymptotic giant branch (AGB) star X Her obtained with the Robert C. Byrd Green Bank Telescope (GBT) and the Very Large Array. We have unambiguously detected Hi emission associated with the circumstellar envelope of the star, with a mass totaling M-HI approximate to 2.1 x 10(-3) M-circle dot. The Hi distribution exhibits a head-tail morphology, similar to those previously observed around the AGB stars Mira and RS Cnc. The tail is elongated along the direction of the star's space motion, with a total extent of >= 6'.0 (0.24 pc) in the plane of the sky. We also detect a systematic radial velocity gradient of similar to 6.5 kms(-1) across the Hi envelope. These results are consistent with the Hi emission tracing a turbulent wake that arises from the motion of a mass-losing star through the interstellar medium (ISM). GBT mapping of a 2 degrees x 2 degrees region around X Her reveals that the star lies (in projection) near the periphery of a much larger Hi cloud that also exhibits signatures of interaction with the ISM. The properties of the cloud are consistent with those of compact high-velocity clouds. Using (CO)-C-12 J = 1-0 observations, we have placed an upper limit on its molecular gas content of N-H2 < 1.3 x 10(20) cm(-2). Although the distance to the cloud is poorly constrained, the probability of a chance coincidence in position, velocity, and apparent position angle of space motion between X Her and the cloud is extremely small, suggesting a possible physical association. However, the large Hi mass of the cloud (>= 2.4M(circle dot)) and the blueshift of its mean velocity relative to X Her are inconsistent with an origin tied directly to ejection from the star. C1 [Matthews, L. D.; Johnson, M. C.] MIT, Haystack Observ, Westford, MA 01886 USA. [Libert, Y.] IRAM, F-38406 St Martin Dheres, France. [Gerard, E.] Observ Paris, GEPI, UMR 8111, F-92195 Meudon, France. [Le Bertre, T.] Observ Paris, LERMA, UMR 8112, F-75014 Paris, France. [Johnson, M. C.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matthews, LD (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. FU National Science Foundation; National Aeronautics and Space Administration FX We thank J. Lockman for valuable guidance on the GBT observing setup and data processing, as well as the entire Green Bank staff for their hospitality and assistance with the GBT observations. We also thank M. Reid and E. Greisen for useful discussions and the anonymous referee for suggestions that helped to improve the manuscript. M.C.J. was supported through a National Science Foundation Research Experience for Undergraduates Grant to MIT Haystack Observatory. The observations presented here were part of NRAO programs AM887 and GM75. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 81 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2011 VL 141 IS 2 AR 60 DI 10.1088/0004-6256/141/2/60 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706AW UT WOS:000286186100032 ER PT J AU Walkowicz, LM Basri, G Batalha, N Gilliland, RL Jenkins, J Borucki, WJ Koch, D Caldwell, D Dupree, AK Latham, DW Meibom, S Howell, S Brown, TM Bryson, S AF Walkowicz, Lucianne M. Basri, Gibor Batalha, Natalie Gilliland, Ronald L. Jenkins, Jon Borucki, William J. Koch, David Caldwell, Doug Dupree, Andrea K. Latham, David W. Meibom, Soeren Howell, Steve Brown, Timothy M. Bryson, Steve TI WHITE-LIGHT FLARES ON COOL STARS IN THE KEPLER QUARTER 1 DATA SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: emission-line, Be; stars: flare; stars: low-mass ID M-DWARFS; AD LEONIS; PHOTOMETRIC VARIABILITY; STELLAR FLARE; SOLAR-FLARES; YZ-CMI; X-RAY; SUN; 1ST; PERFORMANCE AB We present the results of a search for white-light flares on similar to 23,000 cool dwarfs in the Kepler Quarter 1 long cadence data. We have identified 373 flaring stars, some of which flare multiple times during the observation period. We calculate relative flare energies, flare rates, and durations and compare these with the quiescent photometric variability of our sample. We find that M dwarfs tend to flare more frequently but for shorter durations than K dwarfs and that they emit more energy relative to their quiescent luminosity in a given flare than K dwarfs. Stars that are more photometrically variable in quiescence tend to emit relatively more energy during flares, but variability is only weakly correlated with flare frequency. We estimate distances for our sample of flare stars and find that the flaring fraction agrees well with other observations of flare statistics for stars within 300 pc above the Galactic plane. These observations provide a more rounded view of stellar flares by sampling stars that have not been pre-selected by their activity, and are informative for understanding the influence of these flares on planetary habitability. C1 [Walkowicz, Lucianne M.; Basri, Gibor] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Batalha, Natalie; Jenkins, Jon; Borucki, William J.; Koch, David; Caldwell, Doug; Bryson, Steve] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dupree, Andrea K.; Latham, David W.; Meibom, Soeren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howell, Steve] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. RP Walkowicz, LM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU Kepler Fellowship for the Study of Planet-Bearing Stars; NASA's Science Mission Directorate FX L.M.W. is grateful for the support of the Kepler Fellowship for the Study of Planet-Bearing Stars. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. NR 35 TC 73 Z9 73 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 FEB PY 2011 VL 141 IS 2 AR 50 DI 10.1088/0004-6256/141/2/50 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706AW UT WOS:000286186100022 ER PT J AU Winn, JN Howard, AW Johnson, JA Marcy, GW Isaacson, H Shporer, A Bakos, GA Hartman, JD Holman, MJ Albrecht, S Crepp, JR Morton, TD AF Winn, Joshua N. Howard, Andrew W. Johnson, John Asher Marcy, Geoffrey W. Isaacson, Howard Shporer, Avi Bakos, Gaspar A. Hartman, Joel D. Holman, Matthew J. Albrecht, Simon Crepp, Justin R. Morton, Timothy D. TI ORBITAL ORIENTATIONS OF EXOPLANETS: HAT-P-4b IS PROGRADE AND HAT-P-14b IS RETROGRADE SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: formation; planet-star interactions; stars: rotation ID SPIN-ORBIT; PLANETARY SYSTEMS; ALIGNMENT; STAR; MISALIGNMENT; TRANSITS; CURVES; MODELS; MASS AB We present observations of the Rossiter-McLaughlin effect for two exoplanetary systems, revealing the orientations of their orbits relative to the rotation axes of their parent stars. HAT-P-4b is prograde, with a sky-projected spin-orbit angle of lambda = -4.9 +/- 11.9 deg. In contrast, HAT-P-14b is retrograde, with lambda = 189.1 +/- 5.1 deg. These results conform with a previously noted pattern among the stellar hosts of close-in giant planets: hotter stars have a wide range of obliquities and cooler stars have low obliquities. This, in turn, suggests that three-body dynamics and tidal dissipation are responsible for the short-period orbits of many exoplanets. In addition, our data revealed a third body in the HAT-P-4 system, which could be a second planet or a companion star. C1 [Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Howard, Andrew W.; Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Johnson, John Asher; Crepp, Justin R.; Morton, Timothy D.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Johnson, John Asher; Crepp, Justin R.; Morton, Timothy D.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bakos, Gaspar A.; Hartman, Joel D.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Hartman, Joel/0000-0001-8732-6166 FU NASA [NNX09AD36G, NNX09AB33G]; MIT; NWO FX We thank Teruyuki Hirano for interesting discussions related to this work, Amaury Triaud and the anonymous referee for insightful comments on the manuscript, and John Southworth for making available his useful code JKTLD for calculating theoretical limb-darkening coefficients. We gratefully acknowledge support from the NASA Origins program through awards NNX09AD36G and NNX09AB33G, and the MIT Class of 1942. S.A. acknowledges support from an NWO Rubicon fellowship. NR 43 TC 46 Z9 46 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2011 VL 141 IS 2 AR 63 DI 10.1088/0004-6256/141/2/63 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706AW UT WOS:000286186100035 ER PT J AU Amo-Baladron, MA Martin-Pintado, J Martin, S AF Amo-Baladron, M. A. Martin-Pintado, J. Martin, S. TI Mapping photodissociation and shocks in the vicinity of Sagittarius A* SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; ISM: clouds; ISM: molecules; Galaxy: abundances; Galaxy: nucleus; Galaxy: center ID GALACTIC-CENTER REGION; SPECTRAL-LINE SURVEY; APERTURE SYNTHESIS OBSERVATIONS; PHOTON-DOMINATED REGIONS; CENTER MOLECULAR CLOUDS; YOUNG STELLAR OBJECTS; CENTRAL 2 PARSECS; NEUTRAL-GAS DISK; CIRCUMNUCLEAR DISK; SGR-A AB Aims. We study the chemistry in the harsh environments of galactic nuclei using the nearest one, the Galactic center (GC). Methods. We have obtained maps of the molecular emission within the central five arcminutes (12 pc) of the GC in selected molecular tracers: SiO(2-1), HNCO(5(0,5)-4(0,4)), and the J = 1 -> 0 transition of (HCO+)-C-13, (HNC)-C-13, and (CO)-O-18 at an angular resolution of 30 '' (1.2 pc). The mapped region includes the circumnuclear disk (CND) and the two surrounding giant molecular clouds (GMCs) of the Sgr A complex, known as the 20 and 50 km s(-1) molecular clouds. Additionally, we simultaneously observed the J = 2 -> 1 and J = 3 -> 2 transitions of SiO toward selected positions to estimate the physical conditions of the molecular gas using the large velocity gradient approximation. Results. The SiO(2-1) emission shows all the molecular features identified in previous studies, covering the same velocity range as the (HCO+)-C-13(1-0) emission, which also presents a similar distribution. In contrast, HNCO(5-4) emission appears in a narrow velocity range mostly concentrated in the 20 and 50 km s(-1) GMCs. A similar trend follows the (HNC)-C-13(1-0) emission. The HNCO column densities and fractional abundances present the highest contrast, with difference factors of >= 60 and 28, respectively. Their highest values are found toward the cores of the GMCs, whereas the lowest ones are measured at the CND. SiO abundances do not follow this trend, with high values found toward the CND, as well as the GMCs. By comparing our abundances with those of prototypical Galactic sources we conclude that HNCO, similar to SiO, is ejected from grain mantles into gas-phase by nondissociative C-shocks. This results in the high abundances measured toward the CND and the GMCs. However, the strong UV radiation from the Central cluster utterly photodissociates HNCO as we get closer to the center, whereas SiO seems to be more resistant against UV-photons or it is produced more efficiently by the strong shocks in the CND. This UV field could be also responsible for the trend found in the (HNC)-C-13 abundance. Conclusions. We discuss the possible connections between the molecular gas at the CND and the GMCs using the HNCO/SiO, SiO/CS, and HNCO/CS intensity ratios as probes of distance to the Central cluster. In particular, the HNCO/SiO intensity ratio is proved to be an excellent tool for evaluating the distance to the center of the different gas components. C1 [Amo-Baladron, M. A.; Martin-Pintado, J.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Martin, S.] European So Observ, Santiago 19, Chile. [Martin, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Amo-Baladron, MA (reprint author), CSIC INTA, Ctr Astrobiol, Ctra Torrejon Ajalvir Km 4, Madrid 28850, Spain. EM arancha@damir.iem.csic.es RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU Spanish Ministerio de Ciencia e Innovacion [ESP2007-65812-C02-01] FX The authors would like to thank Prof. M. Tsuboi and D. M. Montero-Castano for kindly providing their CS(1-0) and HCN(4-3) data, respectively. We also thank the referee for the suggestions. This work was supported by the Spanish Ministerio de Ciencia e Innovacion under project ESP2007-65812-C02-01. NR 126 TC 19 Z9 19 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A54 DI 10.1051/0004-6361/200913545 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400066 ER PT J AU Barnard, R Garcia, M Murray, S Nooraee, N Pietsch, W AF Barnard, R. Garcia, M. Murray, S. Nooraee, N. Pietsch, W. TI Observations of the recurrent M31 transient XMMU J004215.8+411924 with Swift, Chandra, HST, and Einstein SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: general; X-rays: binaries; galaxies: individual: M31 ID X-RAY SOURCES; SMALL-MAGELLANIC-CLOUD; GLOBULAR-CLUSTERS; UPDATED SURVEY; NEUTRON-STAR; M-31; CANDIDATE; BINARIES; PHOTOMETRY; ACCRETION AB Context. The transient X-ray source XMMU J004215.8+411924 within M31 was found to be in outburst again in the 2010 May 27 Chandra observation. We present results from our four Chandra and seven Swift observations that covered this outburst. Aims. X-ray transient behaviour is generally caused by one of two things: mass accretion from a high mass companion during some restricted phase range in the orbital cycle, or disc instability in a low mass system. We aim to exploit Einstein, HST, Chandra and Swift observations to determine the nature of XMMU J004215.8+411924. Methods. We model the 2010 May spectrum, and use the results to convert from intensity to counts in the fainter Chandra observations, as well as the Swift observations; these data are used to create a lightcurve. We also estimate the flux in the 1979 January 13 Einstein observation. Additionally, we search for an optical counterpart in HST data. Results. Our best X-ray positions from the 2006 and 2010 outbursts are 0.3 '' apart, and 1.6 '' from the Einstein source; these outbursts are likely to come from the same star system. We see no evidence for an optical counterpart with m(B) less than or similar to 25.5; this new limit is 3.5 mag fainter than the existing one. Furthermore, we see no V band counterpart with m(V) less than or similar to 26. The local absorption is similar to 7 times higher than the Galactic line-of-sight, and provides similar to 2 mag of extinction in the V band. Hence M-V greater than or similar to -0.5. Fits to the X-ray emission spectrum suggest a black hole primary. Conclusions. We find that XMMU J004215.8+411924 is most likely to be a transient LMXB, rather than a HMXB as originaly proposed. The nature of the primary is unclear, although we argue that a black hole is likely. C1 [Barnard, R.; Garcia, M.; Murray, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nooraee, N.] Dublin Inst Adv Studies, Dublin 4, Ireland. [Pietsch, W.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rbarnard@head.cfa.harvard.edu FU Chandra grant [GO9-0100X]; HST [GO-11013]; NASA [NAS-03060] FX We thank the anonymous referee for their thoughtful comments. We thank the Swift team for carrying out the Target of Opportunity observations. R. B. is funded by Chandra grant GO9-0100X and HST grant GO-11013. MRG is partially supported by NASA grant NAS-03060. This work has made use of the data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center, and the Hubble Legacy Archive. NR 27 TC 2 Z9 2 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A50 DI 10.1051/0004-6361/201015467 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400062 ER PT J AU Blondin, S Mandel, KS Kirshner, RP AF Blondin, S. Mandel, K. S. Kirshner, R. P. TI Do spectra improve distance measurements of Type Ia supernovae? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE supernovae: general; cosmology: observations ID HUBBLE-SPACE-TELESCOPE; LIGHT-CURVE SHAPES; DARK ENERGY; LUMINOSITY INDICATORS; CONSTRAINTS; DIVERSITY; SPECTROSCOPY; DISCOVERIES; MAGNITUDES; PHOTOMETRY AB We investigate the use of a wide variety of spectroscopic measurements to determine distances to low-redshift Type Ia supernovae (SN Ia) in the Hubble flow observed through the CfA Supernova Program. We consider linear models for predicting distances to SN Ia using light-curve width and color parameters (determined using the SALT2 light-curve fitter) and a spectroscopic indicator, and evaluate the resulting Hubble diagram scatter using a cross-validation procedure. We confirm the ability of spectral flux ratios alone at maximum light to reduce the scatter of Hubble residuals by similar to 10% [weighted rms, or WRMS = 0.189 +/- 0.026 mag for the flux ratio R(6630/4400)] with respect to the standard combination of light-curve width and color, for which WRMS = 0.204 +/- 0.029 mag. When used in combination with the SALT2 color parameter, the color-corrected flux ratio R-c(6420/5290) at maximum light leads to an even lower scatter (WRMS = 0.175 +/- 0.025 mag), although the improvement has low statistical significance (<2 sigma) given the size of our sample (26 SN Ia). We highlight the importance of an accurate relative flux calibration and the failure of this method for highly-reddened objects. Comparison with synthetic spectra from 2D delayed-detonation explosion models shows that the correlation of R(6630/4400) with SN Ia absolute magnitudes can be largely attributed to intrinsic color variations and not to reddening by dust in the host galaxy. We consider flux ratios at other ages, as well as the use of pairs of flux ratios, revealing the presence of small-scale intrinsic spectroscopic variations in the iron-group-dominated absorption features around similar to 4300 angstrom and similar to 4800 angstrom. The best flux ratio overall is the color-corrected R-c(4610/4260) at t = -2.5 d from maximum light, which leads to similar to 30% lower scatter (WRMS = 0.143 +/- 0.020 mag) with respect to the standard combination of light-curve width and color, at similar to 2 sigma significance. We examine other spectroscopic indicators related to line-profile morphology (absorption velocity, pseudo-equivalent width etc.), but none appear to lead to a significant improvement over the standard light-curve width and color parameters. We discuss the use of spectra in measuring more precise distances to SN Ia and the implications for future surveys which seek to determine the properties of dark energy. C1 [Blondin, S.] CNRS IN2P3, CPPM, F-13288 Marseille 9, France. [Mandel, K. S.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. RP Blondin, S (reprint author), CNRS IN2P3, CPPM, 163 Ave Luminy, F-13288 Marseille 9, France. EM blondin@cppm.in2p3.fr FU NSF [AST 09-07903] FX We acknowledge many useful conversations with members of the RENOIR group at the CPPM, in particular Florent Marmol and Andre Tilquin. We thank Stephen Bailey for his patience in explaining the details of his flux ratio measurements and validation procedure. Alex Conley shared a non-public custom version of his simple_cosfitter code and provided invaluable help with cosmology fits. We further thank Julien Guy and Gautham Narayan for advice on using the SALT2 light-curve fitter, and Dan Kasen for sending us the output of his 2D radiative transfer calculations. Support for supernova research at Harvard University, including the CfA Supernova Archive, is provided in part by NSF grant AST 09-07903. NR 49 TC 38 Z9 38 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A81 DI 10.1051/0004-6361/201015792 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400093 ER PT J AU Comastri, A Ranalli, P Iwasawa, K Vignali, C Gilli, R Georgantopoulos, I Barcons, X Brandt, WN Brunner, H Brusa, M Cappelluti, N Carrera, FJ Civano, F Fiore, F Hasinger, G Mainieri, V Merloni, A Nicastro, F Paolillo, M Puccetti, S Rosati, P Silverman, JD Tozzi, P Zamorani, G Balestra, I Bauer, FE Luo, B Xue, YQ AF Comastri, A. Ranalli, P. Iwasawa, K. Vignali, C. Gilli, R. Georgantopoulos, I. Barcons, X. Brandt, W. N. Brunner, H. Brusa, M. Cappelluti, N. Carrera, F. J. Civano, F. Fiore, F. Hasinger, G. Mainieri, V. Merloni, A. Nicastro, F. Paolillo, M. Puccetti, S. Rosati, P. Silverman, J. D. Tozzi, P. Zamorani, G. Balestra, I. Bauer, F. E. Luo, B. Xue, Y. Q. TI The XMM Deep survey in the CDF-S I. First results on heavily obscured AGN SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: high-redshift; X-rays: galaxies; X-rays: diffuse background ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; COMPTON-THICK QUASARS; HARD X-RAY; FIELD-SOUTH; OPTICAL SPECTROSCOPY; SOURCE CATALOGS; CHANDRA; GALAXIES; UNIVERSE AB We present the first results of the spectroscopy of distant, obscured AGN as obtained with the ultra-deep (approximate to 3.3 Ms) XMM-Newton survey in the Chandra deep field South. One of the primary goals of the project is to characterize the X-ray spectral properties of obscured and heavily obscured Compton-thick AGN over the range of redhifts and luminosities that are relevant in terms of their contribution to the X-ray background. The ultra-deep exposure, coupled with the XMM detector's spectral throughput, allowed us to accumulate good quality X-ray spectra for a large number of X-ray sources and, in particular, for heavily obscured AGN at cosmological redshifts. Specifically we present the X-ray spectral properties of two high-redshift - z = 1.53 and z = 3.70 - sources. The XMM spectra of both are very hard, with a strong iron K alpha line at a rest-frame energy of similar to 6.4 keV. A reflection-dominated continuum provides the best description of the X-ray spectrum of the z = 1.53 source, while the intrinsic continuum of the z = 3.70 AGN is obscured by a large column N-H approximate to 10(24) cm(-2) of cold gas. Compton-thick absorption, or close to it, is unambiguously detected in both sources. Interestingly, these sources would not be selected as candidate Compton thick AGN by some multiwavelength selection criteria based on the mid-infrared to optical and X-ray to optical flux ratios. C1 [Comastri, A.; Ranalli, P.; Iwasawa, K.; Vignali, C.; Gilli, R.; Georgantopoulos, I.; Cappelluti, N.; Zamorani, G.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Ranalli, P.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Iwasawa, K.] Univ Barcelona IEEC UB, ICREA, Barcelona 08028, Spain. [Iwasawa, K.] Univ Barcelona IEEC UB, Inst Ciencies Cosmos, Barcelona 08028, Spain. [Barcons, X.; Carrera, F. J.] CSIC UC, Inst Fis Cantabria, Santander 39005, Spain. [Brandt, W. N.; Luo, B.; Xue, Y. Q.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brunner, H.; Brusa, M.; Merloni, A.; Balestra, I.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Brusa, M.; Cappelluti, N.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Civano, F.; Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fiore, F.; Nicastro, F.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Hasinger, G.; Rosati, P.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Paolillo, M.] Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. Univ Tokyo, IPMU, Chiba 2778568, Japan. [Tozzi, P.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 22, Chile. RP Comastri, A (reprint author), INAF, Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM andrea.comastri@oabo.inaf.it RI Paolillo, Maurizio/J-1733-2012; Barcons, Xavier/L-3335-2014; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; Vignali, Cristian/J-4974-2012; Ranalli, Piero/K-6363-2013; Georgantopoulos, Ioannis/L-3687-2013 OI Cappelluti, Nico/0000-0002-1697-186X; Puccetti, Simonetta/0000-0002-2734-7835; Zamorani, Giovanni/0000-0002-2318-301X; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157; Paolillo, Maurizio/0000-0003-4210-7693; Barcons, Xavier/0000-0003-1081-8861; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Nicastro, Fabrizio/0000-0002-6896-1364; Balestra, Italo/0000-0001-9660-894X; Vignali, Cristian/0000-0002-8853-9611; Ranalli, Piero/0000-0003-3956-755X; FU ESA Member States; USA (NASA); Italian Space Agency (ASI) [ASI-INAF I/088/06/0, I/009/10/0]; NASA [NNX08AX51G, NNX09AQ05G, NNX10AC99G, SV0-80004]; Spanish Ministerio de Ciencia e Innovacion [AYA2009-08059]; Deutsches Zentrum fur Luft- und Raumfahrt, DLR [50 OR 0207, 50 OR 0405]; Blanceflor Boncompagni Ludovisi Foundation; World Premier International (WPI) Research Center Initiative, MEXT, Japan; CONICYT, Chile [1101024, 15010003]; Marie Curie fellowship [FP7-PEOPLE-IEF-2008 Prop. 235285] FX This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).; The authors would like to warmly thank Maria Diaz Trigo and Ignacio della Calle for their valuable help and advice in the scheduling of the XMM-CDF-S observations. Support from the Italian Space Agency (ASI) under the contracts ASI-INAF I/088/06/0 and I/009/10/0 is acknowledged. A. C. acknowledges the NASA grant NNX09AQ05G to visit CfA, where part of this work was written. I. G. and A. C. acknowledge the Marie Curie fellowship FP7-PEOPLE-IEF-2008 Prop. 235285. X. B. and F.J.C. acknowledge financial support from the Spanish Ministerio de Ciencia e Innovacion under project AYA2009-08059. M. B. acknowledges support by the Deutsches Zentrum fur Luft- und Raumfahrt, DLR project numbers 50 OR 0207 and 50 OR 0405. F. C., F.N. and M. B. acknowledge NASA grants NNX08AX51G and NNX09AQ05G. F. C. acknowledges support from the Blanceflor Boncompagni Ludovisi Foundation. J.D.S. is supported by World Premier International (WPI) Research Center Initiative, MEXT, Japan. W.N.B. acknowledges NASA grant SV0-80004 and NASA ADP grant NNX10AC99G. F. E. B. cknowledges the support of CONICYT, Chile, under grants FONDECYT 1101024 and FONDAP (CATA) 15010003. NR 37 TC 69 Z9 69 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 FEB PY 2011 VL 526 AR L9 DI 10.1051/0004-6361/201016119 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400010 ER PT J AU Desert, JM Sing, D Vidal-Madjar, A Hebrard, G Ehrenreich, D des Etangs, AL Parmentier, V Ferlet, R Henry, GW AF Desert, J. -M. Sing, D. Vidal-Madjar, A. Hebrard, G. Ehrenreich, D. des Etangs, A. Lecavelier Parmentier, V. Ferlet, R. Henry, G. W. TI Transit spectrophotometry of the exoplanet HD 189733b II. New Spitzer observations at 3.6 mu m SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; starspots; stars: individual: HD 189733b ID HUBBLE-SPACE-TELESCOPE; EXTRASOLAR GIANT PLANETS; TRANSMISSION SPECTRUM; INFRARED-EMISSION; HD-189733 SYSTEM; ROTATION PERIOD; HOT JUPITERS; LIGHT CURVES; WATER-VAPOR; ATMOSPHERE AB Context. We present a new primary transit observation of the hot-jupiter HD 189733b, obtained at 3.6 mu m with the Infrared Array Camera (IRAC) onboard the Spitzer Space Telescope. Previous measurements at 3.6 microns suffered from strong systematics, and conclusions could hardly be obtained with confidence on the water detection by comparison of the 3.6 and 5.8 microns observations. Aims. We aim at constraining the atmospheric structure and composition of the planet and improving previously derived parameters. Methods. We use a high-S/N Spitzer photometric transit light curve to improve the precision of the near infrared radius of the planet at 3.6 mu m. The observation has been performed using high-cadence time series integrated in the subarray mode. We are able to derive accurate system parameters, including planet-to-star radius ratio, impact parameter, scale of the system, and central time of the transit from the fits of the transit light curve. We compare the results with transmission spectroscopic models and with results from previous observations at the same wavelength. Results. We obtained the following system parameters of R-p/R-star = 0.15566-0.00024(-0.00024)(+0.00011) , b = 0.661(-0.0050)(+0.0053), and a/R-star = 8.925(-0.0523)(+0.0490) at 3.6 mu m. These measurements are three times more accurate than previous studies at this wavelength because they benefit from greater observational efficiency and less statistic and systematic errors. Nonetheless, we find that the radius ratio has to be corrected for stellar activity and present a method to do so using ground-based long-duration photometric follow-up in the V-band. The resulting planet-to-star radius ratio corrected for the stellar variability agrees with our previous measurement obtained in the same bandpass. We also discuss that water vapour could not be detected by a comparison of the planetary radius measured at 3.6 and 5.8 mu m, because the radius measured at 3.6 mu m is affected by absorption by other species, possibly Rayleigh scattering by haze. C1 [Desert, J. -M.; Sing, D.; Vidal-Madjar, A.; Hebrard, G.; des Etangs, A. Lecavelier; Parmentier, V.; Ferlet, R.] Univ Paris 06, CNRS, Inst Astrophys Paris, CNRS,UMR7095, F-75014 Paris, France. [Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sing, D.] Univ Exeter, Astrophys Grp, Sch Phys, Exeter EX4 4QL, Devon, England. [Ehrenreich, D.] Univ Grenoble 1, Astrophys Lab, Observ Grenoble, CNRS,UMR 5571, F-38041 Grenoble 9, France. [Henry, G. W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. RP Desert, JM (reprint author), Univ Paris 06, CNRS, Inst Astrophys Paris, CNRS,UMR7095, 98bis Blvd Arago, F-75014 Paris, France. EM jdesert@cfa.harvard.edu FU NASA; Centre National d'Etudes Spatiales (CNES); French Agence Nationale pour la Recherche [NT05-4_44463] FX D.K.S. is supported by CNES. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. D. E. is supported by the Centre National d'Etudes Spatiales (CNES). D. E. acknowledges financial support from the French Agence Nationale pour la Recherche through ANR project NT05-4_44463. We thank our anonymous referee for his comments that strengthen the presentation of our results. NR 63 TC 55 Z9 55 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A12 DI 10.1051/0004-6361/200913093 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400024 ER PT J AU Gunther, HM Wawrzyn, AC AF Guenther, H. M. Wawrzyn, A. C. TI A method to simulate inhomogeneously irradiated objects with a superposition of 1D models SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiative transfer; binaries: close; binaries: eclipsing; stars: atmospheres ID CLOSE BINARY-SYSTEMS; STELLAR ATMOSPHERES; NUMERICAL-SOLUTION; SECONDARY STAR; UU SAGITTAE; CONVECTION; VARIABLES; PROFILES; ALBEDO AB Context. In close binary systems the atmosphere of one or both components can be significantly influenced by irradiation from the companion. Often the irradiated atmosphere is simulated with a single-temperature approximation for the entire half-sphere. Aims. We present a scheme to take the varying irradiation angle into account by combining several separate 1D models. This is independent of the actual code which provides the separate stellar spectra. Methods. We calculate the projected area of zones with given irradiation angle and use this geometrical factor to scale separate 1D models. As an example we calculate two different irradiation scenarios with the PHOENIX code. Results. The scheme to calculate the projected area is applicable independent of the physical mechanism that forms these zones. In the case of irradiation by a primary with T = 125 000 K, the secondary forms ions at different ionisation states for different irradiation angles. No single irradiation angle exists which provides an accurate description of the spectrum. We show a similar simulation for weaker irradiation, where the profile of the Ha line depends on the irradiation angle. C1 [Guenther, H. M.; Wawrzyn, A. C.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gunther, HM (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM moritz.guenther@hs.uni-hamburg.de OI Gunther, Hans Moritz/0000-0003-4243-2840 FU DLR [50OR0105]; DFG (Deutsche Forschungsgemeinschaft) [HA 3457/7-1]; State of Hamburg FX The authors thank T. Barman for his support in setting up calculations of irradiated atmospheres with PHOENIX. H.M.G. acknowledges support from DLR for project number 50OR0105. A.C.W. was supported by the DFG (Deutsche Forschungsgemeinschaft), project number HA 3457/7-1. Calculations were performed at the Hamburger Sternwarte Delta Opteron Cluster ("Nathan") financially supported by the DFG and the State of Hamburg. NR 35 TC 2 Z9 2 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A117 DI 10.1051/0004-6361/201014824 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400129 ER PT J AU Kariyappa, R DeLuca, EE Saar, SH Golub, L Dame, L Pevtsov, AA Varghese, BA AF Kariyappa, R. DeLuca, E. E. Saar, S. H. Golub, L. Dame, L. Pevtsov, A. A. Varghese, B. A. TI Temperature variability in X-ray bright points observed with Hinode/XRT SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: X-rays, gamma rays; Sun: magnetic topology ID HYDROGEN LYMAN LINES; INTENSITY OSCILLATIONS; CHROMOSPHERIC FEATURES; RECONNECTION; TELESCOPE; ROTATION; ELEMENTS; REGION; ENERGY; CORONA AB Aims. We investigate the variability in temperature as a function of time among a sample of coronal X-ray bright points (XBPs). Methods. We analysed a 7-h (17:00-24:00 UT) long time sequence of soft X-ray images observed almost simultaneously in two filters (Ti_poly and Al_mesh) on April 14, 2007 with X-ray telescope (XRT) onboard the Hinode mission. We identified and selected 14 XBPs for a detailed analysis. The light curves of XBPs were derived using the SolarSoft library in IDL. The temperature of XBPs was determined using the calibrated temperature response curves of the two filters by means of the intensity ratio method. Results. We find that the XBPs show a high variability in their temperature and that the average temperature ranges from 1.1 MK to 3.4 MK. The variations in temperature are often correlated with changes in average X-ray emission. It is evident from the results of time series that the XBP heating rate can be highly variable on short timescales, suggesting that it has a reconnection origin. C1 [Kariyappa, R.; Varghese, B. A.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Kariyappa, R.; DeLuca, E. E.; Saar, S. H.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dame, L.] LATMOS, F-78280 Guyancourt, France. [Pevtsov, A. A.] Natl Solar Observ, Sunspot, NM 88349 USA. RP Kariyappa, R (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. EM rkari@iiap.res.in RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Pevtsov, Alexei/0000-0003-0489-0920 FU JAXA; NAOJ (Japan); STFC (UK); NASA (USA); ESA; NSC (Norway) FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the postlaunch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA (USA), ESA, and NSC (Norway). We are grateful to the Hinode team for all their efforts in the design, build, and operation of the mission. The authors would like to thank Professors Loren Acton and Stuart M. Jefferies for stimulating discussion and valuable suggestions on this research. One of the authors (Kariyappa) wish to express his sincere thanks to Professor Siraj Hasan, Director, Indian Institute of Astrophysics for constant support and encouragement provided during this research work. The National Solar Observatory (NSO) is operated by the Association for Research in Astronomy (AURA, Inc.) under cooperative agreement with the National Science Foundation (NSF). We wish to express our sincere thanks to referee for valuable comments and suggestions that improved the manuscript considerably. NR 37 TC 11 Z9 11 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A78 DI 10.1051/0004-6361/201014878 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400090 ER PT J AU Moscadelli, L Cesaroni, R Rioja, MJ Dodson, R Reid, MJ AF Moscadelli, L. Cesaroni, R. Rioja, M. J. Dodson, R. Reid, M. J. TI Methanol and water masers in IRAS 20126+4104: the distance, the disk, and the jet SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: individual objects: IRAS 20126+4104; masers; proper motions ID STAR-FORMING REGIONS; HIGH-MASS STAR; VLBI OBSERVATIONS; TRIGONOMETRIC PARALLAXES; MOLECULAR OUTFLOW; IRAS-20126+4104; SYSTEM; IRAS20126+4104; PROTOSTARS; ACCRETION AB Context. Knowledge of the distance to high-mass star forming regions is crucial to obtain accurate luminosity and mass estimates of young OB-type (proto) stars and thus better constrain their nature and age. IRAS 20126+4104 is a special case, being the best candidate of a high-mass (proto) star surrounded by an accretion disk. Such a fact may be used to set constraints on theories of high-mass star formation, but requires confirmation that the mass and luminosity of IRAS 20126+4104 are indeed typical of a B0.5 star, which in turn requires an accurate estimate of the distance. Aims. The goal of our study is twofold: to determine the distance to IRAS 20126+4104, using the parallax of H2O masers associated with the source, and unveil the 3D velocity field of the disk, through proper motion measurements of the 6.7 GHz CH3OH masers. At the same time, we can also obtain an estimate of the systemic velocity in the plane of the sky of the disk+star system. Methods. We used the Very Long Baseline Array and the European VLBI Network to observe the 22.2 GHz H2O and 6.7 GHz CH3OH masers in IRAS 20126+4104 at a number of epochs suitably distributed in time. The absolute positions of the maser features were established with respect to reference quasars, which allowed us to derive absolute proper motions. Results. From the parallax of the H2O masers we obtain a distance of 1.64 +/- 0.05 kpc, which is very similar to the value adopted so far in the literature (1.7 kpc) and confirms that IRAS 20126+4104 is a high-mass (proto) star. From the CH3OH masers we derive the component in the plane of the sky of the systemic velocity of the disk+star system (-16 km s(-1) in right-ascension and +7.6 km s(-1) in declination). Accurate knowledge of the distance and systemic velocity allows us to improve on the model fit to the H2O maser jet presented in a previous study. Finally, we identify two groups of CH3OH maser features, one undergoing rotation in the disk and possibly distributed along a narrow ring centered on the star, the other characterised by relative proper motions indicating that the features are moving away from the disk, perpendicular to it. We speculate that the latter group might be tracing the disk material marginally entrained by the jet. Conclusions. VLBI multi-epoch observations with phase referencing are confirmed to be an excellent tool for distance determinations and for the investigation of the structure and 3D velocity field within a few 100 AU from newly born high-mass stars. C1 [Moscadelli, L.; Cesaroni, R.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Rioja, M. J.; Dodson, R.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia. [Rioja, M. J.] Observ Astron Nacl, Madrid 28803, Spain. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moscadelli, L (reprint author), INAF, Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. EM mosca@arcetri.astro.it; cesa@arcetri.astro.it OI Moscadelli, Luca/0000-0002-8517-8881; Cesaroni, Riccardo/0000-0002-2430-5103 FU European Community under RadioNet [R113CT 2003 5058187]; European Community [227290] FX We thank Francesca Bacciotti for useful discussions about the properties of X-winds and disk-winds. We also thank the referee, Gary Fuller, for his careful reading of the manuscript and useful suggestions. This work has benefited from research funding from the European Community's sixth Framework Programme under RadioNet R113CT 2003 5058187 and has been partly supported by the European Community Framework Programme 7, Advanced Radio Astronomy in Europe, grant agreement No. 227290. NR 38 TC 33 Z9 33 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A66 DI 10.1051/0004-6361/201015641 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400078 ER PT J AU Murgia, M Parma, P Mack, KH de Ruiter, HR Fanti, R Govoni, F Tarchi, A Giacintucci, S Markevitch, M AF Murgia, M. Parma, P. Mack, K. -H. de Ruiter, H. R. Fanti, R. Govoni, F. Tarchi, A. Giacintucci, S. Markevitch, M. TI Dying radio galaxies in clusters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radio continuum: galaxies; galaxies: active; galaxies: clusters: general ID NORTH ECLIPTIC POLE; SKY SURVEY; 6C SURVEY; ELLIPTICAL GALAXIES; SYNCHROTRON SPECTRA; RENEWED ACTIVITY; BRIGHT GALAXIES; LOW-LUMINOSITY; MHZ SURVEY; SAMPLE AB Aims. We present a study of five "dying" nearby (z <= 0.2) radio galaxies belonging to both the WENSS minisurvey and the B2 bright catalogs WNB1734+6407, WNB1829+6911, WNB1851+5707, B2 0120+33, and B2 1610+29. Methods. These sources have been selected on the basis of their extremely steep broad-band radio spectra, which strongly indicates that either these objects belong to the rare class of dying radio galaxies or we are observing "fossil" radio plasma remaining from a previous instance of nuclear activity. We derive the relative duration of the dying phase from the fit of a synchrotron radiative model to the radio spectra of the sources. Results. The modeling of the integrated spectra and the deep spectral index images obtained with the VLA confirmed that in these sources the central engine has ceased to be active for a significant fraction of their lifetime, although their extended lobes have not yet completely faded away. We found that WNB1851+5707 is in reality composed of two distinct dying galaxies, which appear blended together as a single source in the WENSS. In the cases of WNB1829+6911 and B2 0120+33, the fossil radio lobes are seen in conjunction with a currently active core. A very faint core is also detected in a MERLIN image of WNB1851+5707a, one of the two dying sources composing WNB1851+5707. We found that all sources in our sample are located (at least in projection) at the center of an X-ray emitting cluster. Conclusions. Our results suggest that the duration of the dying phase for a radio source in a cluster can be significantly higher than that of a radio galaxy in the field, although no firm conclusions can be drawn because of the small number statistics involved. The simplest interpretation of the tendency for dying galaxies to be found in clusters is that the low-frequency radio emission from the fading radio lobes lasts longer if their expansion is somewhat reduced or even stopped. Another possibility is that the occurrence of dying sources is higher in galaxy clusters. We argue that radio sources in dense environments, such as the center of cooling core clusters, may have a peculiar accretion mode which results in a bursting duty cycle sequence of active and quiescent periods. This result could have important implications for theories of the life cycles of radio sources and AGN feedback in clusters of galaxies but awaits confirmation from future observations of larger, statistically significant, samples of objects. C1 [Murgia, M.; Govoni, F.; Tarchi, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, CA, Italy. [Parma, P.; Mack, K. -H.; de Ruiter, H. R.; Fanti, R.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Giacintucci, S.; Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Murgia, M (reprint author), Osservatorio Astron Cagliari, INAF, Loc Poggio Pini,Str 54, I-09012 Capoterra, CA, Italy. EM matteo@oa-cagliari.inaf.it OI Tarchi, Andrea/0000-0001-8540-3500; Murgia, Matteo/0000-0002-4800-0806; Govoni, Federica/0000-0003-3644-3084 FU Chandra grant [GO9-0133X]; NASA [NAS8-39073]; Smithsonian Institution; ASI-INAF [I/009/10/0]; European Community [R113CT 2003 5058187] FX We are grateful to the anonymous referee for very useful comments that improved this paper. FG and MM thank the hospitality of the Harvard-Smithsonian Center for Astrophysics where part of this research was done. Support was provided by Chandra grant GO9-0133X, NASA contract NAS8-39073, and the Smithsonian Institution. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under contract with the National Science Foundation. This research made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. MERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of STFC. This work has benefited from research funding from the European Community's sixth Framework Programme under RadioNet R113CT 2003 5058187. This research made use also of the CATS Database (Astrophysical CATalogs support System). The optical DSS2 red images were taken from: http://archive.eso.org/dss/dss. We thank the staff of the National Galileo Telescope (TNG) for carrying out the optical observations in service mode. NR 52 TC 31 Z9 31 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A148 DI 10.1051/0004-6361/201015302 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400160 ER PT J AU Nordin, J Ostman, L Goobar, A Amanullah, R Nichol, RC Smith, M Sollerman, J Bassett, BA Frieman, J Garnavich, PM Leloudas, G Sako, M Schneider, DP AF Nordin, J. Ostman, L. Goobar, A. Amanullah, R. Nichol, R. C. Smith, M. Sollerman, J. Bassett, B. A. Frieman, J. Garnavich, P. M. Leloudas, G. Sako, M. Schneider, D. P. TI Spectral properties of type Ia supernovae up to z similar to 0.3 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; techniques: spectroscopic; supernovae: general; cosmology: observations; line: profiles ID DIGITAL SKY SURVEY; NEAR-INFRARED OBSERVATIONS; HOST GALAXIES; K-CORRECTIONS; LIGHT CURVES; SPECTROSCOPIC OBSERVATIONS; OPTICAL SPECTROSCOPY; IMPROVED DISTANCES; HUBBLE DIAGRAM; DARK ENERGY AB Aims. Spectroscopic observations of type Ia supernovae obtained at the New Technology Telescope (NTT) and the Nordic Optical Telescope (NOT), in conjunction with the SDSS-II Supernova Survey, are analysed. We use spectral indicators measured up to a month after the lightcurve peak luminosity to characterise the supernova properties, and examine these for potential correlations with host galaxy type, lightcurve shape, colour excess, and redshift. Methods. Our analysis is based on 89 type Ia supernovae at a redshift interval z = 0.05-0.3, for which multiband SDSS photometry is available. A lower-z spectroscopy reference sample was used for comparisons over cosmic time. We present measurements of time series of pseudo equivalent widths and line velocities of the main spectral features in type Ia supernovae. Results. Supernovae with shallower features are found predominantly among the intrinsically brighter slow declining supernovae. We detect the strongest correlation between lightcurve stretch and the Si II lambda 4000 absorption feature, which also correlates with the estimated mass and star formation rate of the host galaxy. We also report a tentative correlation between colour excess and spectral properties. If confirmed, this would suggest that moderate reddening of type Ia supernovae is dominated by effects in the explosion or its immediate environment, as opposed to extinction by interstellar dust. C1 [Nordin, J.; Ostman, L.; Goobar, A.; Amanullah, R.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden. [Nordin, J.; Ostman, L.; Goobar, A.; Amanullah, R.; Sollerman, J.] Oskar Klein Ctr Cosmo Particle Phys, S-10691 Stockholm, Sweden. [Ostman, L.] Inst Fis Altes Energies, Barcelona 08193, Spain. [Nichol, R. C.; Smith, M.] Inst Cosmol & Gravitat, Portsmouth PO13FX, Hants, England. [Smith, M.; Bassett, B. A.] Univ Cape Town, Dept Math & Appl Math, ZA-7925 Cape Town, South Africa. [Sollerman, J.; Leloudas, G.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Sollerman, J.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Bassett, B. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Bassett, B. A.] African Inst Math Sci, Cape Town, South Africa. [Frieman, J.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Garnavich, P. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garnavich, P. M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Nordin, J (reprint author), Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden. EM nordin@physto.se OI Sollerman, Jesper/0000-0003-1546-6615 FU Alfred P. Sloan Foundation; National Aeronautics and Space Administration; National Science Foundation; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; University of Chicago; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; University of Pittsburgh; Princeton University; United States Naval Observatory; University of Washington; Swedish Research Council; Danish National Research Foundation; Swedish Foundation for International Cooperation in Research and Higher Education (STINT) FX We thank the anonymous referee for valuable comments. We also thank Ryan J. Foley for helpful discussions. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. The paper is partly based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The data have been taken using ALFOSC, which is owned by the Instituto de Astrofisica de Andalucia (IAA) and operated at the Nordic Optical Telescope under agreement between IAA and the NBI. This paper is partly based on observations collected at the New Technology Telescope (NTT), operated by the European Organisation for Astronomical Research in the Southern Hemisphere, Chile. The Oskar Klein Centre is funded by the Swedish Research Council. The Dark Cosmology Centre is funded by the Danish National Research Foundation. We thank the Swedish Foundation for International Cooperation in Research and Higher Education (STINT) for financial support. NR 111 TC 12 Z9 12 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A119 DI 10.1051/0004-6361/201015705 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400131 ER PT J AU Wilcock, LA Kirk, JM Stamatellos, D Ward-Thompson, D Whitworth, A Battersby, C Brunt, C Fuller, GA Griffin, M Molinari, S Martin, P Mottram, JC Peretto, N Plume, R Smith, HA Thompson, MA AF Wilcock, L. A. Kirk, J. M. Stamatellos, D. Ward-Thompson, D. Whitworth, A. Battersby, C. Brunt, C. Fuller, G. A. Griffin, M. Molinari, S. Martin, P. Mottram, J. C. Peretto, N. Plume, R. Smith, H. A. Thompson, M. A. TI The initial conditions of high-mass star formation: radiative transfer models of IRDCs seen in the Herschel Hi-GAL survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: clouds; dust, extinction ID INFRARED-DARK CLOUDS; PRESTELLAR CORES; GALACTIC PLANE; DUST OPACITIES; MILKY-WAY; SPIRE; PROTOSTARS; DENSITY; RADIO; PACS AB The densest infrared dark clouds (IRDCs) may represent the earliest observable stage of high-mass star formation. These clouds are very cold, hence they emit mainly at far-infrared and sub-mm wavelengths. For the first time, Herschel has provided multi-wavelength, spatially resolved observations of cores within IRDCs, which, when combined with radiative transfer modelling, can constrain their properties, such as mass, density profile and dust temperature. We use a 3D, multi-wavelength Monte Carlo radiative transfer code to model in detail the emission from six cores in three typical IRDCs seen in the Hi-GAL survey (G030.50+00.95, G031.03+00.26 and G031.03+00.76), and thereby to determine the properties of these cores and compare them with their low-mass equivalents. We found masses ranging from 90 to 290 M(circle dot) with temperatures from 8 to 11 K at the centre of each core and 18 to 28 K at the surface. The maximum luminosity of an embedded star within each core was calculated, and we rule out the possibility of significant high mass star formation having yet occurred in three of our cores. C1 [Wilcock, L. A.; Kirk, J. M.; Stamatellos, D.; Ward-Thompson, D.; Whitworth, A.; Griffin, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Battersby, C.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Brunt, C.; Mottram, J. C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Fuller, G. A.; Peretto, N.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Molinari, S.] CNR, Inst Fis Spazio Interplanetario, I-00133 Rome, Italy. [Martin, P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Peretto, N.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IFRU,Serv Astrophys,CE Saclay, F-91191 Gif Sur Yvette, France. [Plume, R.] Univ Calgary, Dept Phys Astron, Calgary, AB T2N 1N4, Canada. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. RP Wilcock, LA (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. EM lucy.wilcock@astro.cf.ac.uk RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Stamatellos, Dimitris/0000-0002-4502-8344 FU STFC; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX L.A.W. acknowledges STFC studentship funding. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This work is also based, in part, on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 37 TC 10 Z9 10 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2011 VL 526 AR A159 DI 10.1051/0004-6361/201015488 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709RF UT WOS:000286458400171 ER PT J AU Abdo, AA Ackermann, M Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Baring, MG Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bouvier, A Brandt, TJ Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Cannon, A Caraveo, PA Carrigan, S Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S Dermer, CD de Palma, F Silva, EDE Drell, PS Dubois, R Dumora, D Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Frailis, M Fuhrmann, L Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Guillemot, L Guiriec, S Hayashida, M Hays, E Horan, D Hughes, RE Johannesson, G Johnson, AS Johnson, WN Kadler, M Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Max-Moerbeck, W Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nishino, S Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Paneque, D Panetta, JH Parent, D Pavlidou, V Pearson, TJ Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Readhead, A Reimer, A Reimer, O Richards, JL Ripken, J Ritz, S Roth, M Sadrozinski, HFW Sanchez, D Sander, A Scargle, JD Sgro, C Siskind, EJ Smith, PD Spandre, G Spinelli, P Stawarz, L Stevenson, M Strickman, MS Sokolovsky, KV Suson, DJ Takahashi, H Takahashi, T Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, F Tosti, G Tramacere, A Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Wehrle, AE Winer, BL Wood, KS Yang, Z Ylinen, T Zensus, JA Ziegler, M Aleksic, J Antonelli, LA Antoranz, P Backes, M Barrio, JA Gonzalez, JB Bednarek, W Berdyugin, A Berger, K Bernardini, E Biland, A Blanch, O Bock, RK Boller, A Bonnoli, G Bordas, P Tridon, DB Bosch-Ramon, V Bose, D Braun, I Bretz, T Camara, M Carmona, E Carosi, A Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Dazzi, F de Angelis, A del Pozo, ED De Lotto, B De Maria, M De Sabata, F Mendez, CD Ortega, AD Doert, M Dominguez, A Prester, DD Dorner, D Doro, M Elsaesser, D Ferenc, D Fonseca, MV Font, L Lopen, RJG Garczarczyk, M Gaug, M Giavitto, G Godinovi, N Hadasch, D Herrero, A Hildebrand, D Hohne-Monch, D Hose, J Hrupec, D Jogler, T Klepser, S Krahenbuhl, T Kranich, D Krause, J La Barbera, A Leonardo, E Lindfors, E Lombardi, S Lopez, M Lorenz, E Majumdar, P Makariev, E Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Mariotti, M Martinez, M Mazin, D Meucci, M Miranda, JM Mirzoyan, R Miyamoto, H Moldon, J Moralejo, A Nieto, D Nilsson, K Orito, R Oya, I Paoletti, R Paredes, JM Partini, S Pasanen, M Pauss, F Pegna, RG Perez-Torres, MA Persic, M Peruzzo, J Pochon, J Moroni, PGP Prada, F Prandini, E Puchades, N Puljak, I Reichardt, T Reinthal, R Rhode, W Ribo, M Rico, J Rissi, M Rugamer, S Saggion, A Saito, K Saito, TY Salvati, M Sanchez-Conde, M Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shayduk, M Shore, SN Sierpowska-Bartosik, A Sillanpaa, A Sitarek, J Sobczynska, D Spanier, F Spiro, S Stamerra, A Steinke, B Storz, J Strah, N Struebig, JC Suric, T Takalo, LO Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Vankov, H Wagner, RM Weitzel, Q Zabalza, V Zandanel, F Zanin, R Acciari, VA Arlen, T Aune, T Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Cannon, A Cesarini, A Ciupik, L Cui, W Dickherber, R Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Huang, D Hui, CM Humensky, TB Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Mukherjee, R Ong, R Otte, N Pandel, D Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Rovero, AC Schroedter, M Sembroski, GH Senturk, GD Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Varlotta, A Vincent, S Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wood, M Zitzer, B Villata, M Raiteri, CM Aller, HD Aller, MF Arkharov, AA Blinov, DA Calcidese, P Chen, WP Efimova, NV Kimeridze, G Konstantinova, TS Kopatskaya, EN Koptelova, E Kurtanidze, OM Kurtanidze, SO Lahteenmaki, A Larionov, VM Larionova, EG Larionova, LV Ligustri, R Morozova, DA Nikolashvili, MG Sigua, LA Troitsky, IS Angelakis, E Capalbi, M Carraminana, A Carrasco, L Cassaro, P de la Fuente, E Gurwell, MA Kovalev, YY Kovalev, YA Krichbaum, TP Krimm, HA Leto, P Lister, ML Maccaferri, G Moody, JW Mori, Y Nestoras, I Orlati, A Pagani, C Pace, C Pearson, R Perri, M Piner, BG Pushkarev, AB Ros, E Sadun, AC Sakamoto, T Tornikoski, M Yatsu, Y Zook, A AF Abdo, A. A. Ackermann, M. Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Baring, M. G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bouvier, A. Brandt, T. J. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Cannon, A. Caraveo, P. A. Carrigan, S. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, O. . Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. Dermer, C. D. de Palma, F. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fortin, P. Frailis, M. Fuhrmann, L. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Guillemot, L. Guiriec, S. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, W. N. Kadler, M. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Max-Moerbeck, W. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nishino, S. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Parent, D. Pavlidou, V. Pearson, T. J. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Readhead, A. Reimer, A. Reimer, O. Richards, J. L. Ripken, J. Ritz, S. Roth, M. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Scargle, J. D. Sgro, C. Siskind, E. J. Smith, P. D. Spandre, G. Spinelli, P. Stawarz, L. Stevenson, M. Strickman, M. S. Sokolovsky, K. V. Suson, D. J. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Wehrle, A. E. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Zensus, J. A. Ziegler, M. Aleksic, J. Antonelli, L. A. Antoranz, P. Backes, M. Barrio, J. A. Gonzalez, J. Becerra Bednarek, W. Berdyugin, A. Berger, K. Bernardini, E. Biland, A. Blanch, O. Bock, R. K. Boller, A. Bonnoli, G. Bordas, P. Tridon, D. Borla Bosch-Ramon, V. Bose, D. Braun, I. Bretz, T. Camara, M. Carmona, E. Carosi, A. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Dazzi, F. de Angelis, A. del Pozo, E. De Cea De Lotto, B. De Maria, M. De Sabata, F. Mendez, C. Delgado Ortega, A. Diago Doert, M. Dominguez, A. Prester, D. Dominis Dorner, D. Doro, M. Elsaesser, D. Ferenc, D. Fonseca, M. V. Font, L. Lopen, R. J. Garcia Garczarczyk, M. Gaug, M. Giavitto, G. Godinovi, N. Hadasch, D. Herrero, A. Hildebrand, D. Hoehne-Moench, D. Hose, J. Hrupec, D. Jogler, T. Klepser, S. Kraehenbuehl, T. Kranich, D. Krause, J. La Barbera, A. Leonardo, E. Lindfors, E. Lombardi, S. Lopez, M. Lorenz, E. Majumdar, P. Makariev, E. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Mariotti, M. Martinez, M. Mazin, D. Meucci, M. Miranda, J. M. Mirzoyan, R. Miyamoto, H. Moldon, J. Moralejo, A. Nieto, D. Nilsson, K. Orito, R. Oya, I. Paoletti, R. Paredes, J. M. Partini, S. Pasanen, M. Pauss, F. Pegna, R. G. Perez-Torres, M. A. Persic, M. Peruzzo, J. Pochon, J. Moroni, P. G. Prada Prada, F. Prandini, E. Puchades, N. Puljak, I. Reichardt, T. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Rissi, M. Ruegamer, S. Saggion, A. Saito, K. Saito, T. Y. Salvati, M. Sanchez-Conde, M. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Shayduk, M. Shore, S. N. Sierpowska-Bartosik, A. Sillanpaa, A. Sitarek, J. Sobczynska, D. Spanier, F. Spiro, S. Stamerra, A. Steinke, B. Storz, J. Strah, N. Struebig, J. C. Suric, T. Takalo, L. O. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Vankov, H. Wagner, R. M. Weitzel, Q. Zabalza, V. Zandanel, F. Zanin, R. Acciari, V. A. Arlen, T. Aune, T. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Cannon, A. Cesarini, A. Ciupik, L. Cui, W. Dickherber, R. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Huang, D. Hui, C. M. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Mukherjee, R. Ong, R. Otte, N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Rovero, A. C. Schroedter, M. Sembroski, G. H. Senturk, G. D. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vincent, S. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wood, M. Zitzer, B. Villata, M. Raiteri, C. M. Aller, H. D. Aller, M. F. Arkharov, A. A. Blinov, D. A. Calcidese, P. Chen, W. P. Efimova, N. V. Kimeridze, G. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kurtanidze, O. M. Kurtanidze, S. O. Lahteenmaki, A. Larionov, V. M. Larionova, E. G. Larionova, L. V. Ligustri, R. Morozova, D. A. Nikolashvili, M. G. Sigua, L. A. Troitsky, I. S. Angelakis, E. Capalbi, M. Carraminana, A. Carrasco, L. Cassaro, P. de la Fuente, E. Gurwell, M. A. Kovalev, Y. Y. Kovalev, Yu. A. Krichbaum, T. P. Krimm, H. A. Leto, P. Lister, M. L. Maccaferri, G. Moody, J. W. Mori, Y. Nestoras, I. Orlati, A. Pagani, C. Pace, C. Pearson, R., III Perri, M. Piner, B. G. Pushkarev, A. B. Ros, E. Sadun, A. C. Sakamoto, T. Tornikoski, M. Yatsu, Y. Zook, A. CA Fermi-LAT Collaboration MAGIC Collaboration VERITAS Collaboration TI INSIGHTS INTO THE HIGH-ENERGY gamma-RAY EMISSION OF MARKARIAN 501 FROM EXTENSIVE MULTIFREQUENCY OBSERVATIONS IN THE FERMI ERA SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; BL Lacertae objects: general; BL Lacertae objects: individual (Mrk 501); galaxies: active; gamma rays: general; radiation mechanisms: non-thermal ID BL LACERTAE OBJECTS; CHERENKOV TELESCOPE SYSTEM; MAGNETOSONIC SHOCK-WAVES; ACTIVE GALACTIC NUCLEI; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE; EARLY-TYPE GALAXIES; X-RAY; PARTICLE-ACCELERATION; TEV VARIABILITY AB We report on the gamma-ray activity of the blazar Mrk 501 during the first 480 days of Fermi operation. We find that the average Large Area Telescope (LAT) gamma-ray spectrum of Mrk 501 can be well described by a single power-law function with a photon index of 1.78 +/- 0.03. While we observe relatively mild flux variations with the Fermi-LAT (within less than a factor of two), we detect remarkable spectral variability where the hardest observed spectral index within the LAT energy range is 1.52 +/- 0.14, and the softest one is 2.51 +/- 0.20. These unexpected spectral changes do not correlate with the measured flux variations above 0.3 GeV. In this paper, we also present the first results from the 4.5 month long multifrequency campaign (2009 March 15-August 1) on Mrk 501, which included the Very Long Baseline Array (VLBA), Swift, RXTE, MAGIC, and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent temporal and energy coverage of the source throughout the entire campaign. The extensive radio to TeV data set from this campaign provides us with the most detailed spectral energy distribution yet collected for this source during its relatively low activity. The average spectral energy distribution of Mrk 501 is well described by the standard one-zone synchrotron self-Compton (SSC) model. In the framework of this model, we find that the dominant emission region is characterized by a size less than or similar to 0.1 pc (comparable within a factor of few to the size of the partially resolved VLBA core at 15-43 GHz), and that the total jet power (similar or equal to 10(44) erg s(-1)) constitutes only a small fraction (similar to 10(-3)) of the Eddington luminosity. The energy distribution of the freshly accelerated radiating electrons required to fit the time-averaged data has a broken power-law form in the energy range 0.3 GeV-10 TeV, with spectral indices 2.2 and 2.7 below and above the break energy of 20 GeV. We argue that such a form is consistent with a scenario in which the bulk of the energy dissipation within the dominant emission zone of Mrk 501 is due to relativistic, proton-mediated shocks. We find that the ultrarelativistic electrons and mildly relativistic protons within the blazar zone, if comparable in number, are in approximate energy equipartition, with their energy dominating the jet magnetic field energy by about two orders of magnitude. C1 [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Shore, S. N.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Peruzzo, J.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Peruzzo, J.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Brandt, T. J.; Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] M Merlin Univ, Dipartimento Fis, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Horan, D.] CNRS, IN2P3, Lab Leprince Ringuet, Ecole Polytech, Palaiseau, France. [Caliandro, G. A.; Torres, F.; del Pozo, E. De Cea; Hadasch, D.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Cannon, A.; Celik, O. .; Ferrara, E. C.; Gehrels, N.; Hays, E.; Kadler, M.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Vasileiou, V.; Krimm, H. A.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cannon, A.; Cannon, A.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Dublin 4, Ireland. [Caraveo, P. A.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Capalbi, M.; Perri, M.] ASI, Sci Data Ctr, I-00044 Rome, Italy. [Celik, O. .; Kadler, M.; Moiseev, A. A.; Vasileiou, V.; Krimm, H. A.] CRESST, Greenbelt, MD 20771 USA. [Celik, O. .; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, O. .; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Conrad, J.; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Ripken, J.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Dumora, D.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Frailis, M.; Dazzi, F.; de Angelis, A.; Mankuzhiyil, N.; Persic, M.; Scapin, V.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [Frailis, M.; Dazzi, F.; de Angelis, A.; Mankuzhiyil, N.; Persic, M.; Scapin, V.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Fuhrmann, L.; Guillemot, L.; Sokolovsky, K. V.; Zensus, J. A.; Angelakis, E.; Kovalev, Y. Y.; Krichbaum, T. P.; Nestoras, I.; Ros, E.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Fukazawa, Y.; Katagiri, H.; Mizuno, T.; Nishino, S.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Giroletti, M.] Ist Radioastron, INAF, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Kadler, M.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kadler, M.; Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Max-Moerbeck, W.; Pavlidou, V.; Pearson, T. J.; Readhead, A.; Richards, J. L.; Stevenson, M.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Okumura, A.; Stawarz, L.; Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Paneque, D.; Bock, R. K.; Tridon, D. Borla; Carmona, E.; Colin, P.; Hose, J.; Jogler, T.; Krause, J.; Lorenz, E.; Mirzoyan, R.; Miyamoto, H.; Orito, R.; Saito, K.; Saito, T. Y.; Schweizer, T.; Shayduk, M.; Sitarek, J.; Steinke, B.; Teshima, M.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.; Aune, T.; Furniss, A.; Otte, N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.; Aune, T.; Furniss, A.; Otte, N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Sokolovsky, K. V.; Kovalev, Y. Y.; Kovalev, Yu. A.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, F.; Rico, J.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA. [Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Aleksic, J.; Blanch, O.; Cortina, J.; Giavitto, G.; Klepser, S.; Majumdar, P.; Martinez, M.; Mazin, D.; Moldon, J.; Moralejo, A.; Puchades, N.; Reichardt, T.; Rico, J.; Tescaro, D.; Zanin, R.] Univ Autonoma Barcelona, IFAE, E-08193 Bellaterra, Barcelona, Spain. [Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Pegna, R. G.; Moroni, P. G. Prada; Stamerra, A.] Univ Siena, I-53100 Siena, Italy. [Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Pegna, R. G.; Moroni, P. G. Prada; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy. [Backes, M.; Doert, M.; Rhode, W.; Strah, N.] Tech Univ Dortmund, D-44221 Dortmund, Germany. [Barrio, J. A.; Bose, D.; Camara, M.; Contreras, J. L.; Fonseca, M. V.; Nieto, D.; Oya, I.] Univ Complutense, E-28040 Madrid, Spain. [Gonzalez, J. Becerra; Berger, K.; Ortega, A. Diago; Lopen, R. J. Garcia; Herrero, A.; Sanchez-Conde, M.] Univ La Laguna, Dept Astrophys, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Bednarek, W.; Sierpowska-Bartosik, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland. [Berdyugin, A.; Lindfors, E.; Nilsson, K.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, FIN-21500 Piikkio, Finland. [Bernardini, E.; Satalecka, K.; Maier, G.; Pohl, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Biland, A.; Boller, A.; Braun, I.; Dorner, D.; Hildebrand, D.; Kraehenbuehl, T.; Kranich, D.; Lorenz, E.; Pauss, F.; Rissi, M.; Weitzel, Q.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Bordas, P.; Bosch-Ramon, V.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona ICC IEED, E-08028 Barcelona, Spain. [Bretz, T.; Elsaesser, D.; Hoehne-Moench, D.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Storz, J.; Struebig, J. C.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [De Lotto, B.; De Maria, M.; De Sabata, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [De Lotto, B.; De Maria, M.; De Sabata, F.] Univ Trieste, I-34127 Trieste, Italy. [Mendez, C. Delgado] Ctr Invest Energet Medioambientales & Tecnol CIE, Madrid, Spain. [Dominguez, A.; Perez-Torres, M. A.; Prada, F.; Zandanel, F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Prester, D. Dominis; Ferenc, D.; Godinovi, N.; Hrupec, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia. [Font, L.] Univ Autonoma Barcelona, E-08193 Barcelona, Spain. [Makariev, E.; Maneva, G.; Temnikov, P.; Vankov, H.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria. [Maraschi, L.; Tavecchio, F.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Persic, M.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Salvati, M.; Spiro, S.] INAF Natl Inst Astrophys, I-00136 Rome, Italy. [Shore, S. N.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy. [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Arlen, T.; Ong, R.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Galway, Ireland. [Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.; Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Huang, D.; Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Krennrich, F.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pichel, A.; Rovero, A. C.] Parbellon IAFE, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina. [Pohl, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Senturk, G. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Steele, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Arkharov, A. A.; Blinov, D. A.; Efimova, N. V.; Larionov, V. M.; Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia. [Chen, W. P.; Koptelova, E.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan. [Efimova, N. V.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Nikolashvili, M. G.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Kimeridze, G.; Kurtanidze, O. M.; Kurtanidze, S. O.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Ligustri, R.] Circolo Astrofili Talmassons, I-33030 Campoformido, UD, Italy. [Carraminana, A.; Carrasco, L.] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico. [Cassaro, P.] Ist Radioastron, Sez Noto, INAF, I-96017 Noto, SR, Italy. [de la Fuente, E.] Univ Guadalajara, CUCEI, Dpto Fis, Inst Astron & Meteorol, Jalisco, Mexico. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leto, P.] Osserv Astrofis Catania, I-95123 Catania, Italy. [Maccaferri, G.; Orlati, A.] Ist Radioastron, INAF, Staz Radioastron Med, I-40059 Bologna, Italy. [Moody, J. W.; Pace, C.; Pearson, R., III] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. [Mori, Y.; Yatsu, Y.] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan. [Pagani, C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Piner, B. G.] Whittier Coll, Dept Phys & Astron, Whittier, CA USA. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. [Ros, E.] Univ Valencia, Valencia 46010, Spain. [Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80220 USA. [Zook, A.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden. RP Paneque, D (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. EM dpaneque@mppmu.mpg.de; stawarz@astro.isas.jaxa.jp RI Sgro, Carmelo/K-3395-2016; Maneva, Galina/L-7120-2016; Backes, Michael/N-5126-2016; Torres, Diego/O-9422-2016; Temnikov, Petar/L-6999-2016; Orlando, E/R-5594-2016; Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Grishina, Tatiana/H-6873-2013; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Pushkarev, Alexander/M-9997-2015; Miranda, Jose Miguel/F-2913-2013; Font, Lluis/L-4197-2014; Moskalenko, Igor/A-1301-2007; Contreras Gonzalez, Jose Luis/K-7255-2014; Mazziotta, Mario /O-8867-2015; Lopez Moya, Marcos/L-2304-2014; GAug, Markus/L-2340-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Kovalev, Yuri/J-5671-2013; Funk, Stefan/B-7629-2015; Pavlidou, Vasiliki/C-2944-2011; Sokolovsky, Kirill/D-2246-2015; Antoranz, Pedro/H-5095-2015; Delgado, Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Kovalev, Yuri/N-1053-2015; Pearson, Timothy/N-2376-2015; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013; Efimova, Natalia/I-2196-2013; Blinov, Dmitry/G-9925-2013; Rando, Riccardo/M-7179-2013; Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Prada Moroni, Pier Giorgio/G-5565-2011; Braun, Isabel/C-9373-2012; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; Mannheim, Karl/F-6705-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; Doro, Michele/F-9458-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Fonseca Gonzalez, Maria Victoria/I-2004-2015; OI Backes, Michael/0000-0002-9326-6400; Torres, Diego/0000-0002-1522-9065; Temnikov, Petar/0000-0002-9559-3384; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Villata, Massimo/0000-0003-1743-6946; Larionova, Liudmila/0000-0002-0274-1481; Leto, Paolo/0000-0003-4864-2806; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Grishina, Tatiana/0000-0002-3953-6676; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Miranda, Jose Miguel/0000-0002-1472-9690; Font, Lluis/0000-0003-2109-5961; Moskalenko, Igor/0000-0001-6141-458X; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Mazziotta, Mario /0000-0001-9325-4672; Lopez Moya, Marcos/0000-0002-8791-7908; GAug, Markus/0000-0001-8442-7877; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Kovalev, Yuri/0000-0001-9303-3263; Funk, Stefan/0000-0002-2012-0080; Pavlidou, Vasiliki/0000-0002-0870-1368; Sokolovsky, Kirill/0000-0001-5991-6863; Antoranz, Pedro/0000-0002-3015-3601; Delgado, Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755; Pearson, Timothy/0000-0001-5213-6231; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500; Efimova, Natalia/0000-0002-8071-4753; Blinov, Dmitry/0000-0003-0611-5784; Rico, Javier/0000-0003-4137-1134; Braun, Isabel/0000-0002-9389-0502; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; Doro, Michele/0000-0001-9104-3214; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Frailis, Marco/0000-0002-7400-2135; Cesarini, Andrea/0000-0002-8611-8610; leonardo, elvira/0000-0003-0271-7673; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; Caraveo, Patrizia/0000-0003-2478-8018; De Lotto, Barbara/0000-0003-3624-4480; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Persic, Massimo/0000-0003-1853-4900; Ward, John E/0000-0003-1973-0794; Cassaro, Pietro/0000-0001-5139-9662; Giordano, Francesco/0000-0002-8651-2394; Orlati, Andrea/0000-0001-8737-255X; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; De Angelis, Alessandro/0000-0002-3288-2517; LA BARBERA, ANTONINO/0000-0002-5880-8913; Cui, Wei/0000-0002-6324-5772 FU K. A. Wallenberg Foundation; International Doctorate on Astroparticle Physics (IDAPP) program; INFN Padova; Academy of Finland [212656, 210338]; National Radio Astronomy Observatory's Very Long Baseline Array (VLBA) [BK150, BP143, MOJAVE]; Russian RFBR foundation [09-02-00092]; Georgian National Science Foundation [GNSF/ST07/4-180]; NASA [NNX08AW31G]; NSF [AST-0808050] FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; Partially supported by the International Doctorate on Astroparticle Physics (IDAPP) program.; Supported by INFN Padova.; We acknowledge the use of public data from the Swift and RXTE data archive. The Metsahovi team acknowledges the support from the Academy of Finland to the observing projects (numbers 212656, 210338, among others). This research has made use of data obtained from the National Radio Astronomy Observatory's Very Long Baseline Array (VLBA), projects BK150, BP143, and MOJAVE. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. St. Petersburg University team acknowledges support from Russian RFBR foundation via grant 09-02-00092. AZT-24 observations are made within an agreement between Pulkovo, Rome and Teramo observatories. This research is partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg, as well as with the Medicina and Noto telescopes operated by INAF-Istituto di Radioastronomia. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. M. Villata organized the optical-to-radio observations by GASP-WEBT as the president of the collaboration. Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST07/4-180. The OVRO 40 m program was funded in part by NASA (NNX08AW31G) and the NSF (AST-0808050). NR 122 TC 92 Z9 92 U1 4 U2 39 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2011 VL 727 IS 2 AR 129 DI 10.1088/0004-637X/727/2/129 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000068 ER PT J AU Campo, CJ Harrington, J Hardy, RA Stevenson, KB Nymeyer, S Ragozzine, D Lust, NB Anderson, DR Collier-Cameron, A Blecic, J Britt, CBT Bowman, WC Wheatley, PJ Loredo, TJ Deming, D Hebb, L Hellier, C Maxted, PFL Pollaco, D West, RG AF Campo, Christopher J. Harrington, Joseph Hardy, Ryan A. Stevenson, Kevin B. Nymeyer, Sarah Ragozzine, Darin Lust, Nate B. Anderson, David R. Collier-Cameron, Andrew Blecic, Jasmina Britt, Christopher B. T. Bowman, William C. Wheatley, Peter J. Loredo, Thomas J. Deming, Drake Hebb, Leslie Hellier, Coel Maxted, Pierre F. L. Pollaco, Don West, Richard G. TI ON THE ORBIT OF EXOPLANET WASP-12b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (WASP-12); techniques: photometric ID SPITZER-SPACE-TELESCOPE; EXTRASOLAR GIANT PLANETS; INFRARED ARRAY CAMERA; THERMAL EMISSION; TIDAL EVOLUTION; BAND EMISSION; LIGHT CURVES; ATMOSPHERE; INVERSION; SYSTEMS AB We observed two secondary eclipses of the exoplanet WASP-12b using the Infrared Array Camera on the Spitzer Space Telescope. The close proximity of WASP-12b to its G-type star results in extreme tidal forces capable of inducing apsidal precession with a period as short as a few decades. This precession would be measurable if the orbit had a significant eccentricity, leading to an estimate of the tidal Love number and an assessment of the degree of central concentration in the planetary interior. An initial ground-based secondary-eclipse phase reported by Lopez-Morales et al. (0.510 +/- 0.002) implied eccentricity at the 4.5 sigma level. The spectroscopic orbit of Hebb et al. has eccentricity 0.049 +/- 0.015, a 3 sigma result, implying an eclipse phase of 0.509 +/- 0.007. However, there is a well-documented tendency of spectroscopic data to overestimate small eccentricities. Our eclipse phases are 0.5010 +/- 0.0006 (3.6 and 5.8 mu m) and 0.5006 +/- 0.0007 (4.5 and 8.0 mu m). An unlikely orbital precession scenario invoking an alignment of the orbit during the Spitzer observations could have explained this apparent discrepancy, but the final eclipse phase of Lopez-Morales et al. (0.510 +/-(+0.007)(-0.006)) is consistent with a circular orbit at better than 2 sigma. An orbit fit to all the available transit, eclipse, and radial-velocity data indicates precession at < 1 sigma; a non-precessing solution fits better. We also comment on analysis and reporting for Spitzer exoplanet data in light of recent re-analyses. C1 [Campo, Christopher J.; Harrington, Joseph; Hardy, Ryan A.; Stevenson, Kevin B.; Nymeyer, Sarah; Lust, Nate B.; Blecic, Jasmina; Britt, Christopher B. T.; Bowman, William C.] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA. [Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Anderson, David R.; Hellier, Coel; Maxted, Pierre F. L.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Collier-Cameron, Andrew] Univ St Andrews, Sch Phys & Astron, Haugh KY16 9SS, Fife, Scotland. [Wheatley, Peter J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Loredo, Thomas J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hebb, Leslie] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Pollaco, Don] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [West, Richard G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Campo, CJ (reprint author), Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA. EM ccampo@knights.ucf.edu RI Harrington, Joseph/E-6250-2011; Ragozzine, Darin/C-4926-2013; OI Blecic, Jasmina/0000-0002-0769-9614; Stevenson, Kevin/0000-0002-7352-7941; Cameron, Andrew/0000-0002-8863-7828; Hardy, Ryan/0000-0002-3849-9551; Harrington, Joseph/0000-0002-8955-8531; Wheatley, Peter/0000-0003-1452-2240 FU NASA; NASA through JPL/Caltech FX We thank the observers listed in Table 2 for allowing us to use their results and the organizers of the Exoplanet Transit Database for coordinating the collection and uniform analysis of these data. The IRAC data are based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The point of M. Ingemyr is based on observations made with the Nordic Optical Telescope (NOT), operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos Instituto Astrofisica de Canarias, and ALFOSC, which is owned by the Instituto Astrofisica de Andalucia (IAA) and operated at the NOT under agreement between IAA and NBlfAFG of the Astronomical Observatory of Copenhagen. We thank contributors to SciPy, Matplotlib, and the Python Programming Language, W. Landsman and other contributors to the Interactive Data Language Astronomy Library, the free- and open-source community, the NASA Astrophysics Data System, and the JPL Solar System Dynamics group for free software and services. NR 40 TC 65 Z9 65 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2011 VL 727 IS 2 AR 125 DI 10.1088/0004-637X/727/2/125 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000064 ER PT J AU Hughes, AM Wilner, DJ Andrews, SM Qi, CH Hogerheijde, MR AF Hughes, A. Meredith Wilner, David J. Andrews, Sean M. Qi, Chunhua Hogerheijde, Michiel R. TI EMPIRICAL CONSTRAINTS ON TURBULENCE IN PROTOPLANETARY ACCRETION DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (HD 163296, TW Hydrae) ID T-TAURI DISKS; GLOBAL MHD SIMULATIONS; YOUNG STELLAR OBJECTS; HERBIG AE/BE STARS; CIRCUMSTELLAR DISKS; X-RAY; MAGNETOROTATIONAL INSTABILITY; SUBMILLIMETER ARRAY; HYDRAE ASSOCIATION; VERTICAL STRUCTURE AB We present arcsecond-scale Submillimeter Array observations of the CO(3-2) line emission from the disks around the young stars HD 163296 and TW Hya at a spectral resolution of 44 m s(-1). These observations probe below the similar to 100 m s(-1) turbulent linewidth inferred from lower-resolution observations, and allow us to place constraints on the turbulent linewidth in the disk atmospheres. We reproduce the observed CO(3-2) emission using two physical models of disk structure: (1) a power-law temperature distribution with a tapered density distribution following a simple functional form for an evolving accretion disk, and (2) the radiative transfer models developed by D'Alessio et al. that can reproduce the dust emission probed by the spectral energy distribution. Both types of models yield a low upper limit on the turbulent linewidth (Doppler b-parameter) in the TW Hya system (less than or similar to 40 m s(-1)) and a tentative (3 sigma) detection of a similar to 300 m s(-1) turbulent linewidth in the upper layers of the HD 163296 disk. These correspond to roughly <= 10% and 40% of the sound speed at size scales commensurate with the resolution of the data. The derived linewidths imply a turbulent viscosity coefficient, alpha, of order 0.01 and provide observational support for theoretical predictions of subsonic turbulence in protoplanetary accretion disks. C1 [Hughes, A. Meredith; Wilner, David J.; Andrews, Sean M.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Hughes, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhughes@cfa.harvard.edu; dwilner@cfa.harvard.edu; sandrews@cfa.harvard.edu; cqi@cfa.harvard.edu; michiel@strw.leidenuniv.nl FU NASA [NAG5-11777]; National Science Foundation FX The authors thank Shin-Yi Lin for collaboration on collection of the extended TW Hya observations. We also thank Ramesh Narayan for helpful conversations about comparing the data with theoretical simulations, as well as Shane Davis for providing several quantities that were not tabulated in his paper. Partial support for this work was provided by NASA Origins of Solar Systems Program Grant NAG5-11777. A.M.H. acknowledges support from a National Science Foundation Graduate Research Fellowship. NR 72 TC 81 Z9 81 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 FEB 1 PY 2011 VL 727 IS 2 AR 85 DI 10.1088/0004-637X/727/2/85 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000024 ER PT J AU Kirk, H Myers, PC AF Kirk, Helen Myers, Philip C. TI YOUNG STELLAR GROUPS AND THEIR MOST MASSIVE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; stars: formation ID ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; FORMING REGION; MOLECULAR CLOUDS; DISK POPULATION; SPATIAL-DISTRIBUTION; EVOLUTIONARY MODELS; INFRARED EXTINCTION; STRUCTURAL-ANALYSIS; SPITZER SURVEY AB We analyze the masses and spatial distributions of 14 young stellar groups in Taurus, Lupus3, ChaI, and IC348. These nearby groups, which typically contain 20-40 members, have membership catalogs complete to similar to 0.02 M-circle dot, and are sufficiently young that their locations should be similar to where they formed. These groups show five properties seen in clusters having many more stars and much greater surface density of stars: (1) a broad range of masses, (2) a concentration of the most massive star toward the center of the group, (3) an association of the most massive star with a high surface density of lower mass stars, (4) a correlation of the mass of the most massive star with the total mass of the group, and (5) the distribution of a large fraction of the mass in a small fraction of the stars. C1 [Kirk, Helen; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, Cambridge, MA 02138 USA. RP Kirk, H (reprint author), Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, MS 42, Cambridge, MA 02138 USA. EM hkirk@cfa.harvard.edu FU Natural Sciences and Engineering Research Council of Canada; Smithsonian Astrophysical Observatory FX The authors thank Kevin Luhman for providing us with his YSO catalogs, as well as fielding numerous questions throughout this work, and Luisa Rebull for sending us a copy of her Taurus catalog and paper before publication and answering several queries. We also thank Francesco Palla and Steve Stahler for providing their stellar isochrone data, Eric Feigelson for alerting us to alternative cluster-identification techniques, and providing us with a copy of the chapter from his upcoming astro statistics text on this topic, and Paula Teixeira for sending us her Lupus3 extinction data. We are grateful for illuminating discussions with many people including Alyssa Goodman, Rob Gutermuth, Eric Mamajek, Tom Megeath, Manon Michel, Gus Muench, and Tom Robitaille, and thank the referee for a thoughtful report which improved this paper. H.K. is supported by a Natural Sciences and Engineering Research Council of Canada Postdoctoral Fellowship, with additional support from the Smithsonian Astrophysical Observatory. NR 75 TC 51 Z9 51 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2011 VL 727 IS 2 AR 64 DI 10.1088/0004-637X/727/2/64 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000003 ER PT J AU Osborne, JP Page, KL Beardmore, AP Bode, MF Goad, MR O'Brien, TJ Starrfield, S Rauch, T Ness, JU Krautter, J Schwarz, G Burrows, DN Gehrels, N Drake, JJ Evans, A Eyres, SPS AF Osborne, J. P. Page, K. L. Beardmore, A. P. Bode, M. F. Goad, M. R. O'Brien, T. J. Starrfield, S. Rauch, T. Ness, J. -U. Krautter, J. Schwarz, G. Burrows, D. N. Gehrels, N. Drake, J. J. Evans, A. Eyres, S. P. S. TI THE SUPERSOFT X-RAY PHASE OF NOVA RS OPHIUCHI 2006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: symbiotic; novae, cataclysmic variables; stars: oscillations; X-rays: individual (RS Oph) ID SWIFT OBSERVATIONS; LIGHT-CURVE; BLAST WAVE; INTERFEROMETRIC OBSERVATIONS; CATACLYSMIC VARIABLES; INFRARED OBSERVATIONS; SPECTRAL EVOLUTION; MODEL ATMOSPHERES; RECURRENT NOVAE; CLASSICAL NOVAE AB Swift X-ray observations of the similar to 60 day supersoft phase of the recurrent nova RS Ophiuchi (RS Oph) 2006 show the progress of nuclear burning on the white dwarf (WD) in exquisite detail. First seen 26 days after the optical outburst, this phase started with extreme variability likely due to variable absorption, although intrinsic WD variations are not excluded. About 32 days later, a steady decline in count rate set in. NLTE model atmosphere spectral fits during the supersoft phase show that the effective temperature of the WD increases from similar to 65 eV to similar to 90 eV during the extreme variability phase, falling slowly after about day 60 and more rapidly after day 80. The bolometric luminosity is seen to be approximately constant and close to Eddington from day 45 up to day 60, the subsequent decline possibly signaling the end of extensive nuclear burning. Before the decline, a multiply-periodic similar to 35 s modulation of the soft X-rays was present and may be the signature of a nuclear fusion driven instability. Our measurements are consistent with a WD mass near the Chandrasekhar limit; combined with a deduced accumulation of mass transferred from its binary companion, this leads us to suggest that RS Oph is a strong candidate for a future supernova explosion. The main uncertainty now is whether the WD is the CO type necessary for a Type Ia supernova. This may be confirmed by detailed abundance analyses of spectroscopic data from the outbursts. C1 [Osborne, J. P.; Page, K. L.; Beardmore, A. P.; Goad, M. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [O'Brien, T. J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Ness, J. -U.] ESAC, XMM Newton Sci Operat Ctr, Madrid 28691, Spain. [Krautter, J.] Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. [Schwarz, G.] Amer Astron Soc, Washington, DC 20009 USA. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Drake, J. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Evans, A.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Eyres, S. P. S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. RP Osborne, JP (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM julo@star.le.ac.uk RI Gehrels, Neil/D-2971-2012 FU STFC; NSF; NASA; German Aerospace Center (DLR) [05 OR 0806] FX We thank the Swift Science Team and the Swift Mission Operations Team for their excellent support of this observing campaign. J.O., K. P., M. G., A. B., and M. F. B. acknowledge the support of STFC. S. S. acknowledges partial support to ASU from NSF and NASA. T. R. is supported by the German Aerospace Center (DLR) under grant 05 OR 0806. The authors are grateful to John Nousek for his helpful comments on an initial draft of this paper and to Simon Vaughan for providing the TCL "shakefit" procedure. NR 79 TC 55 Z9 55 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2011 VL 727 IS 2 AR 124 DI 10.1088/0004-637X/727/2/124 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000063 ER PT J AU Trac, H Bode, P Ostriker, JP AF Trac, Hy Bode, Paul Ostriker, Jeremiah P. TI TEMPLATES FOR THE SUNYAEV-ZEL'DOVICH ANGULAR POWER SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: theory; galaxies: clusters: general; intergalactic medium; large-scale structure of universe; methods: numerical ID SOUTH-POLE TELESCOPE; X-RAY; GALAXY CLUSTERS; XMM-NEWTON; HYDRODYNAMICAL SIMULATIONS; RELATIVISTIC CORRECTIONS; PATCHY REIONIZATION; NONTHERMAL PRESSURE; INTRACLUSTER MEDIUM; BACKGROUND LIGHT AB We present templates for the Sunyaev-Zel'dovich (SZ) angular power spectrum based on four models for the nonlinear gas distribution. The frequency-dependent SZ temperature fluctuations, with thermal (TSZ) and kinetic (KSZ) contributions, are calculated by tracing through a dark matter simulation, processed to include gas in dark matter halos and in the filamentary intergalactic medium. Different halo gas models are compared to study how star formation, energetic feedback, and nonthermal pressure support influence the angular power spectrum. The standard model has been calibrated to reproduce the stellar and gas fractions and X-ray scaling relations measured from low-redshift clusters and groups. The other models illustrate the current theoretical and empirical uncertainties relating to properties of the intracluster medium. Relative to the standard model, their angular power spectra differ by approximately +/- 50% (TSZ), +/- 20% (KSZ), and +/- 40% (SZ at 148 GHz) for l = 3000, sigma(8) = 0.8, and homogeneous reionization at z = 10. The angular power spectrum decreases in amplitude as gas mass and binding energy are removed through star formation, and as gas is pushed out to larger radii by energetic feedback. With nonthermal pressure support, less pressure is required to maintain hydrostatic equilibrium, thus reducing the thermal contribution to the SZ power. We also calculate the SZ templates as a function of s8 and quantify this dependence. Assuming C-l proportional to (sigma(8)/0.8)(alpha), the effective scaling index ranges from 7 less than or similar to alpha(TSZ) less than or similar to 9, 4.5 less than or similar to alpha(KSZ) less than or similar to 5.5, and 6.5 less than or similar to alpha(SZ)(148 GHz) less than or similar to 8 at l = 3000 for 0.6 < sigma(8) < 1. The template spectra are publicly available and can be used when fitting for the SZ contribution to the cosmic microwave background on arcminute scales. C1 [Trac, Hy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Bode, Paul; Ostriker, Jeremiah P.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Trac, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Trac, Hy/N-8838-2014 OI Trac, Hy/0000-0001-6778-3861 FU Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics; NSF [0707731]; NASA through the Advanced Supercomputing Division at Ames Research Center; NSF through Pittsburgh Supercomputing Center; National Center for Supercomputing Applications [AST070021N]; TIGRESS high performance computer center at Princeton University,; Princeton Institute for Computational Science and Engineering; Princeton University Office of Information Technology FX We thank Nick Battaglia, Eric Hallman, Naoki Itoh, Eiichiro Komatsu, Martin Lueker, Kavi Moodley, Neelima Sehgal, David Spergel, and Ryan Warne for helpful discussions. We thank Sudeep Das and Toby Marriage for use of their Flipper code to make flat-sky maps. H. T. is supported by an Institute for Theory and Computation Fellowship at the Harvard-Smithsonian Center for Astrophysics. P. B. is supported by NSF grant 0707731. Computer simulations and analysis were supported by the NASA High-End Computing Program through the Advanced Supercomputing Division at Ames Research Center, the NSF through TeraGrid resources provided by Pittsburgh Supercomputing Center and the National Center for Supercomputing Applications under grant AST070021N, and the TIGRESS high performance computer center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering and the Princeton University Office of Information Technology. NR 78 TC 66 Z9 66 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2011 VL 727 IS 2 AR 94 DI 10.1088/0004-637X/727/2/94 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712JE UT WOS:000286662000033 ER PT J AU Fish, VL Doeleman, SS Beaudoin, C Blundell, R Bolin, DE Bower, GC Chamberlin, R Freund, R Friberg, P Gurwell, MA Honma, M Inoue, M Krichbaum, TP Lamb, J Marrone, DP Moran, JM Oyama, T Plambeck, R Primiani, R Rogers, AEE Smythe, DL SooHoo, J Strittmatter, P Tilanus, RPJ Titus, M Weintroub, J Wright, M Woody, D Young, KH Ziurys, LM AF Fish, Vincent L. Doeleman, Sheperd S. Beaudoin, Christopher Blundell, Ray Bolin, David E. Bower, Geoffrey C. Chamberlin, Richard Freund, Robert Friberg, Per Gurwell, Mark A. Honma, Mareki Inoue, Makoto Krichbaum, Thomas P. Lamb, James Marrone, Daniel P. Moran, James M. Oyama, Tomoaki Plambeck, Richard Primiani, Rurik Rogers, Alan E. E. Smythe, Daniel L. SooHoo, Jason Strittmatter, Peter Tilanus, Remo P. J. Titus, Michael Weintroub, Jonathan Wright, Melvyn Woody, David Young, Ken H. Ziurys, Lucy M. TI 1.3 mm WAVELENGTH VLBI OF SAGITTARIUS A*: DETECTION OF TIME-VARIABLE EMISSION ON EVENT HORIZON SCALES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; submillimeter: general; techniques: high angular resolution; techniques: interferometric ID SUPERMASSIVE BLACK-HOLE; SGR-A; GALACTIC-CENTER; FLARE EMISSION; X-RAY; MILLIMETER VLBI; ACCRETION FLOW; STELLAR ORBITS; MILKY-WAY; SIMULATIONS AB Sagittarius A*, the similar to 4 x 10(6) M(circle dot) black hole candidate at the Galactic center, can be studied on Schwarzschild radius scales with (sub) millimeter wavelength very long baseline interferometry (VLBI). We report on 1.3 mm wavelength observations of Sgr A* using a VLBI array consisting of the JCMT on Mauna Kea, the Arizona Radio Observatory's Submillimeter Telescope on Mt. Graham in Arizona, and two telescopes of the CARMA array at Cedar Flat in California. Both Sgr A* and the quasar calibrator 1924-292 were observed over three consecutive nights, and both sources were clearly detected on all baselines. For the first time, we are able to extract 1.3 mm VLBI interferometer phase information on Sgr A* through measurement of closure phase on the triangle of baselines. On the third night of observing, the correlated flux density of Sgr A* on all VLBI baselines increased relative to the first two nights, providing strong evidence for time-variable change on scales of a few Schwarzschild radii. These results suggest that future VLBI observations with greater sensitivity and additional baselines will play a valuable role in determining the structure of emission near the event horizon of Sgr A*. C1 [Fish, Vincent L.; Doeleman, Sheperd S.; Beaudoin, Christopher; Bolin, David E.; Rogers, Alan E. E.; Smythe, Daniel L.; SooHoo, Jason; Titus, Michael] MIT, Haystack Observ, Westford, MA 01886 USA. [Blundell, Ray; Gurwell, Mark A.; Moran, James M.; Primiani, Rurik; Weintroub, Jonathan; Young, Ken H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Freund, Robert; Strittmatter, Peter; Ziurys, Lucy M.] Univ Arizona, Steward Observ, Arizona Radio Observ, Tucson, AZ 85721 USA. [Bower, Geoffrey C.; Plambeck, Richard; Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Dept Astron, Berkeley, CA 94720 USA. [Chamberlin, Richard] Caltech Submillimeter Observ, Hilo, HI 96720 USA. [Friberg, Per; Tilanus, Remo P. J.] James Clerk Maxwell Telescope, Joint Astron Ctr, Hilo, HI 96720 USA. [Honma, Mareki; Oyama, Tomoaki] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Inoue, Makoto] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Krichbaum, Thomas P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Lamb, James; Woody, David] CALTECH, OVRO, Big Pine, CA 93513 USA. [Marrone, Daniel P.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Tilanus, Remo P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. RP Fish, VL (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM vfish@haystack.mit.edu OI Marrone, Daniel/0000-0002-2367-1080; Moran, James/0000-0002-3882-4414 FU National Science Foundation (NSF); NSF; Smithsonian Institution; Academia Sinica; CARMA; NSFATI program FX High-frequency VLBI work at MIT Haystack Observatory is supported by grants from the National Science Foundation (NSF). AROreceives partial support from the NSFATI program. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Funding for ongoing CARMA development and operations is supported by the NSF and the CARMA partner universities. D. E. B. acknowledges support from the NSF Research Experiences for Undergraduates program. NR 32 TC 68 Z9 67 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2011 VL 727 IS 2 AR L36 DI 10.1088/2041-8205/727/2/L36 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706DB UT WOS:000286196200009 ER PT J AU Reeves, KK Golub, L AF Reeves, Katharine K. Golub, Leon TI ATMOSPHERIC IMAGING ASSEMBLY OBSERVATIONS OF HOT FLARE PLASMA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares ID SUPRA-ARCADE DOWNFLOWS; SOLAR-FLARE; CONDUCTION; REGION; SUN AB We present observations of hot plasma from solar eruptions recorded by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory. AIA is the first narrowband instrument capable of taking images of hot plasma in the 5-15MK range. We find that there are hot structures above flare loops, and that they are typically more diffuse and nebulous than the well-defined flare loops. Because of the narrowband response, high sensitivity, and high spatial resolution of AIA, these supra-arcade structures are visible in exquisite detail, particularly in the 131 angstrom and 94 angstrom channels. In one event, a C4.9 flare observed on 2010 November 3, hot plasma is seen to outline an erupting plasmoid and possibly a current sheet. We compare hot plasma observed with AIA to structures observed with the X-Ray Telescope on the Hinode mission and find that the plasma imaged in AIA contains more fine detail. These new AIA observations show that supra-arcade flare structures and coronal mass ejections are highly structured not only in space and time, but also in temperature. This thermal structuring is expected, based on modeling efforts, but has now been imaged directly for the first time over a large range of temperatures. C1 [Reeves, Katharine K.; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM kreeves@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014; OI Golub, Leon/0000-0001-9638-3082 FU NSF-SHINE [ATM0752257]; Lockheed-Martin [SP02H1701R]; NASA [NNM07AB07C] FX The authors thank the anonymous referee, who provided useful comments that improved the Letter. K. K. R. is partially supported under the NSF-SHINE program, grant number ATM0752257. K. K. R. and L. G. are both supported under contract SP02H1701R from Lockheed-Martin to SAO and contract NNM07AB07C from NASA to SAO. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). NR 21 TC 51 Z9 51 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2011 VL 727 IS 2 AR L52 DI 10.1088/2041-8205/727/2/L52 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706DB UT WOS:000286196200025 ER PT J AU Sun, M Sehgal, N Voit, GM Donahue, M Jones, C Forman, W Vikhlinin, A Sarazin, C AF Sun, M. Sehgal, N. Voit, G. M. Donahue, M. Jones, C. Forman, W. Vikhlinin, A. Sarazin, C. TI THE PRESSURE PROFILES OF HOT GAS IN LOCAL GALAXY GROUPS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general; X-rays: galaxies: clusters ID ZELDOVICH POWER SPECTRUM; SOUTH-POLE TELESCOPE; XMM-NEWTON; INTRACLUSTER MEDIUM; CLUSTERS; CHANDRA; SAMPLE; MASS; THERMODYNAMICS; SIMULATIONS AB Recent measurements of the Sunyaev-Zel'dovich (SZ) angular power spectrum from the South Pole Telescope and the Atacama Cosmology Telescope demonstrate the importance of understanding baryon physics when using the SZ power spectrum to constrain cosmology. This is challenging since roughly half of the SZ power at l = 3000 is from low-mass systems with 10(13) h(-1) M-circle dot < M-500 < 1.5 x 10(14) h(-1) M-circle dot, which are more difficult to study than systems of higher mass. We present a study of the thermal pressure content for a sample of local galaxy groups from Sun et al. The group Y-sph,Y-500-M-500 relation agrees with the one for clusters derived by Arnaud et al. The group median pressure profile also agrees with the universal pressure profile for clusters derived by Arnaud et al. With this in mind, we briefly discuss several ways to alleviate the tension between the measured low SZ power and the predictions from SZ templates. C1 [Sun, M.; Sarazin, C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Sehgal, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Voit, G. M.; Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Jones, C.; Forman, W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. EM msun@virginia.edu RI Donahue, Megan/B-5361-2012; OI Voit, Gerard/0000-0002-3514-0383 FU Chandra [GO9-0135X, GO9-0148X]; XMM-Newton [NNX09AQ01G]; NASA LTSA [NNG-05GD82G]; U.S. Department of Energy [DE-AC3-76SF00515] FX We thank S. Allen, N. Battaglia, P. Bode, G. Holder, J. Hughes, D. Nagai, J. Ostriker, L. Shaw, J. Sievers, and H. Trac for helpful discussions. We thank N. Battaglia, L. Shaw, and H. Trac for providing their best fits of the Y-M relations. M. S. and C. S. were supported in part by Chandra grants GO9-0135X and GO9-0148X, and XMM-Newton grant NNX09AQ01G. M. S., G. M. V., and M. D. were supported in part by the NASA LTSA grant NNG-05GD82G. N. S. is supported by the U.S. Department of Energy contract to SLAC no. DE-AC3-76SF00515. NR 38 TC 34 Z9 34 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2011 VL 727 IS 2 AR L49 DI 10.1088/2041-8205/727/2/L49 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706DB UT WOS:000286196200022 ER PT J AU Wilner, DJ Andrews, SM Hughes, AM AF Wilner, David J. Andrews, Sean M. Hughes, A. Meredith TI MILLIMETER IMAGING OF THE beta PICTORIS DEBRIS DISK: EVIDENCE FOR A PLANETESIMAL BELT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; planetary systems; planet-disk interactions; stars: individual (beta Pictoris) ID DUST DISK; CORONAGRAPHIC OBSERVATIONS; VEGA; SYSTEM; IMAGES; ASYMMETRIES; PLANETS; MODELS; STARS; SIZE AB We present observations at 1.3 mm wavelength of the beta Pictoris debris disk with beam size 4."3 x 2."6 ( 83 x 50 AU) from the Submillimeter Array. The emission shows two peaks separated by similar to 7" along the disk plane, which we interpret as a highly inclined dust ring or belt. A simple model constrains the belt center to 94 +/- 8 AU, close to the prominent break in slope of the optical scattered light. We identify this region as the location of the main reservoir of dust-producing planetesimals in the disk. C1 [Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Miller Institute for Basic Research in Science FX We thank the SMA staff for scheduling and executing the two filler tracks that provided the data used in this Letter. We also thank Sally Heap and Don Linder for providing the Hubble Space Telescope/STIS coronographic image in FITS format. A.M.H. is supported by a fellowship from the Miller Institute for Basic Research in Science. NR 44 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2011 VL 727 IS 2 AR L42 DI 10.1088/2041-8205/727/2/L42 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706DB UT WOS:000286196200015 ER PT J AU Mannion, PD Upchurch, P Carrano, MT Barrett, PM AF Mannion, Philip D. Upchurch, Paul Carrano, Matthew T. Barrett, Paul M. TI Testing the effect of the rock record on diversity: a multidisciplinary approach to elucidating the generic richness of sauropodomorph dinosaurs through time SO BIOLOGICAL REVIEWS LA English DT Review DE dinosaurs; diversity; extinction; macroevolution; rarefaction; residuals; rock record; sampling bias; sauropodomorphs; sea level ID SEA-LEVEL CHANGE; TRILOBITE ALPHA-DIVERSITY; NON-AVIAN DINOSAURS; FOSSIL RECORD; MASS EXTINCTIONS; GLOBAL DIVERSITY; ENVIRONMENTAL ASSOCIATIONS; PHANEROZOIC BIODIVERSITY; MATRIX REPRESENTATION; QUANTITATIVE-ANALYSIS AB The accurate reconstruction of palaeobiodiversity patterns is central to a detailed understanding of the macroevolutionary history of a group of organisms. However, there is increasing evidence that diversity patterns observed directly from the fossil record are strongly influenced by fluctuations in the quality of our sampling of the rock record; thus, any patterns we see may reflect sampling biases, rather than genuine biological signals. Previous dinosaur diversity studies have suggested that fluctuations in sauropodomorph palaeobiodiversity reflect genuine biological signals, in comparison to theropods and ornithischians whose diversity seems to be largely controlled by the rock record. Most previous diversity analyses that have attempted to take into account the effects of sampling biases have used only a single method or proxy: here we use a number of techniques in order to elucidate diversity. A global database of all known sauropodomorph body fossil occurrences (2024) was constructed. A taxic diversity curve for all valid sauropodomorph genera was extracted from this database and compared statistically with several sampling proxies (rock outcrop area and dinosaur-bearing formations and collections), each of which captures a different aspect of fossil record sampling. Phylogenetic diversity estimates, residuals and sample-based rarefaction (including the first attempt to capture 'cryptic' diversity in dinosaurs) were implemented to investigate further the effects of sampling. After 'removal' of biases, sauropodomorph diversity appears to be genuinely high in the Norian, Pliensbachian-Toarcian, Bathonian-Callovian and Kimmeridgian-Tithonian (with a small peak in the Aptian), whereas low diversity levels are recorded for the Oxfordian and Berriasian-Barremian, with the Jurassic/Cretaceous boundary seemingly representing a real diversity trough. Observed diversity in the remaining Triassic-Jurassic stages appears to be largely driven by sampling effort. Late Cretaceous diversity is difficult to elucidate and it is possible that this interval remains relatively under-sampled. Despite its distortion by sampling biases, much of sauropodomorph palaeobiodiversity can be interpreted as a reflection of genuine biological signals, and fluctuations in sea level may account for some of these diversity patterns. C1 [Mannion, Philip D.; Upchurch, Paul] UCL, Dept Earth Sci, London WC1E 6BT, England. [Carrano, Matthew T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Barrett, Paul M.] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. RP Mannion, PD (reprint author), UCL, Dept Earth Sci, Gower St, London WC1E 6BT, England. EM p.mannion@ucl.ac.uk RI Mannion, Philip/B-3159-2011; Upchurch, Paul/C-1654-2008; Barrett, Paul/A-2648-2010; Carrano, Matthew/C-7601-2011 OI Barrett, Paul/0000-0003-0412-3000; Carrano, Matthew/0000-0003-2129-1612 FU University College London [NER/S/A/2006/14347]; Abbey International Collaborative Grant scheme; Royal Society FX We would like to express particular thanks to all those who allowed the study of dinosaur material in their care. Advice on statistical tests by Alistair J. McGowan is very much appreciated and reviews by David E. Fastovsky and Andrew B. Smith greatly improved this work. Jerald D. Harris is also thanked for assistance with references. P. D. M. is supported by a University College London NERC studentship (NER/S/A/2006/14347). P. U. wishes to thank The Palaeontological Association, The Abbey International Collaborative Grant scheme and The Royal Society for funds that have enabled travel to examine sauropodomorph specimens. NR 178 TC 99 Z9 100 U1 1 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD FEB PY 2011 VL 86 IS 1 BP 157 EP 181 DI 10.1111/j.1469-185X.2010.00139.x PG 25 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 709WZ UT WOS:000286473400007 PM 20412186 ER PT J AU Schnitzer, SA Klironomos, JN HilleRisLambers, J Kinkel, LL Reich, PB Xiao, K Rillig, MC Sikes, BA Callaway, RM Mangan, SA van Nes, EH Scheffer, M AF Schnitzer, Stefan A. Klironomos, John N. HilleRisLambers, Janneke Kinkel, Linda L. Reich, Peter B. Xiao, Kun Rillig, Matthias C. Sikes, Benjamin A. Callaway, Ragan M. Mangan, Scott A. van Nes, Egbert H. Scheffer, Marten TI Soil microbes drive the classic plant diversity-productivity pattern SO ECOLOGY LA English DT Article DE AMF; density dependence; diversity-productivity; negative feedback; pathogens; soil microbes; species richness ID ARBUSCULAR MYCORRHIZAE; NITROGEN DEPOSITION; SPECIES-DIVERSITY; ELEVATED CO2; BIODIVERSITY; FEEDBACK; DISEASE; ECOSYSTEMS; COMMUNITIES; PATHOGENS AB Ecosystem productivity commonly increases asymptotically with plant species diversity, and determining the mechanisms responsible for this well-known pattern is essential to predict potential changes in ecosystem productivity with ongoing species loss. Previous studies attributed the asymptotic diversity-productivity pattern to plant competition and differential resource use (e.g., niche complementarity). Using an analytical model and a series of experiments, we demonstrate theoretically and empirically that host-specific soil microbes can be major determinants of the diversity-productivity relationship in grasslands. In the presence of soil microbes, plant disease decreased with increasing diversity, and productivity increased nearly 500%, primarily because of the strong effect of density-dependent disease on productivity at low diversity. Correspondingly, disease was higher in plants grown in conspecific-trained soils than heterospecific-trained soils (demonstrating host-specificity), and productivity increased and host-specific disease decreased with increasing community diversity, suggesting that disease was the primary cause of reduced productivity in species-poor treatments. In sterilized, microbe-free soils, the increase in productivity with increasing plant species number was markedly lower than the increase measured in the presence of soil microbes, suggesting that niche complementarity was a weaker determinant of the diversity-productivity relationship. Our results demonstrate that soil microbes play an integral role as determinants of the diversity-productivity relationship. C1 [Schnitzer, Stefan A.; Mangan, Scott A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.; Mangan, Scott A.] Smithsonian Trop Res Inst, Balboa 03092, Panama. [Klironomos, John N.] Univ British Columbia Okanagan, Biol & Phys Geog Unit, Kelowna, BC V1V 1V7, Canada. [HilleRisLambers, Janneke] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Kinkel, Linda L.; Xiao, Kun] Univ Minnesota, Dept Plant Pathol, St Paul, MN 55108 USA. [Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Rillig, Matthias C.] Free Univ Berlin, Inst Biol, D-14195 Berlin, Germany. [Sikes, Benjamin A.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78705 USA. [Callaway, Ragan M.] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. [Schnitzer, Stefan A.; van Nes, Egbert H.; Scheffer, Marten] Wageningen Univ, Wageningen, Netherlands. RP Schnitzer, SA (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA. EM Schnitzer@uwm.edu RI van Nes, Egbert/F-2681-2011; Scheffer, Marten/C-1852-2012; Rillig, Matthias/B-3675-2009; OI van Nes, Egbert/0000-0002-6345-104X; Rillig, Matthias/0000-0003-3541-7853; Schnitzer, Stefan/0000-0002-2715-9455; Sikes, Benjamin/0000-0003-0774-2624 FU DOE [DE-FG02-96ER62291]; NSF LTER [DEB-0080382]; NSF [DEB-0614406, 9977907]; Natural Sciences and Engineering Research Council of Canada; University of Wisconsin-Milwaukee Research Growth Initiative FX We thank L. Poorter and two anonymous reviewers for helpful comments on the manuscript. This work was supported by the DOE Program for Ecological Research DE-FG02-96ER62291, NSF LTER DEB-0080382, NSF DEB-0614406, NSF Microbial Observatories Grant 9977907, a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada, and the University of Wisconsin-Milwaukee Research Growth Initiative program. NR 34 TC 145 Z9 151 U1 29 U2 243 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD FEB PY 2011 VL 92 IS 2 BP 296 EP 303 DI 10.1890/10-0773.1 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 750NC UT WOS:000289553600005 PM 21618909 ER PT J AU Craddock, RA AF Craddock, Robert A. TI Are Phobos and Deimos the result of a giant impact? SO ICARUS LA English DT Article DE Mars; Mars, Satellites; Satellites, Formation; Impact processes ID MARTIAN CRUSTAL DICHOTOMY; CRATER DIMENSIONS; ORIGIN; MARS; MOON; HYPOTHESIS; ACCRETION; EVOLUTION; SATELLITES; BASINS AB Despite many efforts an adequate theory describing the origin of Phobos and Deimos has not been realized. In recent years a number of separate observations suggest the possibility that the martian satellites may have been the result of giant impact. Similar to the Earth-Moon system, Mars has too much angular momentum. A planetesimal with 0.02 Mars masses must have collided with that planet early in its history in order for Mars to spin at its current rate (Dones, L, Tremaine, S. [1993]. Science 259, 350-354). Although subject to considerable error, current crater-scaling laws and an analysis of the largest known impact basins on the martian surface suggest that this planetesimal could have formed either the proposed 10,600 by 8500-km-diameter Borealis basin, the 4970-km-diameter Elysium basin, the 4500-km-diameter Daedalia basin or, alternatively, some other basin that is no longer identifiable. It is also probable that this object impacted Mars at a velocity great enough to vaporize rock (>7 km/s), which is necessary to place large amounts of material into orbit. If material vaporized from the collision with the Mars-spinning planetesimal were placed into orbit, an accretion disk would have resulted. It is possible that as material condensed and dissipated beyond the Roche limit forming small, low-mass satellites due to gravity instabilities within the disk. Once the accretion disk dissipated, tidal forces and libration would have pulled these satellites back down toward the martian surface. In this scenario, Phobos and Deimos would have been among the first two satellites to form, and Deimos the only satellite formed-and preserved-beyond synchronous rotation. The low mass of Phobos and Deimos is explained by the possibility that they are composed of loosely aggregated material from the accretion disk, which also implies that they do not contain any volatile elements. Their orbital eccentricity and inclination, which are the most difficult parameters to explain easily with the various capture scenarios, are the natural result of accretion from a circum-planetary disk. Published by Elsevier Inc. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Craddock, RA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC-315, Washington, DC 20560 USA. EM craddockb@si.edu RI Craddock, Robert/B-3884-2013 NR 66 TC 22 Z9 22 U1 2 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 2011 VL 211 IS 2 BP 1150 EP 1161 DI 10.1016/j.icarus.2010.10.023 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 715TE UT WOS:000286909700017 ER PT J AU Leather, SR Didham, RK Basset, Y AF Leather, Simon R. Didham, Raphael K. Basset, Yves TI Insect Conservation and Diversity - making an impact SO INSECT CONSERVATION AND DIVERSITY LA English DT Editorial Material C1 [Leather, Simon R.] Univ London Imperial Coll Sci Technol & Med, Div Biol, Ascot SL5 7PY, Berks, England. [Didham, Raphael K.] Univ Western Australia, Sch Anim Biol, Crawley, WA 6009, Australia. [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. RP Leather, SR (reprint author), Univ London Imperial Coll Sci Technol & Med, Div Biol, Silwood Pk Campus, Ascot SL5 7PY, Berks, England. RI Didham, Raphael/B-5953-2011; Basset, Yves/B-6642-2014; OI Leather, Simon/0000-0003-3007-8514 NR 5 TC 0 Z9 0 U1 1 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1752-458X J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD FEB PY 2011 VL 4 IS 1 BP 1 EP 1 DI 10.1111/j.1752-4598.2010.00128.x PG 1 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 704KS UT WOS:000286052500001 ER PT J AU Gingerich, O AF Gingerich, Owen TI Astrum 2009. Astronomy and Instruments: Italian Heritage Four Hundred Years after Galileo SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 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 FEB PY 2011 VL 42 BP 116 EP 117 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 797DK UT WOS:000293104500011 ER PT J AU Adshead, P Easther, R Pritchard, J Loeb, A AF Adshead, Peter Easther, Richard Pritchard, Jonathan Loeb, Abraham TI Inflation and the scale dependent spectral index: prospects and strategies SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE inflation; cosmological parameters from LSS; cosmological parameters from CMBR ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; PROBE WMAP OBSERVATIONS; LY-ALPHA FOREST; POWER SPECTRUM; ACOUSTIC-OSCILLATIONS; PARAMETER-ESTIMATION; REDSHIFT SURVEYS; GALAXY SURVEYS; RE-IONIZATION; DARK ENERGY AB We consider the running of the spectral index as a probe of both inflation itself, and of the overall evolution of the very early universe. Surveying a collection of simple single field inflationary models, we confirm that the magnitude of the running is relatively consistent, unlike the tensor amplitude, which varies by orders of magnitude. Given this target, we confirm that the running is potentially detectable by future large scale structure or 21 cm observations, but that only the most futuristic measurements can distinguish between these models on the basis of their running. For any specified inflationary scenario, the combination of the running index and unknown post-inflationary expansion history induces a theoretical uncertainty in the predicted value of the spectral index. This effect can easily dominate the statistical uncertainty with which Planck and its successors are expected to measure the spectral index. More positively, upcoming cosmological experiments thus provide an intriguing probe of physics between TeV and GUT scales by constraining the reheating history associated with any specified inflationary model, opening a window into the "primordial dark age" that follows the end of inflation. C1 [Adshead, Peter; Easther, Richard] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Pritchard, Jonathan; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Adshead, P (reprint author), Yale Univ, Dept Phys, 217 Prospect St, New Haven, CT 06520 USA. EM adshead@kicp.uchicago.edu; richard.easther@yale.edu; jpritchard@cfa.harvard.edu; aloeb@cfa.harvard.edu OI Pritchard, Jonathan/0000-0003-4127-5353; Easther, Richard/0000-0002-7233-665X FU United States Department of Energy [DE-FG02-92ER-40704]; NSF [PHY-0747868, AST-0907890]; NASA, Space Telescope Science Institute [HST-HF-51234.01-A, NAS 5-26555]; NASA [NNX08AL43G, NNA09DB30A] FX PA and RE are supported in part by the United States Department of Energy, grant DE-FG02-92ER-40704. RE is supported by an NSF Career Award PHY-0747868. JRP is supported by NASA through Hubble Fellowship grant HST-HF-51234.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A for AL. RE and JRP thank the Aspen Center for Physics for hospitality during part of this work. We thank Will Kinney and Hiranya Peiris for a number of useful conversations. NR 89 TC 38 Z9 38 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD FEB PY 2011 IS 2 AR 021 DI 10.1088/1475-7516/2011/02/021 PG 33 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 728FK UT WOS:000287859800022 ER PT J AU Tocheri, MW Solhan, CR Orr, CM Femiani, J Frohlich, B Groves, CP Harcourt-Smith, WE Richmond, BG Shoelson, B Jungers, WL AF Tocheri, Matthew W. Solhan, Christyna R. Orr, Caley M. Femiani, John Frohlich, Bruno Groves, Colin P. Harcourt-Smith, William E. Richmond, Brian G. Shoelson, Brett Jungers, William L. TI Ecological divergence and medial cuneiform morphology in gorillas SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Hallux; Tarsals; Functional morphology; Laser scanning; CT scanning; 3D morphometrics ID SYMPATRIC LOWLAND GORILLAS; EVOLUTIONARY HISTORY; POSITIONAL BEHAVIOR; GENETIC DIVERSITY; LOPE RESERVE; GREAT APE; KAHUZI; SHAPE; SIZE; DISTRIBUTIONS AB Gorillas are more closely related to each other than to any other extant primate and are all terrestrial knuckle-walkers, but taxa differ along a gradient of dietary strategies and the frequency of arboreality in their behavioral repertoire. In this study, we test the hypothesis that medial cuneiform morphology falls on a morphocline in gorillas that tracks function related to hallucial abduction ability and relative frequency of arboreality. This morphocline predicts that western gorillas, being the most arboreal, should display a medial cuneiform anatomy that reflects the greatest hallucial abduction ability, followed by grauer gorillas, and then by mountain gorillas. Using a three-dimensional methodology to measure angles between articular surfaces, relative articular and nonarticular areas, and the curvatures of the hallucial articular surface, the functional predictions are partially confirmed in separating western gorillas from both eastern gorillas. Western gorillas are characterized by a more medially oriented, proportionately larger, and more mediolaterally curved hallucial facet than are eastern gorillas. These characteristics follow the predictions for a more prehensile hallux in western gorillas relative to a more stable, plantigrade hallux in eastern gorillas. The characteristics that distinguish eastern gorilla taxa from one another appear unrelated to hallucial abduction ability or frequency of arboreality. In total, this reexamination of medial cuneiform morphology suggests differentiation between eastern and western gorillas due to a longstanding ecological divergence and more recent and possibly non-adaptive differences between eastern taxa. Published by Elsevier Ltd. C1 [Tocheri, Matthew W.; Solhan, Christyna R.; Orr, Caley M.; Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20013 USA. [Solhan, Christyna R.; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Femiani, John] Arizona State Univ Polytech, Dept Engn, Mesa, AZ 85212 USA. [Groves, Colin P.] Australian Natl Univ, Sch Archaeol & Anthropol, Canberra, ACT 0200, Australia. [Harcourt-Smith, William E.] CUNY Herbert H Lehman Coll, Dept Anthropol, Bronx, NY 10468 USA. [Harcourt-Smith, William E.] Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. [Shoelson, Brett] MathWorks, Natick, MA 01760 USA. [Jungers, William L.] SUNY Stony Brook, Med Ctr, Dept Anat Sci, Stony Brook, NY 11794 USA. RP Tocheri, MW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM tocherim@si.edu OI Tocheri, Matthew/0000-0001-7600-8998 FU Wenner-Gren Foundation [7822] FX This research was supported by a Wenner-Gren Foundation post-PhD grant to MWT (Grant Number 7822). Curatorial assistance and access to museum collections provided by Dr. Richard Thorington and Linda Gordon (USNM), Dr. Emmanuel Gilissen and Wim Wendelen (RMCA), and Ned Gilmore (ANSP), is gratefully acknowledged. We also thank SIEMENS for generously donating to the USNM the Somatom Emotion CT scanner used in this work and three anonymous reviewers for their helpful and constructive criticisms of an earlier version of this manuscript. NR 92 TC 31 Z9 31 U1 2 U2 13 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 FEB PY 2011 VL 60 IS 2 BP 171 EP 184 DI 10.1016/j.jhevol.2010.09.002 PG 14 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 717UQ UT WOS:000287073300004 PM 21093014 ER PT J AU Jin, L Hinde, K Tao, L AF Jin, L. Hinde, K. Tao, L. TI Species diversity and relative abundance of lactic acid bacteria in the milk of rhesus monkeys (Macaca mulatta) SO JOURNAL OF MEDICAL PRIMATOLOGY LA English DT Article DE 16S rRNA; breastfeeding; commensal bacteria; Lactobacillus reuteri; milk microbiota; Streptococcus gallolyticus ID BREAST-MILK; LACTOBACILLUS-REUTERI; STREPTOCOCCUS-BOVIS; HEALTHY WOMEN; GENOME SEQUENCE; INFANT GUT; LACTATION; MACAQUES; STRAIN; GENE AB Background Mother's milk is a source of bacteria that influences the development of the infant commensal gut microbiota. To date, the species diversity and relative abundance of lactic acid bacteria in the milk of non-human primates have not been described. Methods Milk samples were aseptically obtained from 54 female rhesus monkeys (Macaca mulatta) at peak lactation. Following GM17 and MRS agar plating, single bacterial colonies were isolated based on difference in morphotypes, then grouped based on whole-cell protein profiles on SDS-PAGE. Bacterial DNA was isolated and the sequence the 16S rRNA gene was analyzed. Results A total of 106 strains of 19 distinct bacterial species, belonging to five genera, Bacillus, Enterococcus, Lactobacillus, Pediococcus, and Streptococcus, were identified. Conclusions Maternal gut and oral commensal bacteria may be translocated to the mammary gland during lactation and present in milk. This pathway can be an important source of commensal bacteria to the infant gut and oral cavity. C1 [Hinde, K.] Univ Calif Davis, Brain Mind & Behav Unit, Calif Natl Primate Res Ctr, Davis, CA 95616 USA. [Jin, L.; Tao, L.] Univ Illinois, Coll Dent, Dept Oral Biol, Chicago, IL USA. [Hinde, K.] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. RP Hinde, K (reprint author), Univ Calif Davis, Brain Mind & Behav Unit, Calif Natl Primate Res Ctr, 1 Shields Ave, Davis, CA 95616 USA. EM kjhinde@ucdavis.edu; ltao@uic.edu FU NIH [AI066709, RR000169, RR019970]; NSF [BCS-0921978, BCS-0525025] FX This work was supported in part by NIH grants AI066709, RR000169, RR019970, and NSF grants BCS-0921978 and BCS-0525025. NR 43 TC 8 Z9 8 U1 0 U2 10 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0047-2565 J9 J MED PRIMATOL JI J. Med. Primatol. PD FEB PY 2011 VL 40 IS 1 BP 52 EP 58 DI 10.1111/j.1600-0684.2010.00450.x PG 7 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 702VQ UT WOS:000285924400008 PM 20946146 ER PT J AU Lambert, TD Halsey, MK Dittel, JW Mangan, SA Delfosse, E Adler, GH Schnitzer, SA AF Lambert, Thomas D. Halsey, Michaela K. Dittel, Jacob W. Mangan, Scott A. Delfosse, Erika Adler, Gregory H. Schnitzer, Stefan A. TI First record of Alston's Woolly Mouse Opossum (Micoureus alstoni) from the canal area of Central Panama SO MAMMALIA LA English DT Editorial Material DE Barro Colorado Nature Monument; Central America; Didelphimorphia; Panama; range extension ID PROECHIMYS SEMISPINOSUS; RODENTS; MARSUPIALS; ABUNDANCE; ISLANDS C1 [Lambert, Thomas D.; Halsey, Michaela K.] Frostburg State Univ, Dept Biol, Frostburg, MD 21532 USA. [Dittel, Jacob W.; Delfosse, Erika; Adler, Gregory H.] Univ Wisconsin, Dept Biol & Microbiol, Oshkosh, WI 54901 USA. [Mangan, Scott A.; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Lambert, TD (reprint author), Frostburg State Univ, Dept Biol, Frostburg, MD 21532 USA. EM tdlambert@frostburg.edu OI Schnitzer, Stefan/0000-0002-2715-9455 NR 14 TC 0 Z9 0 U1 1 U2 1 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0025-1461 J9 MAMMALIA JI Mammalia PD FEB PY 2011 VL 75 IS 1 BP 107 EP 109 DI 10.1515/MAMM.2010.076 PG 3 WC Zoology SC Zoology GA 780TO UT WOS:000291882300017 ER PT J AU Sarty, GE Szalai, A Kiss, LL Matthews, JM Wu, K Kuschnig, R Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW Huziak, R Johnston, HM Phillips, A Ashley, MCB AF Sarty, Gordon E. Szalai, Tamas Kiss, Laszlo L. Matthews, Jaymie M. Wu, Kinwah Kuschnig, Rainer Guenther, David B. Moffat, Anthony F. J. Rucinski, Slavek M. Sasselov, Dimitar Weiss, Werner W. Huziak, Richard Johnston, Helen M. Phillips, Andre Ashley, Michael C. B. TI The gamma-ray binary LS 5039: mass and orbit constraints from MOST observations star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: binaries: close; circumstellar matter; stars: individual: LS 5039 ID MICROQUASAR LS-5039; STELLAR PARAMETERS; MAGELLANIC CLOUDS; 4TH EDITION; BLACK-HOLE; EMISSION; DISCOVERY; GALAXY; WIND; MODULATION AB The results of a coordinated space-based photometric and ground-based spectroscopic observing campaign on the enigmatic gamma-ray binary LS 5039 are reported. 16 d of observations from the MOST satellite have been combined with high-resolution optical echelle spectroscopy from the 2.3-m ANU Telescope in Siding Spring, Australia. These observat ions were used to measure the orbital parameters of the binary and to study the properties of stellar wind from the O primary. We found that any broad-band optical photometric variability at the orbital period is below the 2 mmag level, supporting the scenario that the orbital eccentricity of the system is near the 0.24 +/- 0.08 value implied by our spectroscopy, which is lower than values previously obtained by other workers. The low amplitude optical variability also implies the component masses are at the higher end of estimates based on the primary's O6.5V((f)) spectral type with a primary mass of similar to 26 M-circle dot and a mass for the compact star of at least 1.8 M-circle dot. The mass-loss rate from the O primary was determined to be 3.7 to 4.8 x 10-7 M-circle dot yr-1. C1 [Sarty, Gordon E.; Huziak, Richard] RPO Univ, Saskatoon Ctr, Royal Astron Soc Canada, Saskatoon, SK S7N 4J8, Canada. [Sarty, Gordon E.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK S7N 5E2, Canada. [Szalai, Tamas] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Kiss, Laszlo L.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Kiss, Laszlo L.; Wu, Kinwah; Johnston, Helen M.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Matthews, Jaymie M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Wu, Kinwah] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, David B.] St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Observ Astron Mt Megant, Montreal, PQ H3C 3J7, Canada. [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Phillips, Andre; Ashley, Michael C. B.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. RP Sarty, GE (reprint author), RPO Univ, Saskatoon Ctr, Royal Astron Soc Canada, POB 317, Saskatoon, SK S7N 4J8, Canada. EM gordon.sarty@usask.ca OI Sarty, Gordon/0000-0001-5516-7869 FU Australian Research Council; University of Sydney; Hungarian OTKA [K76816, MB0C 81013]; Hungarian Academy of Sciences FX This work has been supported by the Australian Research Council, the University of Sydney, the Hungarian OTKA Grants K76816 and MB0C 81013, and the 'Lendulet' Young Researchers' Programme of the Hungarian Academy of Sciences. KW's visits to Sydney University were supported by the University of Sydney International Visiting Fellowship. NR 52 TC 26 Z9 26 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 411 IS 2 BP 1293 EP 1300 DI 10.1111/j.1365-2966.2010.17757.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716QO UT WOS:000286988800044 ER PT J AU Nicholas, B Rowell, G Burton, MG Walsh, A Fukui, Y Kawamura, A Longmore, S Keto, E AF Nicholas, B. Rowell, G. Burton, M. G. Walsh, A. Fukui, Y. Kawamura, A. Longmore, S. Keto, E. TI 12 mm line survey of the dense molecular gas towards the W28 field TeV gamma-ray sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE molecular data; supernovae: individual: W28; ISM: clouds; cosmic rays; H ii regions; gamma rays: ISM; radio lines: ISM ID SUPERNOVA REMNANT W28; H-II REGIONS; ULTRACOMPACT HII-REGIONS; STAR-FORMING REGIONS; RADIO-CONTINUUM; EXTENDED ENVELOPES; RADIATIVE-TRANSFER; INFRARED-EMISSION; MASSIVE OUTFLOW; GALACTIC-CENTER AB We present 12 mm Mopra observations of dense molecular gas towards the W28 supernova remnant (SNR) field. The focus is on the dense molecular gas towards the TeV gamma-ray sources detected by the HESS telescopes, which likely trace the cosmic rays from W28 and possibly other sources in the region. Using the NH3 inversion transitions we reveal several dense cores inside the molecular clouds, the majority of which coincide with high-mass star formation and H ii regions, including the energetic ultracompact H ii region G5.89-0.39. A key exception to this is the cloud north-east of W28, which is well known to be disrupted as evidenced by clusters of 1720 MHz OH masers and broad CO line emission. Here we detect broad NH3, up to the (9,9) transition, with linewidths up to 16 km s-1. This broad NH3 emission spatially matches well with the TeV source HESS J1801-233 and CO emission, and its velocity dispersion distribution suggests external disruption from the W28 SNR direction. Other lines are detected, such as HC3N and HC5N, H2O masers, and many radio recombination lines, all of which are primarily found towards the southern high-mass star formation regions. These observations provide a new view on to the internal structures and dynamics of the dense molecular gas towards the W28 SNR field and, in tandem with future higher-resolution TeV gamma-ray observations, will offer the chance to probe the transport of cosmic rays into molecular clouds. C1 [Nicholas, B.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Burton, M. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Walsh, A.] James Cook Univ, Sch Engn & Phys Sci, Ctr Astron, Townsville, Qld 4811, Australia. [Fukui, Y.; Kawamura, A.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Keto, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nicholas, B (reprint author), Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. EM brent.nicholas@adelaide.edu.au RI Walsh, Andrew/B-5627-2013; OI Walsh, Andrew/0000-0001-9506-0855; Burton, Michael/0000-0001-7289-1998; Rowell, Gavin/0000-0002-9516-1581 FU Australian Research Council [DP0662810]; Commonwealth of Australia; University of Sydney; Monash University; CSIRO; University of New South Wales FX BN would like to thank Nigel Maxted for useful discussions and the referee for comments which improved the quality of this work. This work was supported by an Australian Research Council grant (DP0662810). The Mopra Telescope is part of the Australia Telescope and is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The University of New South Wales Mopra Spectrometer Digital Filter Bank used for these Mopra observations was provided with support from the Australian Research Council, together with the University of New South Wales, University of Sydney, Monash University and the CSIRO. NR 80 TC 14 Z9 14 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 411 IS 2 BP 1367 EP 1385 DI 10.1111/j.1365-2966.2010.17778.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716QO UT WOS:000286988800050 ER PT J AU Davies, B Bastian, N Gieles, M Seth, AC Mengel, S Konstantopoulos, IS AF Davies, Ben Bastian, Nate Gieles, Mark Seth, Anil C. Mengel, Sabine Konstantopoulos, Iraklis S. TI GLIMPSE-CO1: the most massive intermediate-age stellar cluster in the Galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; globular clusters: individual: GLIMPSE-C01 ID LARGE-MAGELLANIC-CLOUD; STAR-FORMATION HISTORY; GLOBULAR-CLUSTERS; RED SUPERGIANTS; MILKY-WAY; IDENTIFICATION; WESTERLUND-1; METALLICITY; POPULATIONS; DISRUPTION AB The stellar cluster GLIMPSE-C01 is a dense stellar system located in the Galactic plane. Though often referred to in the literature as an old globular cluster traversing the Galactic disc, previous observations do not rule out that it is an intermediate-age (less than a few Gyr) disc-borne cluster. Here, we present high-resolution near-infrared spectroscopy of over 50 stars in the cluster. We find an average radial velocity is consistent with being part of the disc, and determine the cluster's dynamical mass to be (8 +/- 3) x 104 M-circle dot. Analysis of the cluster's M/L ratio, the location of the red clump and an extremely high stellar density, all suggest an age of 400-800 Myr for GLIMPSE-C01, much lower than that for a typical globular cluster. This evidence therefore leads us to conclude that GLIMPSE-C01 is a part of the disc population, and is the most massive Galactic intermediate-age cluster discovered to date. C1 [Davies, Ben] Rochester Inst Technol, Rochester, NY 14623 USA. [Davies, Ben] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Bastian, Nate] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Bastian, Nate; Gieles, Mark] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mengel, Sabine] European So Observ, D-85748 Garching, Germany. [Konstantopoulos, Iraklis S.] Penn State Univ, Eberly Coll Sci, University Pk, PA 16802 USA. RP Davies, B (reprint author), Rochester Inst Technol, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM b.davies@leeds.ac.uk RI Davies, Ben/K-3996-2012; OI Konstantopoulos, Iraklis/0000-0003-2177-0146; Gieles, Mark/0000-0002-9716-1868; Davies, Ben/0000-0002-2010-2122 FU National Aeronautics and Space Administration; National Science Foundation FX We thank the referee Valentin Ivanov for his comments and suggestions which helped us improve the paper, and for kindly supplying us with the photometry of GLIMPSE-C01. We also thank Don Figer for useful discussions. The data in this paper were obtained through ESO under the observing programme 383. D-0025. This work makes use of the UKIDSS survey; the UKIDSS project is defined in Lawrence et al. (2007). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Casali et al. 2007) and a photometric system described in Hewett et al. (2006). The pipeline processing and science archive are described in Hambly et al. (2008). This paper makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 40 TC 18 Z9 18 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 411 IS 2 BP 1386 EP 1394 DI 10.1111/j.1365-2966.2010.17777.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716QO UT WOS:000286988800051 ER PT J AU Brown, WR Kilic, M Prieto, CA Kenyon, SJ AF Brown, Warren R. Kilic, Mukremin Allende Prieto, Carlos Kenyon, Scott J. TI The merger rate of extremely low mass white dwarf binaries: links to the formation of AM CVn stars and underluminous supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; white dwarfs; Galaxy: stellar content ID MILKY-WAY; HYPERVELOCITY STAR; SDSS 1257+5428; GALACTIC DISK; HELIUM; MODELS; DETONATIONS; POPULATION; LUMINOSITY; EXPLOSION AB We study a complete, colour-selected sample of double-degenerate binary systems containing extremely low mass (ELM) <= 0.25M(circle dot) white dwarfs (WDs). We show, for the first time, that Milky Way disc ELM WDs have a merger rate of approximately 4 x 10(-5) yr(-1) due to gravitational wave radiation. The merger end product depends on the mass ratio of the binary. The ELM WD systems that undergo stable mass transfer can account for greater than or similar to 3 per cent of AM Canum Venaticorum (AM CVn) stars. More importantly, the ELM WD systems that may detonate merge at a rate comparable to the estimated rate of underluminous supernovae (SNe), rare explosions estimated to produce only similar to 0.2M(circle dot) worth of ejecta. At least 25 per cent of our ELM WD sample belong to the old thick disc and halo components of the Milky Way. Thus, if merging ELM WD systems are the progenitors of underluminous SNe, transient surveys must find them in both elliptical and spiral galaxies. C1 [Brown, Warren R.; Kilic, Mukremin; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU Smithsonian Institution; NASA under CalTech FX This research makes use of NASA's Astrophysics Data System Bibliographic Services. This work was supported in part by the Smithsonian Institution. MK is supported by NASA through the Spitzer Space Telescope Fellowship Programme, under an award from CalTech. NR 37 TC 23 Z9 23 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 411 IS 1 BP L31 EP L35 DI 10.1111/j.1745-3933.2010.00986.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710QF UT WOS:000286525600007 ER PT J AU Campana, S Salvaterra, R Tagliaferri, G Kouveliotou, C Grindlay, J AF Campana, S. Salvaterra, R. Tagliaferri, G. Kouveliotou, C. Grindlay, J. TI Probing the very high redshift Universe with gamma-ray bursts: prospects for observations with future X-ray instruments SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: general; X-rays: general ID DISTANT COSMIC EXPLOSION; CORE-COLLAPSE SUPERNOVAE; EARLY STAR-FORMATION; POPULATION-III; COLUMN DENSITIES; ALPHA SYSTEMS; BLACK-HOLES; HII REGION; 1ST STARS; AFTERGLOW AB Gamma-ray bursts (GRBs) are the most violent explosions in the Universe. Long-duration GRBs are associated with the collapse of massive stars, rivalling their host galaxies in luminosity. The discovery of the most distant spectroscopically confirmed object in the Universe, GRB090423, opened a new window on the high-redshift Universe, making it possible to study the cosmic reionization epoch and the preceding dark ages, as well as the generation of the first stars (Population III) using GRBs. Obviously this enables a wealth of new studies using the near-infrared (NIR) characteristics of GRB afterglows. Here we explore a different path, focusing on the next generation of X-ray missions with large-area-focusing telescopes and fast-repointing capabilities. We found that X-ray data can complement NIR observations and for the brightest GRBs can provide an accurate and independent redshift determination. Metallicity studies can also be carried out profitably once the redshift is known. Finally we discuss observational signatures of GRBs arising from Population III stars in the X-ray band. C1 [Campana, S.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, Lc, Italy. [Salvaterra, R.] Univ Insubria, I-22100 Como, Italy. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Campana, S (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, Lc, Italy. EM sergio.campana@brera.inaf.it OI Campana, Sergio/0000-0001-6278-1576; Salvaterra, Ruben/0000-0002-9393-8078; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU ASI [I/011/07/0] FX This work has been partially supported by ASI grant I/011/07/0. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 55 TC 8 Z9 8 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 410 IS 3 BP 1611 EP 1616 DI 10.1111/j.1365-2966.2010.17540.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703TN UT WOS:000286004300018 ER PT J AU Dutton, AA van den Bosch, FC Faber, SM Simard, L Kassin, SA Koo, DC Bundy, K Huang, JS Weiner, BJ Cooper, MC Newman, JA Mozena, M Koekemoer, AM AF Dutton, Aaron A. van den Bosch, Frank C. Faber, Sandra M. Simard, Luc Kassin, Susan A. Koo, David C. Bundy, Kevin Huang, Jiasheng Weiner, Benjamin J. Cooper, Michael C. Newman, Jeffrey A. Mozena, Mark Koekemoer, Anton M. TI On the evolution of the velocity-mass-size relations of disc-dominated galaxies over the past 10 billion years SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: haloes; galaxies: high-redshift; galaxies: spiral ID TULLY-FISHER RELATION; STAR-FORMING GALAXIES; DARK-MATTER HALOES; DIGITAL SKY SURVEY; OPTICAL-ROTATION CURVES; DISTANT FIELD GALAXIES; TKRS/GOODS-N FIELD; DEEP GROTH STRIP; STELLAR MASS; SURFACE BRIGHTNESS AB We study the evolution of the scaling relations between the maximum circular velocity, stellar mass and optical half-light radius of star-forming disc-dominated galaxies in the context of Lambda cold dark matter-based galaxy formation models. Using data from the literature combined with new data from the Deep Extragalactic Evolutionary Probe 2 (DEEP2) and All-wavelength Extended Groth Strip International Survey (AEGIS) surveys, we show that there is a consistent picture for the evolution of these scaling relations from z similar to 2 to z = 0, both observationally and theoretically. The evolution of the observed stellar scaling relations is weaker than that of the virial scaling relations of dark matter haloes, which can be reproduced, both qualitatively and quantitatively, with a simple, cosmologically motivated model for disc evolution inside growing Navarro-Frenk-White dark matter haloes. In this model optical half-light radii are smaller, both at fixed stellar mass and at maximum circular velocity, at higher redshifts. This model also predicts that the scaling relations between baryonic quantities (baryonic mass, baryonic half-mass radii and maximum circular velocity) evolve even more weakly than the corresponding stellar relations. We emphasize, though, that this weak evolution does not imply that individual galaxies evolve weakly. On the contrary, individual galaxies grow strongly in mass, size and velocity but in such a way that they move largely along the scaling relations. Finally, recent observations have claimed surprisingly large sizes for a number of star-forming disc galaxies at z similar or equal to 2, which has caused some authors to suggest that high-redshift disc galaxies have abnormally high spin parameters. However, we argue that the disc scalelengths in question have been systematically overestimated by a factor of similar to 2 and that there is an offset of a factor of similar to 1.4 between H alpha sizes and optical sizes. Taking these effects into account, there is no indication that star-forming galaxies at high redshifts (z similar or equal to 2) have abnormally high spin parameters. C1 [Dutton, Aaron A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Faber, Sandra M.; Koo, David C.; Mozena, Mark] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Faber, Sandra M.; Koo, David C.; Mozena, Mark] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [van den Bosch, Frank C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [van den Bosch, Frank C.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Simard, Luc] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Kassin, Susan A.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Bundy, Kevin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94705 USA. [Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weiner, Benjamin J.; Cooper, Michael C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Dutton, AA (reprint author), Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. EM dutton@uvic.ca OI Weiner, Benjamin/0000-0001-6065-7483; Koekemoer, Anton/0000-0002-6610-2048 FU National Science Foundation [AST-08-08133, AST 95-29098, 00-711098, 05-07483, 08-08133, AST 00-71048, 05-07428, 08-07630]; Hubble Space Telescope [GO-10532.02-A, GO-11206.02-A]; NSF Center for Particle Astrophysics; NASA [HST-AR-01947] FX We thank Nicolas Bouche for useful discussions regarding the SINS data. AAD acknowledges financial support from a CITA National Fellowship, from the National Science Foundation grant AST-08-08133 and from Hubble Space Telescope grants GO-10532.02-A and GO-11206.02-A.; The DEEP2 survey was initiated under the auspices of the NSF Center for Particle Astrophysics. Major grant support was provided by National Science Foundation grants AST 95-29098, 00-711098, 05-07483 and 08-08133 to UCSC and AST 00-71048, 05-07428 and 08-07630 to UCB. The DEEP2 survey has been made possible through the dedicated efforts of the DEIMOS instrument team at UC Santa Cruz and support of the staff at Keck Observatory. The HST ACS mosaic in EGS was constructed by Anton Koekemoer and Jennifer Lotz and was funded by grant HST-AR-01947 from NASA. Finally, we recognize and acknowledge the highly significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; it has been a privilege to be given the opportunity to conduct observations from this mountain. NR 93 TC 76 Z9 76 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 410 IS 3 BP 1660 EP 1676 DI 10.1111/j.1365-2966.2010.17555.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703TN UT WOS:000286004300024 ER PT J AU Danielson, ALR Swinbank, AM Smail, I Cox, P Edge, AC Weiss, A Harris, AI Baker, AJ De Breuck, C Geach, JE Ivison, RJ Krips, M Lundgren, A Longmore, S Neri, R Flaquer, BO AF Danielson, A. L. R. Swinbank, A. M. Smail, Ian Cox, P. Edge, A. C. Weiss, A. Harris, A. I. Baker, A. J. De Breuck, C. Geach, J. E. Ivison, R. J. Krips, M. Lundgren, A. Longmore, S. Neri, R. Ocana Flaquer, B. TI The properties of the interstellar medium within a star-forming galaxy at z=2.3 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: starburst; submillimetre: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; NEUTRAL ATOMIC CARBON; DENSE MOLECULAR GAS; LYMAN BREAK GALAXY; C I EMISSION; SUBMILLIMETER GALAXIES; HIGH-REDSHIFT; ARP 220; PHYSICAL CONDITIONS; NEARBY GALAXIES AB We present an analysis of the molecular and atomic gas emission in the rest-frame far-infrared and submillimetre from the lensed z = 2.3 submillimetre galaxy SMM J2135-0102. We obtain very high signal-to-noise ratio detections of 11 transitions from three species and limits on a further 20 transitions from nine species. We use the 12CO, [C i] and HCN line strengths to investigate the gas mass, kinematic structure and interstellar medium (ISM) chemistry and find strong evidence for a two-phase medium within this high-redshift starburst galaxy, comprising a hot, dense, luminous component and an underlying extended cool, low-excitation massive component. Employing a suite of photodissociation region models, we show that on average the molecular gas is exposed to an ultraviolet (UV) radiation field that is similar to 1000 times more intense than the Milky Way, with star-forming regions having a characteristic density of n similar to 104 cm-3. Thus, the average ISM density and far-UV radiation field intensity are similar to those found in local ultraluminous infrared galaxies (ULIRGs) and to those found in the central regions of typical starburst galaxies, even though the star formation rate is far higher in this system. The 12CO spectral line energy distribution and line profiles give strong evidence that the system comprises multiple kinematic components with different conditions, including temperature, and line ratios suggestive of high cosmic-ray flux within clouds, likely as a result of high star formation density. We find tentative evidence of a factor of similar to 4 temperature range within the system. We expect that such internal structures are common in high-redshift ULIRGs but are missed due to the poor signal-to-noise ratio of typical observations. We show that, when integrated over the galaxy, the gas and star formation surface densities appear to follow the Kennicutt-Schmidt relation, although by comparing our data to high-resolution submillimetre imaging, our data suggest that this relation breaks down on scales of < 100 pc. By virtue of the lens amplification, these observations uncover a wealth of information on the star formation and ISM at z similar to 2.3 at a level of detail that has only recently become possible at z < 0.1 and show the potential physical properties that will be studied in unlensed galaxies when the Atacama Large Millimeter Array is in full operation. C1 [Danielson, A. L. R.; Swinbank, A. M.; Smail, Ian; Edge, A. C.; Geach, J. E.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Cox, P.; Krips, M.; Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Ivison, R. J.] UK Astron Technol Ctr, Royal Observ, Edinburgh EH19 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Edinburgh EH19 3HJ, Midlothian, Scotland. [Lundgren, A.] European So Observ, Santiago 19, Chile. [Longmore, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ocana Flaquer, B.] Inst Radioastron Milimetr, Granada 18012, Spain. RP Danielson, ALR (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. EM a.l.r.danielson@durham.ac.uk RI Ocana Flaquer, Breezy/N-2734-2013; Smail, Ian/M-5161-2013; Ivison, R./G-4450-2011; OI Ocana Flaquer, Breezy/0000-0003-1685-4599; Smail, Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313; Edge, Alastair/0000-0002-3398-6916; De Breuck, Carlos/0000-0002-6637-3315 FU STFC; Sir Norman Lockyer Royal Astronomical Society; INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution and the Academia Sinica; National Science Foundation [AST-0503946, AST-070865]; National Radio Astronomy Observatory FX ALRD acknowledges an STFC studentship, AMS gratefully acknowledges a Sir Norman Lockyer Royal Astronomical Society Fellowship, IRS acknowledges support from STFC. We are very grateful to Padeli Papadopoulos for extensive disccusion and comments on this manuscript. We also thank Estelle Bayet, Carsten Kramer, Rowin Meijerink, Serena Viti, Paul van der Werf and Chris Wilson for a number of useful discussions. We thank the anonymous referee for useful comments which added to the clarity and content of this paper. The observations in this paper were carried out with the IRAM 30m and the Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). We also thank the ESO Director for generously granting DDT observations with the SHFI as part of program 283.A-5014 which is based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory and the Onsala Space Observatory. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Zpectrometer observations were taken as part of program 09A-040. Zpectrometer is supported by National Science Foundation grants AST-0503946 and AST-070865 and by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 98 TC 77 Z9 77 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 FEB PY 2011 VL 410 IS 3 BP 1687 EP 1702 DI 10.1111/j.1365-2966.2010.17549.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703TN UT WOS:000286004300026 ER PT J AU Sanders, JS Fabian, AC Smith, RK AF Sanders, J. S. Fabian, A. C. Smith, R. K. TI Constraints on turbulent velocity broadening for a sample of clusters, groups and elliptical galaxies using XMM-Newton SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE intergalactic medium; X-rays: galaxies: clusters ID X-RAY SPECTROSCOPY; INTRACLUSTER MEDIUM; CENTAURUS CLUSTER; RX J1347.5-1145; BULK MOTIONS; PROFILES; GAS; RX-J1347.5-1145; J1347-1145; PRESSURE AB Using the width of emission lines in XMM-Newton Reflection Grating Spectrometer spectra, we place direct constraints on the turbulent velocities of the X-ray emitting medium in the cores of 62 galaxy clusters, groups and elliptical galaxies. We find five objects where we can place an upper limit on the line-of-sight broadening of 500 km s-1 (90 per cent confidence level), using a single thermal component model. Two other objects are lower than this limit when two thermal components are used. Half of the objects examined have an upper limit on the velocity broadening of less than 700 km s-1. To look for objects which have significant turbulent broadening, we use Chandra spectral maps to compute the expected broadening caused by the spatial extent of the source. Comparing these with our observed results, we find that Klemola 44 has extra broadening at the level of 1500 km s-1. RX J1347.5-1145 shows weak evidence for turbulent velocities at 800 km s-1. In addition we obtain limits on turbulence for Zw 3146, Abell 496, Abell 1795, Abell 2204 and HCG 62 of less than 200 km s-1. After subtraction of the spatial contribution and including a 50 km s-1 systematic uncertainty, we find at least 15 sources with less than 20 per cent of the thermal energy density in turbulence. C1 [Sanders, J. S.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Smith, R. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sanders, JS (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM jss@ast.cam.ac.uk OI Sanders, Jeremy/0000-0003-2189-4501 FU Royal Society; National Aeronautics and Space Administration FX ACF thanks the Royal Society for support. We also thank J.-W. den Herder and G. Pratt for useful discussions.; This research has made use of the NASA/IPAC Extragalactic Data base (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 37 TC 59 Z9 59 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 FEB PY 2011 VL 410 IS 3 BP 1797 EP 1812 DI 10.1111/j.1365-2966.2010.17561.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703TN UT WOS:000286004300033 ER PT J AU Dominguez, A Primack, JR Rosario, DJ Prada, F Gilmore, RC Faber, SM Koo, DC Somerville, RS Perez-Torres, MA Perez-Gonzalez, P Huang, JS Davis, M Guhathakurta, P Barmby, P Conselice, CJ Lozano, M Newman, JA Cooper, MC AF Dominguez, A. Primack, J. R. Rosario, D. J. Prada, F. Gilmore, R. C. Faber, S. M. Koo, D. C. Somerville, R. S. Perez-Torres, M. A. Perez-Gonzalez, P. Huang, J. -S. Davis, M. Guhathakurta, P. Barmby, P. Conselice, C. J. Lozano, M. Newman, J. A. Cooper, M. C. TI Extragalactic background light inferred from AEGIS galaxy-SED-type fractions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; cosmology: observations; diffuse radiation; infrared: diffuse background ID ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; STAR-FORMATION RATES; ENERGY GAMMA-RAYS; OPTICAL LUMINOSITY FUNCTIONS; SUPERMASSIVE BLACK-HOLES; HIGH-REDSHIFT GALAXIES; MICRON SOURCE COUNTS; DIGITAL SKY SURVEY; FORS DEEP FIELD AB The extragalactic background light (EBL) is of fundamental importance both for understanding the entire process of galaxy evolution and for gamma-ray astronomy, but the overall spectrum of the EBL between 0.1 and 1000 mu m has never been determined directly from galaxy spectral energy distribution (SED) observations over a wide redshift range. The evolving, overall spectrum of the EBL is derived here utilizing a novel method based on observations only. This is achieved from the observed evolution of the rest-frame K-band galaxy luminosity function up to redshift 4, combined with a determination of galaxy-SED-type fractions. These are based on fitting Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE) templates to a multiwavelength sample of about 6000 galaxies in the redshift range from 0.2 to 1 from the All-wavelength Extended Groth Strip International Survey (AEGIS). The changing fractions of quiescent galaxies, star-forming galaxies, starburst galaxies and active galactic nucleus (AGN) galaxies in that redshift range are estimated, and two alternative extrapolations of SED types to higher redshifts are considered. This allows calculation of the evolution of the luminosity densities from the ultraviolet (UV) to the infrared (IR), the evolving star formation rate density of the Universe, the evolving contribution to the bolometric EBL from the different galaxy populations including AGN galaxies and the buildup of the EBL. Our EBL calculations are compared with those from a semi-analytic model, another observationally based model and observational data. The EBL uncertainties in our modelling based directly on the data are quantified, and their consequences for attenuation of very-high-energy gamma-rays due to pair production on the EBL are discussed. It is concluded that the EBL is well constrained from the UV to the mid-IR, but independent efforts from IR and gamma-ray astronomy are needed in order to reduce the uncertainties in the far-IR. C1 [Dominguez, A.; Lozano, M.] Univ Seville, Dept Fis Atom Mol & Nucl, E-41080 Seville, Spain. [Dominguez, A.; Prada, F.; Perez-Torres, M. A.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Primack, J. R.; Gilmore, R. C.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Rosario, D. J.; Faber, S. M.; Koo, D. C.; Guhathakurta, P.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Gilmore, R. C.] SISSA, I-34136 Trieste, Italy. [Somerville, R. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Perez-Gonzalez, P.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Davis, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Cooper, M. C.] Univ Arizona, Steward Observ, Tucson, AZ USA. RP Dominguez, A (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. EM alberto@iaa.es 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; Lozano Leyva, Manuel Luis/0000-0003-2853-4103; Conselice, Christopher/0000-0003-1949-7638; Dominguez, Alberto/0000-0002-3433-4610 FU Spanish Ministerio de Educacion y Ciencia; European regional development fund (FEDER) [FIS2008-04189, CSD2007-00042]; Junta de Andalucia [P07-FQM-02894]; Spanish MEC; Fermi Theory Grants [NNX08AW37G, NNX09AT98G, NNX10AP54G]; National Science Foundation [AST-0507483, AST-0808133]; Spanish MICINN [CSD2009-00064]; SISSA Astrophysics Sector; NASA; STFC FX We are grateful to Ranga-Ram Chary, Darren Croton, Amy Furniss, Valentino Gonzalez, Patrik Jonsson, Nepomuk Otte, Miguel Angel Sanchez-Conde, David Williams and Li Yan-Rong for fruitful discussions and to the anonymous referee for useful comments. We also thank Valentino Gonzalez for his help running FAST. AD warmly thanks the staff at SCIPP and the Astronomy Department-UCSC for their hospitality, where most of this work was done. AD's work has been supported by the Spanish Ministerio de Educacion y Ciencia and the European regional development fund (FEDER) under projects FIS2008-04189 and CPAN-Ingenio (CSD2007-00042), and by the Junta de Andalucia (P07-FQM-02894). AD also acknowledges the Spanish MEC for an FPI grant. JRP's and RCG's research is supported by Fermi Theory Grants NNX08AW37G, NNX09AT98G and NNX10AP54G. DJR acknowledges the support of the National Science Foundation through grants AST-0507483 and AST-0808133. FP thanks the support of the Spanish MICINN's Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064. RCG was also supported by a research fellowship from the SISSA Astrophysics Sector. This study makes use of data from AEGIS, a multiwavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA and other telescopes and supported in part by the NSF, NASA and the STFC. NR 149 TC 181 Z9 181 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2011 VL 410 IS 4 BP 2556 EP 2578 DI 10.1111/j.1365-2966.2010.17631.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706IG UT WOS:000286211000041 ER PT J AU Chakraborti, S Ray, A Soderberg, AM Loeb, A Chandra, P AF Chakraborti, S. Ray, A. Soderberg, A. M. Loeb, A. Chandra, P. TI Ultra-high-energy cosmic ray acceleration in engine-driven relativistic supernovae SO NATURE COMMUNICATIONS LA English DT Article ID RADIO-EMISSION; BURSTS; NEUTRINOS; ORIGIN; PROPAGATION; REDSHIFT; GALAXIES; PARTICLE; EVENTS; NUCLEI AB The origin of ultra-high-energy cosmic rays (UHECRs) remains an enigma. They offer a window to new physics, including tests of physical laws at energies unattainable by terrestrial accelerators. They must be accelerated locally, otherwise, background radiations would severely suppress the flux of protons and nuclei, at energies above the Greisen-Zatsepin-Kuzmin (GZK) limit. Nearby, gamma ray bursts (GRBs), hypernovae, active galactic nuclei and their flares have all been suggested and debated as possible sources. A local sub-population of type Ibc supernovae (SNe) with mildly relativistic outflows have been detected as sub-energetic GRBs, X-ray flashes and recently as radio afterglows without detected GRB counterparts. Here, we measure the size-magnetic field evolution, baryon loading and energetics, using the observed radio spectra of SN 2009bb. We place such engine-driven SNe above the Hillas line and establish that they can readily explain the post-GZK UHECRs. C1 [Chakraborti, S.; Ray, A.] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Chakraborti, S.; Ray, A.; Soderberg, A. M.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Chandra, P.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. RP Chakraborti, S (reprint author), Tata Inst Fundamental Res, Dept Astron & Astrophys, 1 Homi Bhabha Rd, Bombay 400005, Maharashtra, India. EM sayan@tifr.res.in FU Associated Universities FX S. C. and A. R. acknowledge discussions with Malcom Longair, Rohini Godbole and Shobo Bhattacharya. We thank the staff of the GMRT who have made some of the observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research (TIFR). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). S. C. and A. R. thank the Institute for Theory and Computation, Harvard University for their hospitality. NR 40 TC 20 Z9 21 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD FEB PY 2011 VL 2 AR 175 DI 10.1038/ncomms1178 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 732YP UT WOS:000288225900004 PM 21285953 ER PT J AU Agnarsson, I AF Agnarsson, Ingi TI Habitat patch size and isolation as predictors of occupancy and number of argyrodine spider kleptoparasites in Nephila webs SO NATURWISSENSCHAFTEN LA English DT Article DE Argyrodes elevates; Faiditus americanus; Patch size; Occupancy; Abundance; Patch connectedness; Spider webs; Kleptoparasites; Ideal free distribution ID ORB-WEAVING SPIDER; ANTIPODIANUS ARANEAE; THERIDIIDAE; AREA; TETRAGNATHIDAE; RESPONSES AB How fully a suitable habitat patch is utilized by organisms depends crucially on patch size and isolation. Testing this interplay is made difficult in many systems by the arbitrariness of defining a "habitat patch", measuring its boarders, and relatively low detection probability of the inhabitants. Spider webs as habitat patches for obligate web kleptoparasites are free from these problems. Each individual web is a highly discrete and readily measured habitat patch, and the detection probability of argyrodine spider kleptoparasites is very nearly 1. Hence, spider webs emerge as simple systems for ecological models such as patch occupancy and metapopulation biology. Recently, I showed that the distribution of kleptoparasites among host webs relates both to web (patch) size as well as patch connectivity. Here, I test the relative importance of patch size versus isolation in explaining patch occupancy and abundance of inhabitants. I find that (1) web size is the better predictor of patch occupancy and abundance. (2) Web size is overall positively correlated with abundance, but predicts it most precisely among interconnected webs and not at all among the most isolated webs. Hence, patch occupancy and inhabitant abundance is explained by a rather complex interplay between patch size and isolation. C1 [Agnarsson, Ingi] UPRRP, Dept Biol, Rio Piedras, PR 00931 USA. [Agnarsson, Ingi] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Agnarsson, I (reprint author), UPRRP, Dept Biol, Rio Piedras, PR 00931 USA. EM iagnarsson@gmail.com FU UMEB funded by NSF [DBI-0602642] FX Thanks go to Laura J. May-Collado for help with logistics and fieldwork, and Gabriel Jacome and Plinio Gondola at the STRI Bocas del Toro field station for their hospitality and help with permits and various logistics. This study was funded through the UMEB program funded by NSF grant (DBI-0602642) to A. Ramirez. Matjaz Kuntner, Jonathan Coddington, and two anonymous reviewers provided very useful comments which improved this manuscript. NR 27 TC 7 Z9 7 U1 4 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD FEB PY 2011 VL 98 IS 2 BP 163 EP 167 DI 10.1007/s00114-010-0750-3 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 712KD UT WOS:000286664700009 PM 21136246 ER PT J AU Suen, G Teiling, C Li, L Holt, C Abouheif, E Bornberg-Bauer, E Bouffard, P Caldera, EJ Cash, E Cavanaugh, A Denas, O Elhaik, E Fave, MJ Gadau, JR Gibson, JD Graur, D Grubbs, KJ Hagen, DE Harkins, TT Helmkampf, M Hu, H Johnson, BR Kim, J Marsh, SE Moeller, JA Munoz-Torres, MC Murphy, MC Naughton, MC Nigam, S Overson, R Rajakumar, R Reese, JT Scott, JJ Smith, CR Tao, S Tsutsui, ND Viljakainen, L Wissler, L Yandell, MD Zimmer, F Taylor, J Slater, SC Clifton, SW Warren, WC Elsik, CG Smith, CD Weinstock, GM Gerardo, NM Currie, CR AF Suen, Garret Teiling, Clotilde Li, Lewyn Holt, Carson Abouheif, Ehab Bornberg-Bauer, Erich Bouffard, Pascal Caldera, Eric J. Cash, Elizabeth Cavanaugh, Amy Denas, Olgert Elhaik, Eran Fave, Marie-Julie Gadau, Juergen Gibson, Joshua D. Graur, Dan Grubbs, Kirk J. Hagen, Darren E. Harkins, Timothy T. Helmkampf, Martin Hu, Hao Johnson, Brian R. Kim, Jay Marsh, Sarah E. Moeller, Joseph A. Munoz-Torres, Monica C. Murphy, Marguerite C. Naughton, Meredith C. Nigam, Surabhi Overson, Rick Rajakumar, Rajendhran Reese, Justin T. Scott, Jarrod J. Smith, Chris R. Tao, Shu Tsutsui, Neil D. Viljakainen, Lumi Wissler, Lothar Yandell, Mark D. Zimmer, Fabian Taylor, James Slater, Steven C. Clifton, Sandra W. Warren, Wesley C. Elsik, Christine G. Smith, Christopher D. Weinstock, George M. Gerardo, Nicole M. Currie, Cameron R. TI The Genome Sequence of the Leaf-Cutter Ant Atta cephalotes Reveals Insights into Its Obligate Symbiotic Lifestyle SO PLOS GENETICS LA English DT Article ID FUNGUS-GROWING ANTS; HONEYBEE APIS-MELLIFERA; DE-NOVO IDENTIFICATION; INSULIN-LIKE PEPTIDES; DNA METHYLATION; GENE ONTOLOGY; MITOCHONDRIAL GENOME; TRIPARTITE MUTUALISM; EUKARYOTIC GENOMES; MICROBE SYMBIOSIS AB Leaf-cutter ants are one of the most important herbivorous insects in the Neotropics, harvesting vast quantities of fresh leaf material. The ants use leaves to cultivate a fungus that serves as the colony's primary food source. This obligate ant-fungus mutualism is one of the few occurrences of farming by non-humans and likely facilitated the formation of their massive colonies. Mature leaf-cutter ant colonies contain millions of workers ranging in size from small garden tenders to large soldiers, resulting in one of the most complex polymorphic caste systems within ants. To begin uncovering the genomic underpinnings of this system, we sequenced the genome of Atta cephalotes using 454 pyrosequencing. One prediction from this ant's lifestyle is that it has undergone genetic modifications that reflect its obligate dependence on the fungus for nutrients. Analysis of this genome sequence is consistent with this hypothesis, as we find evidence for reductions in genes related to nutrient acquisition. These include extensive reductions in serine proteases (which are likely unnecessary because proteolysis is not a primary mechanism used to process nutrients obtained from the fungus), a loss of genes involved in arginine biosynthesis (suggesting that this amino acid is obtained from the fungus), and the absence of a hexamerin (which sequesters amino acids during larval development in other insects). Following recent reports of genome sequences from other insects that engage in symbioses with beneficial microbes, the A. cephalotes genome provides new insights into the symbiotic lifestyle of this ant and advances our understanding of host-microbe symbioses. C1 [Suen, Garret; Caldera, Eric J.; Cavanaugh, Amy; Grubbs, Kirk J.; Marsh, Sarah E.; Moeller, Joseph A.; Scott, Jarrod J.; Slater, Steven C.; Currie, Cameron R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Suen, Garret; Moeller, Joseph A.; Scott, Jarrod J.; Slater, Steven C.; Currie, Cameron R.] Univ Wisconsin, Dept Energy, Great Lakes Bioenergy Res Ctr, Madison, WI USA. [Teiling, Clotilde; Harkins, Timothy T.] Roche Diagnost, Indianapolis, IN USA. [Li, Lewyn; Bouffard, Pascal] 454 Life Sci, Branford, CT USA. [Holt, Carson; Hu, Hao; Yandell, Mark D.] Univ Utah, Dept Human Genet, Salt Lake City, UT USA. [Abouheif, Ehab; Fave, Marie-Julie; Rajakumar, Rajendhran] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Bornberg-Bauer, Erich; Wissler, Lothar; Zimmer, Fabian] Univ Munster, Inst Evolut & Biodivers, Munster, Germany. [Caldera, Eric J.] Univ Wisconsin, Dept Zool, Madison, WI 53706 USA. [Cash, Elizabeth; Gadau, Juergen; Gibson, Joshua D.; Helmkampf, Martin; Overson, Rick] Arizona State Univ, Sch Life Sci, Tempe, AZ USA. [Cavanaugh, Amy] Univ Wisconsin Rock Cty, Dept Biol, Janesville, WI USA. [Denas, Olgert; Taylor, James] Emory Univ, Dept Math & Comp Sci, Atlanta, GA 30322 USA. [Elhaik, Eran] Johns Hopkins Univ, Sch Med, Baltimore, MD USA. [Graur, Dan] Univ Houston, Dept Biol & Biochem, Houston, TX USA. [Grubbs, Kirk J.] Univ Wisconsin, Cellular & Mol Pathol Grad Program, Madison, WI USA. [Hagen, Darren E.; Munoz-Torres, Monica C.; Reese, Justin T.; Tao, Shu; Elsik, Christine G.] Georgetown Univ, Dept Biol, Washington, DC 20057 USA. [Johnson, Brian R.; Tsutsui, Neil D.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Kim, Jay; Smith, Christopher D.] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. [Marsh, Sarah E.] Univ Wisconsin, Dept Genet, Madison, WI 53706 USA. [Murphy, Marguerite C.; Nigam, Surabhi] San Francisco State Univ, Dept Comp Sci, San Francisco, CA 94132 USA. [Naughton, Meredith C.; Smith, Chris R.] Earlham Coll, Dept Biol, Richmond, IN 47374 USA. [Scott, Jarrod J.; Currie, Cameron R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Viljakainen, Lumi] Cornell Univ, Dept Mol Biol & Genet, Ithaca, NY USA. [Taylor, James; Gerardo, Nicole M.] Emory Univ, Dept Biol, Atlanta, GA 30322 USA. [Clifton, Sandra W.; Warren, Wesley C.; Weinstock, George M.] Washington Univ, Sch Med, Genome Ctr, St Louis, MO USA. RP Suen, G (reprint author), Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. EM gsuen@wisc.edu; currie@bact.wisc.edu RI Taylor, James/F-1026-2011; Weinstock, George/C-6314-2013; Bornberg-Bauer, Erich/A-1563-2013; Hu, Hao/I-4399-2014; Elsik, Christine/C-4120-2017; OI Taylor, James/0000-0001-5079-840X; Weinstock, George/0000-0002-2997-4592; Bornberg-Bauer, Erich/0000-0002-1826-3576; Elsik, Christine/0000-0002-4248-7713; Suen, Garret/0000-0002-6170-711X FU Roche Diagnostics; DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science) [DE-FC02-07ER64494]; Volkswagen Foundation; Deutsche Forschungsgemeinschaft (DFG) [BO2544-4/1]; National Science Foundation; University of Wisconsin-Madison Colleges; US National Library of Medicine [LM010009-01]; Smithsonian Institution; National Institutes of Health [5R01HG004694]; National Institutes of Health NIMH [5SC2MH086071]; National Institute of Food and Agriculture, United States Department of Agriculture [WISO1321]; University of Wisconsin-Madison CALS; National Science Foundation [DEB-0747002, MCB-0702025, MCB-0731822] FX This work was supported by a Roche Diagnostics 10 Gigabase Sequencing and Transcriptome Analysis Grant awarded to GS, JT, SCS, SWC, GMW, NMG, and CRC. This work was also funded by the DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science DE-FC02-07ER64494) supporting GS, CRC, JAM, and SCS; a Volkswagen Foundation grant supporting EB-B and LW; a Deutsche Forschungsgemeinschaft (DFG) grant BO2544-4/1 to EB-B; a National Science Foundation Graduate Research Fellowship supporting EJC; a University of Wisconsin-Madison Colleges Summer Research Grant supporting AC; a US National Library of Medicine Grant LM010009-01 to DG; a Smithsonian Institution Predoctoral Fellowship supporting JJS; a National Institutes of Health grant 5R01HG004694 to MDY supporting the MAKER genome annotation; and a National Institutes of Health NIMH grant 5SC2MH086071 to CDS. This material is also based upon work support by the National Institute of Food and Agriculture, United States Department of Agriculture, under ID number WISO1321, a University of Wisconsin-Madison CALS grant, and the National Science Foundation grants DEB-0747002, MCB-0702025, and MCB-0731822 to CRC. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 96 TC 120 Z9 124 U1 5 U2 88 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1553-7390 J9 PLOS GENET JI PLoS Genet. PD FEB PY 2011 VL 7 IS 2 AR e1002007 DI 10.1371/journal.pgen.1002007 PG 11 WC Genetics & Heredity SC Genetics & Heredity GA 726CV UT WOS:000287697300039 PM 21347285 ER PT J AU Schoenian, I Spiteller, M Ghaste, M Wirth, R Herz, H Spiteller, D AF Schoenian, Ilka Spiteller, Michael Ghaste, Manoj Wirth, Rainer Herz, Hubert Spiteller, Dieter TI Chemical basis of the synergism and antagonism in microbial communities in the nests of leaf-cutting ants SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE chemical imaging; antibiotics; chemical defense; ecological function ID FUNGUS-GROWING ANTS; ATTA-SEXDENS-RUBROPILOSA; FILAMENTOUS BACTERIA; ANTIFUNGAL ACTIVITY; ACTINOMYCIN-D; VALINOMYCIN; ANTIMYCIN; ANTIBIOTICS; SYMBIOSIS; GARDENS AB Leaf-cutting ants cultivate the fungus Leucoagaricus gongylophorus, which serves as a major food source. This symbiosis is threatened by microbial pathogens that can severely infect L. gongylophorus. Microbial symbionts of leaf-cutting ants, mainly Pseudonocardia and Streptomyces, support the ants in defending their fungus gardens against infections by supplying antimicrobial and antifungal compounds. The ecological role of microorganisms in the nests of leaf-cutting ants can only be addressed in detail if their secondary metabolites are known. Here, we use an approach for the rapid identification of established bioactive compounds from microorganisms in ecological contexts by combining phylogenetic data, database searches, and liquid chromatography electrospray ionisation high resolution mass spectrometry (LC-ESI-HR-MS) screening. Antimycins A(1)-A(4), valinomycins, and actinomycins were identified in this manner from Streptomyces symbionts of leaf-cutting ants. Matrix-assisted laser desorption ionization (MALDI) imaging revealed the distribution of valinomycin directly on the integument of Acromyrmex echinatior workers. Valinomycins and actinomycins were also directly identified in samples from the waste of A. echinatior and A. niger leaf-cutting ants, suggesting that the compounds exert their antimicrobial and antifungal potential in the nests of leaf-cutting ants. Strong synergistic effects of the secondary metabolites produced by ant-associated Streptomyces were observed in the agar diffusion assay against Escovopsis weberi. Actinomycins strongly inhibit soil bacteria as well as other Streptomyces and Pseudonocardia symbionts. The antifungal antimycins are not only active against pathogenic fungi but also the garden fungus L. gongylophorus itself. In conclusion, secondary metabolites of microbial symbionts of leaf-cutting ants contribute to shaping the microbial communities within the nests of leaf-cutting ants. C1 [Schoenian, Ilka; Spiteller, Dieter] Max Planck Inst Chem Ecol, Dept Bioorgan Chem, D-07745 Jena, Germany. [Spiteller, Michael; Ghaste, Manoj] Dortmund Univ Technol, Fac Chem, Inst Environm Res, D-44221 Dortmund, Germany. [Wirth, Rainer] Tech Univ Kaiserslautern, Dept Plant Ecol & Systemat, D-67663 Kaiserslautern, Germany. [Herz, Hubert] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Spiteller, D (reprint author), Max Planck Inst Chem Ecol, Dept Bioorgan Chem, D-07745 Jena, Germany. EM dspiteller@ice.mpg.de RI Ghaste, Manoj/G-9149-2011; Wirth, Rainer/I-1552-2013; OI Wirth, Rainer/0000-0001-8042-3123; Ghaste, Manoj/0000-0002-5018-2178 FU Deutsche Forschungsgemeinschaft [SP 1106/3-1]; Jena School for Microbial Communication (JSMC); Verband der Chemischen Industrie; Max Planck Society FX We thank the Smithsonian Tropical Research Institute (STRI) for providing logistic help and the Autoridad Nacional del Ambiente y el Mar (ANAM) for permission to sample ant colonies in Panama and for issuing export permits. We are indebted to Dr. Kusari for performing the stereomicroscope imaging and Emily Wheeler for editorial assistance. D.S. thanks Professor Dr. Boland for his generous support, the Deutsche Forschungsgemeinschaft for an Emmy Noether Fellowship (SP 1106/3-1), and the Jena School for Microbial Communication (JSMC) for financial support. Further funding by the Verband der Chemischen Industrie and the Max Planck Society is gratefully acknowledged. NR 51 TC 72 Z9 73 U1 5 U2 91 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 1 PY 2011 VL 108 IS 5 BP 1955 EP 1960 DI 10.1073/pnas.1008441108 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 714JA UT WOS:000286804700040 PM 21245311 ER PT J AU Liebhold, P AF Liebhold, Peter TI Special Review Section: Corporate Presentations of History Introduction SO PUBLIC HISTORIAN LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Liebhold, P (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RI Liebhold, Andrew/C-1423-2008 OI Liebhold, Andrew/0000-0001-7427-6534 NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS & DIGITAL PUBLISHING DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FEB PY 2011 VL 33 IS 1 BP 73 EP 74 DI 10.1525/tph.2011.33.1.73 PG 2 WC History SC History GA 731XR UT WOS:000288144400005 ER PT J AU Stine, JK AF Stine, Jeffrey K. TI Working in the Dry: Cofferdams, In-River Construction, and the United States Army Corps of Engineers SO PUBLIC HISTORIAN LA English DT Book Review C1 [Stine, Jeffrey K.] Smithsonian Inst, Washington, DC 20560 USA. RP Stine, JK (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS & DIGITAL PUBLISHING DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FEB PY 2011 VL 33 IS 1 BP 113 EP 114 DI 10.1525/tph.2011.33.1.113 PG 2 WC History SC History GA 731XR UT WOS:000288144400021 ER PT J AU van Dishoeck, EF Kristensen, LE Benz, AO Bergin, EA Caselli, P Cernicharo, J Herpin, F Hogerheijde, MR Johnstone, D Liseau, R Nisini, B Shipman, R Tafalla, M van der Tak, F Wyrowski, F Aikawa, Y Bachiller, R Baudry, A Benedettini, M Bjerkeli, P Blake, GA Bontemps, S Braine, J Brinch, C Bruderer, S Chavarria, L Codella, C Daniel, F de Graauw, T Deul, E di Giorgio, AM Dominik, C Doty, SD Dubernet, ML Encrenaz, P Feuchtgruber, H Fich, M Frieswijk, W Fuente, A Giannini, T Goicoechea, JR Helmich, FP Herczeg, GJ Jacq, T Jorgensen, JK Karska, A Kaufman, MJ Keto, E Larsson, B Lefloch, B Lis, D Marseille, M McCoey, C Melnick, G Neufeld, D Olberg, M Pagani, L Panic, O Parise, B Pearson, JC Plume, R Risacher, C Salter, D Santiago-Garcia, J Saraceno, P Stauber, P van Kempen, TA Visser, R Viti, S Walmsley, M Wampfler, SF Yildiz, UA AF van Dishoeck, E. F. Kristensen, L. E. Benz, A. O. Bergin, E. A. Caselli, P. Cernicharo, J. Herpin, F. Hogerheijde, M. R. Johnstone, D. Liseau, R. Nisini, B. Shipman, R. Tafalla, M. van der Tak, F. Wyrowski, F. Aikawa, Y. Bachiller, R. Baudry, A. Benedettini, M. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Brinch, C. Bruderer, S. Chavarria, L. Codella, C. Daniel, F. de Graauw, Th. Deul, E. di Giorgio, A. M. Dominik, C. Doty, S. D. Dubernet, M. L. Encrenaz, P. Feuchtgruber, H. Fich, M. Frieswijk, W. Fuente, A. Giannini, T. Goicoechea, J. R. Helmich, F. P. Herczeg, G. J. Jacq, T. Jorgensen, J. K. Karska, A. Kaufman, M. J. Keto, E. Larsson, B. Lefloch, B. Lis, D. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Olberg, M. Pagani, L. Panic, O. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Salter, D. Santiago-Garcia, J. Saraceno, P. Staeuber, P. van Kempen, T. A. Visser, R. Viti, S. Walmsley, M. Wampfler, S. F. Yildiz, U. A. TI Water in Star-forming Regions with the Herschel Space Observatory (WISH). I. Overview of Key Program and First Results SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; PROTOSTELLAR SHOCK L1157-B1; FAR-INFRARED OBSERVATIONS; WAVE-ASTRONOMY-SATELLITE; VELA MOLECULAR CLOUDS; CHESS SPECTRAL SURVEY; NGC-7129 FIRS 2; GAS-PHASE H2O; HOT CORES AB Water In Star-forming regions with Herschel (WISH) is a key program on the Herschel Space Observatory designed to probe the physical and chemical structures of young stellar objects using water and related molecules and to follow the water abundance from collapsing clouds to planet-forming disks. About 80 sources are targeted, covering a wide ranee of luminosities-from low (< 1 L-circle dot) to high (> 10(5) L-circle dot)-and a wide range of evolutionary stages-from cold prestellar cores to warm protostellar envelopes and outflows to disks around young stars. Both the HIFI and PACS instruments are used to observe a variety of lines of H2O, (H2O)-O-18 and chemically related species at the source position and in small maps around the protostars and selected outflow positions. In addition, high-frequency lines of CO, (CO)-C-13, and (CO)-O-18 are obtained with Herschel and are complemented by ground-based observations of dust continuum, HDO, CO and its isotopologs, and other molecules to ensure a self-consistent data set for analysis. An overview of the scientific motivation and observational strategy of the program is given, together with the modeling approach and analysis tools that have been developed. Initial science results are presented. These include a lack of water in cold gas at abundances that are lower than most predictions, strong water emission from shocks in protostellar environments, the importance of UV radiation in heating the gas along outflow walls across the full range of luminosities, and surprisingly widespread detection of the chemically related hydrides OH+ and H2O+ in outflows and foreground gas. Quantitative estimates of the energy budget indicate that H2O is generally not the dominant coolant in the warm dense gas associated with protostars. Very deep limits on the cold gaseous water reservoir in the outer regions of protoplanetary disks are obtained that have profound implications for our understanding of grain growth and mixing in disks. C1 [van Dishoeck, E. F.; Kristensen, L. E.; Hogerheijde, M. R.; Brinch, C.; Deul, E.; Salter, D.; van Kempen, T. A.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Feuchtgruber, H.; Herczeg, G. J.; Karska, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Benz, A. O.; Bruderer, S.; Staeuber, P.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.; Walmsley, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Herpin, F.; Baudry, A.; Bontemps, S.; Braine, J.; Chavarria, L.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Herpin, F.; Baudry, A.; Bontemps, S.; Braine, J.; Chavarria, L.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Liseau, R.; Bjerkeli, P.; Olberg, M.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Nisini, B.; Giannini, T.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Shipman, R.; van der Tak, F.; de Graauw, Th.; Helmich, F. P.; Marseille, M.; Risacher, C.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Tafalla, M.; Bachiller, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Aikawa, Y.] Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] Area Ric Tor Vergata, INAF Inst Fis Spazio Interplanetario, I-00133 Rome, Italy. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Dubernet, M. L.] Univ Paris 06, LPMAA UMR CNRS 7092, F-75252 Paris 05, France. [Dubernet, M. L.] Observ Paris, LUTH UMR CNRS 8102, F-92195 Meudon, France. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.; Pagani, L.] Observ Paris, UMR 8112, CNRS, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Jorgensen, J. K.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Kaufman, M. J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Keto, E.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lefloch, B.] Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, UMR5571, F-38041 Grenoble 9, France. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Panic, O.] European So Observ, D-85748 Garching, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst RadioAstron Milimetr, E-18012 Granada, Spain. [Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP van Dishoeck, EF (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM ewine@strw.leidenuniv.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Brinch, Christian/G-5157-2015; Fuente, Asuncion/G-1468-2016; Karska, Agata/O-5311-2016; OI , Brunella Nisini/0000-0002-9190-0113; Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Brinch, Christian/0000-0002-5074-7183; Fuente, Asuncion/0000-0001-6317-6343; Karska, Agata/0000-0001-8913-925X; Bjerkeli, Per/0000-0002-7993-4118; Giannini, Teresa/0000-0002-0224-096X NR 280 TC 139 Z9 139 U1 2 U2 14 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 FEB PY 2011 VL 123 IS 900 BP 138 EP 170 DI 10.1086/658676 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 728WI UT WOS:000287904800004 ER PT J AU Clough, GW AF Clough, G. Wayne TI Trail Blazing SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD FEB PY 2011 VL 41 IS 10 BP 22 EP 22 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 710AN UT WOS:000286482900011 ER PT J AU Sutton-Grier, AE Megonigal, JP AF Sutton-Grier, Ariana E. Megonigal, J. Patrick TI Plant species traits regulate methane production in freshwater wetland soils SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Juncus effusus; Peltandra virginica; Phragmites australis; Typha latifolia; Microbial respiration; Anaerobic decomposition; Maryland; Methane; Wetland; Greenhouse gas; Primary production; Fe(III); Root porosity ID PHRAGMITES-AUSTRALIS; EMERGENT MACROPHYTES; AQUATIC MACROPHYTES; TYPHA-LATIFOLIA; SEDIMENTS; RHIZOSPHERE; CARBON; IRON; METHANOGENESIS; EMISSIONS AB Ecosystem and biogeochemical responses to anthropogenic stressors are the result of complex interactions between plants and microbes. A mechanistic understanding of how plant traits influence microbial processes is needed in order to predict the ecosystem-level effects of natural or anthropogenic change. This is particularly true in wetland ecosystems, where plants alter the availability of both electron donors (e.g., organic carbon) and electron acceptors (e.g., oxygen and ferric iron), thereby regulating the total amount of anaerobic respiration and the production of methane, a highly potent greenhouse gas. In this study, we examined how plant traits associated with plant inputs of carbon (photosynthesis and biomass) and oxygen (root porosity and ferric iron on roots) to mineral soils relate to microbial competition for organic carbon and, ultimately, methane production. Plant productivity was positively correlated with microbial respiration and negatively correlated to methane production. Root porosity was relatively constant across plant species, but belowground biomass, total biomass, and the concentration of oxidized (ferric) iron on roots varied significantly between species. As a result the size of the total root oxidized iron pool varied considerably across plant species, scaling with plant productivity. Large pools of oxidized iron were related to high CO(2):CH(4) ratios during microbial respiration, indicating that as plant productivity and biomass increased, microbes used non-methanogenic respiration pathways, most likely including the reduction of iron oxides. Taken together these results suggest that increased oxygen input from plants with greater biomass can offset any potential stimulation of methanogenic microbes from additional carbon inputs. Because the species composition of plant communities influences both electron donor and acceptor availability in wetland soils, changes in plant species as a consequence of anthropogenic disturbance have the potential to trigger profound effects on microbial processes, including changes in anaerobic decomposition rates and the proportion of mineralized carbon emitted as the greenhouse gas methane. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Sutton-Grier, Ariana E.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Sutton-Grier, AE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM ariana.suttongrier@gmail.com OI Sutton-Grier, Ariana/0000-0002-1242-7728 FU NSF [DEB-0516400] FX We thank Allyson Bullock, Rachel Koch, and Susanna Gomez for help with the lab work, Nick Mudd for help watering, and Jim Duls for help setting up the pots and tubs in the chamber. Karin Kettenring, Mark Feilly at Ernst Conservation Seed, and Penny at Environmental Concern, provided helpful advice for how to start the seeds and plugs in the greenhouse. An earlier version of this manuscript was greatly improved by feedback from the SERC Science and Coffee Discussion Group as well as specific comments from Jason Keller, Virginie Bouchard, Thomas Mozdzer, Kathy Boomer, Eric Lind, Kelly Malone, April Blakeslee, and two anonymous reviewers. This work was supported by NSF Grant DEB-0516400 to JPM. NR 50 TC 33 Z9 43 U1 12 U2 114 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 FEB PY 2011 VL 43 IS 2 BP 413 EP 420 DI 10.1016/j.soilbio.2010.11.009 PG 8 WC Soil Science SC Agriculture GA 716KP UT WOS:000286967800024 ER PT J AU Zhang, JW Nie, ZL Wen, J Sun, H AF Zhang, Jian-Wen Nie, Ze-Long Wen, Jun Sun, Hang TI Molecular phylogeny and biogeography of three closely related genera, Soroseris, Stebbinsia, and Syncalathium (Asteraceae, Cichorieae), endemic to the Tibetan Plateau, SW China SO TAXON LA English DT Article DE biogeography; phylogeny; Soroseris; Stebbinsia; Syncalathium; Tibetan Plateau ID NUCLEAR RIBOSOMAL DNA; INTERNAL TRANSCRIBED SPACERS; TRNL-F SEQUENCES; CHLOROPLAST DNA; SAUSSUREA ASTERACEAE; EVOLUTION; RADIATION; COMPOSITAE; REGIONS; INFERENCE AB Soroseris, Stebbinsia, and Syncalathium are three genera of the sunflower family (Asteraceae) with restricted distributions on high screes of the Tibetan Plateau. We present a molecular analysis to test the monophyly of the genera, evaluate the phylogenetic relationships and construct their biogeographic diversification history. Nuclear ITS and plastid trnL-F and psbA-trnH fragments were analyzed with parsimony, Bayesian inference, and relaxed Bayesian dating for all species of Soroseris, Stebbinsia, and Syncalathium. Stebbinsia is part of a polytomy with several lineages of Soroseris. Syncalathium is biphyletic with Syn. souliei placed within subtribe Lactucinae and the remaining species close to the Soroseris-Stebbinsia clade within subtribe Crepidinae. Bayesian dating based on ITS sequences and using four fossil calibrations suggests that the stem and crown ages of the Soroseris-Stebbinsia clade and the two groups of Syncalathium are between 8.44 and 1.56 million years. Stebbinsia should be treated as a section of Soroseris and Syncalathium souliei should be excluded from Syncalathium and either placed in Lactuca s.l. or established as a new genus in Lactucinae. The remaining species are to be treated as Syncalathium s.str. in Crepidinae. The diversification of these groups in the Tibetan Plateau is of relatively young age, and can be explained by rapid diversification and radiation of the Soroseris-Stebbinsia clade, allopatric speciation within Syncalathium s.str. and convergent evolution of Syncalathium s.str. and Syn. souliei. The speciation events correlated with climatic change and fragmentation of scree habitats during the uplift of the Tibetan Plateau. Possible migration routes in Syncalathium s.str. from the northeast to the central and southern part of the Tibetan Plateau are suggested. C1 [Zhang, Jian-Wen; Nie, Ze-Long; Sun, Hang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Zhang, Jian-Wen] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Sun, H (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. EM hsun@mail.kib.ac.cn RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 FU National 973 Project of China [2007CB411601]; National Natural Science Foundation of China (NSFC) [30625004, 40930209, 31000101]; Yunnan Natural Science Foundation [2008CC013]; Chinese Academy of Sciences [KSCX2-YW-Z-1019]; National Science Foundation of U.S.A. [DEB-0321846] FX This study was supported by grants-in-aid from the National 973 Project of China (2007CB411601), the National Natural Science Foundation of China (NSFC, 30625004, 40930209, 31000101), the Yunnan Natural Science Foundation (2008CC013), Innovation Project of Chinese Academy of Sciences (KSCX2-YW-Z-1019) and the National Science Foundation of U.S.A. (DEB-0321846 to D.E. Boufford). We thank two anonymous reviewers for their helpful suggestions on the manuscript. The first author is indebted to Dr. N. Kilian for providing useful information and suggestions on the manuscript, Sees-editing Ltd. and the editor-in-chief of Taxon for improving the English, K. Fujikawa, T.Y. Tu, Y. Yang and W.D. Zhu for collecting the material, and H.G. Zha, J.P. Yue and Y.H. Zhang for assistance during the experiments and the sequences analysis. NR 78 TC 36 Z9 38 U1 1 U2 18 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD FEB PY 2011 VL 60 IS 1 BP 15 EP 26 PG 12 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 725FS UT WOS:000287631200003 ER PT J AU Cardona, A Valencia, VA Bayona, G Duque, J Ducea, M Gehrels, G Jaramillo, C Montes, C Ojeda, G Ruiz, J AF Cardona, A. Valencia, V. A. Bayona, G. Duque, J. Ducea, M. Gehrels, G. Jaramillo, C. Montes, C. Ojeda, G. Ruiz, J. TI Early-subduction-related orogeny in the northern Andes: Turonian to Eocene magmatic and provenance record in the Santa Marta Massif and Rancheria Basin, northern Colombia SO TERRA NOVA LA English DT Article ID PLATE TECTONIC EVOLUTION; MANTLE REFERENCE FRAME; SOUTH-AMERICA; CONTINENTAL-CRUST; CARIBBEAN PLATEAU; WESTERN COLOMBIA; FLAT SUBDUCTION; OCEANIC-CRUST; SLAB BREAKOFF; ISLAND-ARC AB P>The timing of orogeny in the northern Andes and the mechanism driving it are still debated. We have studied the age, composition and provenance of granitoids and sandstones of the Santa Marta Massif and Rancheria Basin, northern Colombia, to relate deep-seated and surface tectonic processes attending the Late Cretaceous-Palaeogene history of the northern Andes. Our results indicate the development of five tectonic episodes: (1) collision of northwestern South America with a 92-80 Ma Caribbean arc (70 Ma); (2) late-collisional to early-subduction metamorphism and magmatism (65 Ma); (3) distal accumulation of a thick siliciclastic sequence (60-58 Ma); (4) renewed arc magmatism (58-50 Ma); and (5) magmatic quiescence and block uplift (post-50 Ma). The first episodes are related to the onset of subduction, and the last episode is related to shallow subduction and oblique convergence. Similar events in Colombia and Ecuador reveal that the Late Cretaceous-Eocene orogeny of the northern Andes was influenced by the collision and subduction of the Caribbean oceanic plate. C1 [Cardona, A.] Smithsonian Trop Res Inst, Ctr Trop Paleobiol & Archeol, Balbona, Ancon, Panama. [Cardona, A.; Ojeda, G.] Inst Colombiano Petroleo, Piedecuesta, Colombia. [Valencia, V. A.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. [Bayona, G.; Montes, C.] Corp Geol Ares, Bogota, Colombia. [Duque, J.] Univ Autonoma Mexico, Ctr Geociencias, Queretaro, Mexico. [Ducea, M.; Gehrels, G.; Ruiz, J.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleobiol & Archeol, Balbona, Ancon, Panama. EM cardonaa@si.edu RI Ducea, Mihai/C-2872-2011; Ducea, Mihai/I-3139-2012; OI Ducea, Mihai/0000-0002-5322-0782; Montes, Camilo/0000-0002-3553-0787 FU Empresa Colombiana de Petroleos (ECOPETROL); Instituto de Investigaciones Marinas y Costeras (INVEMAR); Instituto Colombiano de Geologia y Mineria (INGEOMINAS); Carbones El Cerrejon; Banco de la Republica de Colombia; National Science Foundation [EAR-0443387, 0732436] FX We are grateful to Empresa Colombiana de Petroleos (ECOPETROL), Instituto de Investigaciones Marinas y Costeras (INVEMAR), Instituto Colombiano de Geologia y Mineria (INGEOMINAS) and Carbones El Cerrejon for partial funding. This research also received support from the Banco de la Republica de Colombia, project 2289. Funding for the Arizona Laser-Chron Center is provided by National Science Foundation grants EAR-0443387 and 0732436. Discussions and suggestions by J. Pindell, W. Winkler, G. Pe Pipper, W. Maresh, J. Wright and an anonymous reviewer, as well as the editorial care of Alfred Kroner and the Associate Editor, are enormously appreciated. This is a contribution to the International Geological Correlation Programme 546, Subduction Zones of the Caribbean. NR 80 TC 13 Z9 17 U1 1 U2 11 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0954-4879 J9 TERRA NOVA JI Terr. Nova PD FEB PY 2011 VL 23 IS 1 BP 26 EP 34 DI 10.1111/j.1365-3121.2010.00979.x PG 9 WC Geosciences, Multidisciplinary SC Geology GA 706IX UT WOS:000286212700004 ER PT J AU Moratelli, R Wilson, DE AF Moratelli, Ricardo Wilson, Don E. TI The identity of Myotis punensis (Chiroptera: Vespertilionidae) SO ZOOLOGIA LA English DT Article DE Ecuador; Myotinae; Myotis albescens; Myotis esmeraldae; synonymy ID BATS AB Currently twelve species of Myotis Kaup, 1829 (Vespertilionidae: Myotinae) are recognized from South America, with several other named taxa regarded as synonyms, among them Myotis punensis J.A. Allen, 1914. This name was first regarded as a junior synonym of Myotis albescens (E. Geoffroy, 1806) and subsequently of Myotis nigricans (Schinz, 1821). To address the taxonomic status of the holotype of M. punensis, we compared it to all South American species in the genus. The fringe of hairs on the trailing edge of the uropatagium, the fur color, and external and skull dimensions all suggest M. punensis should be treated as a junior synonym of M. albescens. C1 [Moratelli, Ricardo] Fundacao Oswaldo Cruz Rio de Janeiro, BR-22713375 Rio De Janeiro, Brazil. [Wilson, Don E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Moratelli, R (reprint author), Fundacao Oswaldo Cruz Rio de Janeiro, Campus Fiocruz Mata Atlantica,Estr Rodrigues Cald, BR-22713375 Rio De Janeiro, Brazil. EM rmoratelli@fiocruz.br; wilsond@si.edu RI Rocha, Ricardo/A-5735-2013 OI Rocha, Ricardo/0000-0003-0942-6633 FU Coordenacao de Aperfeicoamento de Pessoal de Ensino Superior (Ministerio da Educacao, Brazil); National Museum of Natural History; American Museum of Natural History FX The following curators and collection staff provided access to specimens under their care: Adriano L. Peracchi (Universidade Federal Rural do Rio de Janeiro, Brazil), Joao Alves de Oliveira, Stella M. Franco (Museu Nacional, Brazil), Fernando de C. Passos (Universidade Federal do Parana, Brazil), Teresa C. Margarido (Museu de Historia Natural Capao da lmbuia, Brazil), Mario de Vivo, Juliana Barros (Museu de Zoologia da Universidade de Sao Paulo, Brazil), Eliana Morielle-Versute (Universidade Estadual Paulista "Julio de Mesquita Filho", Brazil), Nancy Simmons, Eileen Westwig (American Museum of Natural History, USA), Linda Gordon (National Museum of Natural History, USA), Alfred Gardner (USGS Patuxent Wildlife Research Center, USA), and Patrick Bousses (Museum national d'Histoire naturelle, France). Nancy Simmons permitted the use of the images of the holotype. RM was partially supported by a scholarship from Coordenacao de Aperfeicoamento de Pessoal de Ensino Superior (Ministerio da Educacao, Brazil), and by Short-Term Visitor and Collection Study grants respectively from the National Museum of Natural History and the American Museum of Natural History. NR 15 TC 3 Z9 3 U1 2 U2 4 PU SOC BRASILEIRA ZOOLOGIA, UNIV FEDERAL PARANA PI CURITIBA PA CAIXA POSTAL 19020, CURITIBA, PARANA 81531-980, BRAZIL SN 1984-4670 J9 ZOOLOGIA-CURITIBA JI Zoologia PD FEB PY 2011 VL 28 IS 1 BP 115 EP 121 DI 10.1590/S1984-46702011000100016 PG 7 WC Zoology SC Zoology GA 734TE UT WOS:000288360400016 ER PT J AU Dick, MH Mawatari, SF Sanner, J Grischenko, AV AF Dick, Matthew H. Mawatari, Shunsuke F. Sanner, Joann Grischenko, Andrei V. TI Cribrimorph and Other Cauloramphus Species (Bryozoa: Cheilostomata) from the Northwestern Pacific SO ZOOLOGICAL SCIENCE LA English DT Article DE Bryozoa; Cauloramphus; Cheilostomata; disjunctus clade; dispersal; diversity; new species; phylogeny; speciation ID DIVERSITY; TAXONOMY AB We provide original descriptions for nine new species in the cheilostome bryozoan genus Cauloramphus (C. gracilis, C. ordinarius, C. amphidisjunctus, C. cheliferoides, C. oshurkovi, C. infensus, C. parvus, C. peltatus, and C. ascofer) and a redescription of C. disjunctus Canu and Bassler, 1929. We delineate a group of eight species, here termed the 'C. disjunctus clade,' that have the opesial spine joints calcified to a greater or lesser extent in mature zooids; most also have paired, hypertrophied avicularia. This group includes C. amphidisjunctus, C. cheliferoides, C. infensus, C. parvus, C. peltatus, and C. ascofer in the Aleutian Islands, Alaska; C. oshurkovi in the Commander Islands; and C. disjunctus in Japan. High levels of apparent endemism in two unrelated bryozoan genera (Cauloramphus and Monoporella), and geographical population differentiation in C. ascofer indicating ongoing allopatric speciation, suggest high speciation rates for deep benthic bryozoans in the western Aleutians. A phylogenetic hypothesis for the C. disjunctus clade indicates that populations of Cauloramphus dispersed between the Aleutians and Asia on at least three separate occasions, and that the polarity of at least two of these dispersal events was from the Aleutians to Asia. C1 [Dick, Matthew H.; Mawatari, Shunsuke F.] Hokkaido Univ, Dept Nat Hist Sci, Fac Sci, Sapporo, Hokkaido 0600810, Japan. [Sanner, Joann] Smithsonian Inst, Dept Paleobiol, NMNH, Washington, DC 20013 USA. [Grischenko, Andrei V.] Perm State Univ, Dept Invertebrate Zool & Aquat Ecol, Fac Biol, Perm 614900, Russia. RP Dick, MH (reprint author), Hokkaido Univ, Dept Nat Hist Sci, Fac Sci, N10 W8, Sapporo, Hokkaido 0600810, Japan. EM mhdick@mail.sci.hokudai.ac.jp RI Dick, Matthew/E-1327-2012 FU MEXT, Japan; MEXT [KAKENHI C 17570070] FX We thank Yoshinobu Nodasaka for making available SEM facilities, Paul Taylor for SEM images of fossil C. disjunctus, and Dennis Gordon for reviewing the manuscript. This study was supported in part by the COE Program 'Neo-Science of Natural History' funded by MEXT, Japan, and by a Grant-in-Aid (KAKENHI C 17570070) from MEXT to M.H.D. and S.F. M. The Alaska Fisheries Science Center supported collecting in the Aleutians. NR 24 TC 8 Z9 9 U1 0 U2 6 PU ZOOLOGICAL SOC JAPAN PI TOKYO PA TOSHIN-BUILDING, HONGO 2-27-2, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 0289-0003 J9 ZOOL SCI JI Zool. Sci. PD FEB PY 2011 VL 28 IS 2 BP 134 EP 147 DI 10.2108/zsj.28.134 PG 14 WC Zoology SC Zoology GA 711SL UT WOS:000286611600008 PM 21303206 ER PT J AU Angehr, GR AF Angehr, George R. TI Designation of a lectotype for Notiomystis cincta hautura Mathews, 1935 (Aves: Passeriformes: Meliphagidae) SO ZOOTAXA LA English DT Letter C1 Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Angehr, GR (reprint author), Smithsonian Trop Res Inst, Unit 9100,Box 0948, Miami, FL 34002 USA. EM angehrg@si.edu NR 3 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 FEB 1 PY 2011 IS 2754 BP 67 EP 68 PG 2 WC Zoology SC Zoology GA 715NZ UT WOS:000286892500006 ER PT J AU Gotzek, D Robertson, HM Wurm, Y Shoemaker, D AF Gotzek, Dietrich Robertson, Hugh M. Wurm, Yannick Shoemaker, DeWayne TI Odorant Binding Proteins of the Red Imported Fire Ant, Solenopsis invicta: An Example of the Problems Facing the Analysis of Widely Divergent Proteins SO PLOS ONE LA English DT Article ID AMINO-ACID SITES; DETECTING POSITIVE SELECTION; MULTIPLE SEQUENCE ALIGNMENT; LIKELIHOOD RATIO TESTS; CHEMOSENSORY PROTEINS; PHYLOGENETIC INFERENCE; SUBSTITUTION MODELS; MAXIMUM-LIKELIHOOD; GENOME ANNOTATION; GROUP HYMENOPTERA AB We describe the odorant binding proteins (OBPs) of the red imported fire ant, Solenopsis invicta, obtained from analyses of an EST library and separate 454 sequencing runs of two normalized cDNA libraries. We identified a total of 18 putative functional OBPs in this ant. A third of the fire ant OBPs are orthologs to honey bee OBPs. Another third of the OBPs belong to a lineage-specific expansion, which is a common feature of insect OBP evolution. Like other OBPs, the different fire ant OBPs share little sequence similarity (similar to 20%), rendering evolutionary analyses difficult. We discuss the resulting problems with sequence alignment, phylogenetic analysis, and tests of selection. As previously suggested, our results underscore the importance for careful exploration of the sensitivity to the effects of alignment methods for data comprising widely divergent sequences. C1 [Gotzek, Dietrich; Wurm, Yannick] Univ Lausanne, Dept Ecol & Evolut, Lausanne, Switzerland. [Robertson, Hugh M.] Univ Illinois, Dept Entomol, Urbana, IL USA. [Shoemaker, DeWayne] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL USA. RP Gotzek, D (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. EM gotzekd@si.edu RI Wurm, Yannick/A-9525-2009 OI Wurm, Yannick/0000-0002-3140-2809 FU USDA-AFRI FX Part of this study was funded by USDA-AFRI. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 72 TC 17 Z9 17 U1 2 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 31 PY 2011 VL 6 IS 1 AR e16289 DI 10.1371/journal.pone.0016289 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 714UK UT WOS:000286834300047 PM 21305009 ER PT J AU McMahon, SM Metcalf, CJE Woodall, CW AF McMahon, Sean M. Metcalf, Charlotte J. E. Woodall, Christopher W. TI High-Dimensional Coexistence of Temperate Tree Species: Functional Traits, Demographic Rates, Life-History Stages, and Their Physical Context SO PLOS ONE LA English DT Article ID NEOTROPICAL RAIN-FOREST; TRADE-OFFS; LONG-TERM; GROWTH; MORTALITY; CANOPY; RECRUITMENT; DIVERSITY; ABUNDANCE; PATTERNS AB Theoretical models indicate that trade-offs between growth and survival strategies of tree species can lead to coexistence across life history stages (ontogeny) and physical conditions experienced by individuals. There exist predicted physiological mechanisms regulating these trade-offs, such as an investment in leaf characters that may increase survival in stressful environments at the expense of investment in bole or root growth. Confirming these mechanisms, however, requires that potential environmental, ontogenetic, and trait influences are analyzed together. Here, we infer growth and mortality of tree species given size, site, and light characteristics from forest inventory data from Wisconsin to test hypotheses about growth-survival trade-offs given species functional trait values under different ontogenetic and environmental states. A series of regression analyses including traits and rates their interactions with environmental and ontogenetic stages supported the relationships between traits and vital rates expected from the expectations from tree physiology. A combined model including interactions between all variables indicated that relationships between demographic rates and functional traits supports growth-survival trade-offs and their differences across species in high-dimensional niche space. The combined model explained 65% of the variation in tree growth and supports a concept of community coexistence similar to Hutchinson's n-dimensional hypervolume and not a low-dimensional niche model or neutral model. C1 [McMahon, Sean M.] Smithsonian Environm Res Ctr, Ctr Trop Forest Sci, Smithsonian Trop Res Inst, Edgewater, MD 21037 USA. [Metcalf, Charlotte J. E.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Woodall, Christopher W.] US Forest Serv, St Paul, MN USA. RP McMahon, SM (reprint author), Smithsonian Environm Res Ctr, Ctr Trop Forest Sci, Smithsonian Trop Res Inst, POB 28, Edgewater, MD 21037 USA. EM mcmahons@si.edu OI Woodall, Christopher/0000-0001-8076-6214 FU HSBC through the Smithsonian Tropical Research Institute; Smithsonian Institution FX HSBC Climate Partnership partially funded the work of SMM as a recent postdoctoral fellowship awarded through the Smithsonian Tropical Research Institute. The funders (HSBC Bank) had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. The funding was through the Smithsonian Institution and has funded SMM's current postdoctoral position. This indirect support of SMM has no influence on the ability of the authors to follow all Plos ONE policies concerning data sharing and materials. There are no current external funding sources for this study. NR 36 TC 8 Z9 8 U1 1 U2 22 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 31 PY 2011 VL 6 IS 1 AR e16253 DI 10.1371/journal.pone.0016253 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 714UK UT WOS:000286834300046 PM 21305020 ER PT J AU Anlauf, H D'Croz, L O'Dea, A AF Anlauf, Holger D'Croz, Luis O'Dea, Aaron TI A corrosive concoction: The combined effects of ocean warming and acidification on the early growth of a stony coral are multiplicative SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Bleaching; Calcification; Planulae; Primary polyps; Settlement ID CALCIUM-CARBONATE SATURATION; NON-UPWELLING ENVIRONMENTS; CO2 PARTIAL-PRESSURE; GREAT-BARRIER-REEF; EL-NINO; SCLERACTINIAN CORAL; EASTERN PACIFIC; POCILLOPORA-DAMICORNIS; PORITES-ASTREOIDES; CALCIFICATION RATE AB Survival of coral planulae, and the successful settlement and healthy growth of primary polyps are critical for the dispersal of scleractinian corals and hence the recovery of degraded coral reefs. It is therefore important to explore how the warmer and more acidic oceanic conditions predicted for the future could affect these processes. This study used controlled culture to investigate the effects of a 1 degrees C increase in temperature and a 0.2-0.25 unit decrease in pH on the settlement and survival of planulae and the growth of primary polyps in the Tropical Eastern Pacific coral Porites panamensis. We found that primary polyp growth was reduced only marginally by more acidic seawater but the combined effect of high temperature and lowered pH caused a significant reduction in growth of primary polyps by almost a third. Elevated temperature was found to significantly reduce the amount of zooxanthellae in primary polyps, and when combined with lowered pH resulted in a significant reduction in biomass of primary polyps. However, survival and settlement of planula larvae were unaffected by increased temperature, lowered acidity or the combination of both. These results indicate that in future scenarios of increased temperature and oceanic acidity coral planulae will be able to disperse and settle successfully but primary polyp growth may be hampered. The recovery of reefs may therefore be impeded by global change even if local stressors are curbed and sufficient sources of planulae are available. (C) 2010 Elsevier B.V. All rights reserved. C1 [Anlauf, Holger; D'Croz, Luis; O'Dea, Aaron] Smithsonian Trop Res Inst, Panama City, Panama. [Anlauf, Holger] Leibniz Inst Balt Sea Res, D-18119 Rostock, Germany. [D'Croz, Luis] Univ Panama, Dept Biol Marina & Limnol, Estafeta Univ, Panama. RP Anlauf, H (reprint author), Seacol Germany eV, Kurfustendamm 217, D-10719 Berlin, Germany. EM hanlauf@gmail.com RI O'Dea, Aaron/D-4114-2011 FU German Academic Exchange Service; Smithsonian Tropical Research Institute (STRI) FX This project was funded by the German Academic Exchange Service and the Smithsonian Tropical Research Institute (STRI). Funding to O'Dea was provided by a STRI Tupper Fellowship. STRI also provided facilities and logistic support. Autoridad Nacional del Medio Ambiente (ANAM) granted permission for coral research in Panama. The support in experimental setup, field assistance, discussion, and enduring motivation of Bodo von Bodungen, Carlos Vega, Juan Del Rosario, John Cristy, Alexandra Amat and Carmen Schloeder are all greatly appreciated. We are also grateful to Rebecca Klaus, Christian Wild and the anonymous reviewers for their constructive criticism of the manuscript. [SS] NR 75 TC 62 Z9 63 U1 9 U2 125 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 JAN 31 PY 2011 VL 397 IS 1 BP 13 EP 20 DI 10.1016/j.jembe.2010.11.009 PG 8 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 718IB UT WOS:000287113400003 ER PT J AU Klein, M Hohensee, M Phillips, DF Walsworth, RL AF Klein, M. Hohensee, M. Phillips, D. F. Walsworth, R. L. TI Electromagnetically induced transparency in paraffin-coated vapor cells SO PHYSICAL REVIEW A LA English DT Article ID GROUP-VELOCITY; ATOMIC VAPOR; LIGHT; SLOW; ROTATION; STORAGE; GAS AB Antirelaxation coatings in atomic vapor cells allow ground-state coherent spin states to survive many collisions with the cell walls. This reduction in the ground-state decoherence rate gives rise to ultranarrow-bandwidth features in electromagnetically induced transparency (EIT) spectra, which can form the basis of, for example, long-time scale slow and stored light, sensitive magnetometers, and precise frequency standards. Here we study, both experimentally and theoretically, how Zeeman EIT contrast and width in paraffin-coated rubidium vapor cells are determined by cell and laser-beam geometry, laser intensity, and atomic density. Using a picture of Ramsey pulse sequences, where atoms alternately spend "bright" and "dark" time intervals inside and outside the laser beam, we explain the behavior of EIT features in coated cells, highlighting their unique characteristics and potential applications. C1 [Klein, M.; Hohensee, M.; Phillips, D. F.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Klein, M.; Hohensee, M.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Klein, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hohensee, Michael/0000-0002-8106-4502 NR 38 TC 25 Z9 26 U1 2 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JAN 31 PY 2011 VL 83 IS 1 AR 013826 DI 10.1103/PhysRevA.83.013826 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 713OL UT WOS:000286747200035 ER PT J AU Torres-Carvajal, O Etheridge, R De Queiroz, K AF Torres-Carvajal, Omar Etheridge, Richard De Queiroz, Kevin TI A systematic revision of Neotropical lizards in the clade Hoplocercinae (Squamata: Iguania) SO ZOOTAXA LA English DT Article DE Enyalioides; Hoplocercus; Iguanidae; lizards; Morunasaurus; Neotropics; taxonomy ID PHYLOGENETIC-RELATIONSHIPS; MORPHOLOGICAL DATA; TAXONOMY; REPTILIA; BRAZIL AB The clade Hoplocercinae includes 13 species assigned to three taxa traditionally ranked as genera-Enyalioides, Hoplocercus, and Morunasaurus-, and distributed on both sides of the Andes from Panama to Brazil. We provide a revised taxonomy of Hoplocercinae including synonymies, diagnoses, standardized descriptions, distributions, notes on color and natural history, and a key for species identification. We also propose vernacular names in English and Spanish for all species. C1 [Torres-Carvajal, Omar] Pontificia Univ Catolica Ecuador, Escuela Biol, Quito, Ecuador. [Etheridge, Richard] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Torres-Carvajal, Omar; De Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Torres-Carvajal, O (reprint author), Pontificia Univ Catolica Ecuador, Escuela Biol, Ave 12 Octubre & Roca,Apartado 17-01-2184, Quito, Ecuador. EM omartorcar@gmail.com; rether@sunstroke.sdsu.edu; dequeirozk@si.edu FU Systematics Association's; Smithsonian Institution; Secretaria Nacional de Ciencia y Tecnologia del Ecuador [PIC-08-0000470] FX For the loan of museum specimens we thank A. Almendariz (EPN), R. Casallas Lasso (MLS), J. E. Castillo and J. M. Renjifo (IAvH, IND-R), L. A. Coloma (QCAZ), J. Cordova (MHNSM), K. Garzon and J. Valencia (FHGO), J. Guibe (MHNP), J. Hanken and J. Rosado (MCZ), D. Kizirian and D. Frost (AMNH), J. D. Lynch (ICN), C. McCarthy (BMNH), A. Resetar and H. Voris (FMNH), L. Trueb (KU), J. Vindum (CAS, CAS-SUR), F. Werneck (CHUNB), M. Yanez-Munoz (DH-MECN). Special thanks to R. Langstroth for information on Bolivian locality data, T.C.S. Avila-Pires for various comments, M. Wilber from Georgetown University for help with some measurements and scale counts, and S. Baez for help with statistical analyses. This research was funded by The Systematics Association's Systematics Research Fund (OTC), a Restricted Endowment Award from the Smithsonian Institution (KdQ, OTC), and the Secretaria Nacional de Ciencia y Tecnologia del Ecuador (PIC-08-0000470, OTC). NR 93 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 31 PY 2011 IS 2753 BP 1 EP U74 PG 44 WC Zoology SC Zoology GA 712LS UT WOS:000286668900001 ER PT J AU Torres-Carvajal, O Etheridge, R De Queiroz, K AF Torres-Carvajal, Omar Etheridge, Richard De Queiroz, Kevin TI A systematic revision of Neotropical lizards in the clade Hoplocercinae (Squamata: Iguania) SO ZOOTAXA LA English DT Article DE Enyalioides; Hoplocercus; Iguanidae; lizards; Morunasaurus; Neotropics; taxonomy ID PHYLOGENETIC-RELATIONSHIPS; MORPHOLOGICAL DATA; TAXONOMY; REPTILIA; BRAZIL AB The clade Hoplocercinae includes 13 species assigned to three taxa traditionally ranked as genera-Enyalioides, Hoplocercus, and Morunasaurus-, and distributed on both sides of the Andes from Panama to Brazil. We provide a revised taxonomy of Hoplocercinae including synonymies, diagnoses, standardized descriptions, distributions, notes on color and natural history, and a key for species identification. We also propose vernacular names in English and Spanish for all species. C1 [Torres-Carvajal, Omar] Pontificia Univ Catolica Ecuador, Escuela Biol, Quito, Ecuador. [Etheridge, Richard] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Torres-Carvajal, Omar; De Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Torres-Carvajal, O (reprint author), Pontificia Univ Catolica Ecuador, Escuela Biol, Ave 12 Octubre y Roca,Apartado 17-01-2184, Quito, Ecuador. EM omartorcar@gmail.com; rether@sunstroke.sdsu.edu; dequeirozk@si.edu FU Systematics Association's Systematics Research Fund; Smithsonian Institution; Secretaria Nacional de Ciencia y Tecnologia del Ecuador [PIC-08-0000470] FX For the loan of museum specimens we thank A. Almendariz (EPN), R. Casallas Lasso (MLS), J. E. Castillo and J. M. Renjifo (IAvH, IND-R), L. A. Coloma (QCAZ), J. Cordova (MHNSM), K. Garzon and J. Valencia (FHGO), J. Guibe (MHNP), J. Hanken and J. Rosado (MCZ), D. Kizirian and D. Frost (AMNH), J. D. Lynch (ICN), C. McCarthy (BMNH), A. Resetar and H. Voris (FMNH), L. Trueb (KU), J. Vindum (CAS, CAS-SUR), F. Werneck (CHUNB), M. Yanez-Munoz (DH-MECN). Special thanks to R. Langstroth for information on Bolivian locality data, T. C. S. Avila-Pires for various comments, M. Wilber from Georgetown University for help with some measurements and scale counts, and S. Bacz for help with statistical analyses. This research was funded by The Systematics Association's Systematics Research Fund (OTC), a Restricted Endowment Award from the Smithsonian Institution (KdQ, OTC), and the Secretaria Nacional de Ciencia y Tecnologia del Ecuador (PIC-08-0000470, OTC). NR 93 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 31 PY 2011 IS 2752 BP 1 EP 44 PG 44 WC Zoology SC Zoology GA 712LQ UT WOS:000286668700001 ER PT J AU Collins, AG Bentlage, B Gillan, W Lynn, TH Morandini, AC Marques, AC AF Collins, Allen G. Bentlage, Bastian Gillan, William (Bud) Lynn, Tara H. Morandini, Andre C. Marques, Antonio C. TI Naming the Bonaire banded box jelly, Tamoya ohboya, n. sp. (Cnidaria: Cubozoa: Carybdeida: Tamoyidae) SO ZOOTAXA LA English DT Article DE nematocysts; cnidome; stings; citizen science; taxonomic impediment ID MOLECULAR EVIDENCE; IMPEDIMENT; NEMATOCYST; SCYPHOZOA; TAXONOMY; MORBAKKA; PATTERNS AB A new species of cubozoan jellyfish has been discovered in shallow waters of Bonaire, Netherlands ( Dutch Caribbean). Thus far, approximately 50 sightings of the species, known commonly as the Bonaire banded box jelly, are recorded, and three specimens have been collected. Three physical encounters between humans and the species have been reported. Available evidence suggests that a serious sting is inflicted by this medusa. To increase awareness of the scientific disciplines of systematics and taxonomy, the public has been involved in naming this new species. The Bonaire banded box jelly, Tamoya ohboya, n. sp., can be distinguished from its close relatives T. haplonema from Brazil and T. sp. from the southeastern United States by differences in tentacle coloration, cnidome, and mitochondrial gene sequences. Tamoya ohboya n. sp. possesses striking dark brown to reddish-orange banded tentacles, nematocyst warts that densely cover the animal, and a deep stomach. We provide a detailed comparison of nematocyst data from Tamoya ohboya n. sp., T. haplonema from Brazil, and T. sp. from the Gulf of Mexico. C1 [Collins, Allen G.; Bentlage, Bastian; Lynn, Tara H.] NOAAs Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA. [Collins, Allen G.; Bentlage, Bastian; Lynn, Tara H.] Smithsonian Inst, Natl Museum Nat Hist, MRC 153, Washington, DC 20013 USA. [Bentlage, Bastian] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Gillan, William (Bud)] Boynton Beach Community High Sch, Palm Beach Cty FL Sch, Boynton Beach, FL 33426 USA. [Morandini, Andre C.; Marques, Antonio C.] Univ Sao Paulo, Inst Biociencias, Dept Zool, BR-05508090 Sao Paulo, Brazil. RP Collins, AG (reprint author), NOAAs Natl Marine Fisheries Serv, Natl Systemat Lab, POB 37012, Washington, DC 20013 USA. EM collinsa@si.edu; bentlage@ku.edu; gillanw@palmbeach.k12.fl.us; thtinlynn@gmail.com; acmorand@usp.br; marques@ib.usp.br RI Collins, Allen/A-7944-2008; Marques, Antonio/E-8049-2011; Morandini, Andre/A-9892-2012 OI Collins, Allen/0000-0002-3664-9691; Marques, Antonio/0000-0002-2884-0541; Morandini, Andre/0000-0003-3747-8748 FU Department of the Interior U.S. Geological Survey [05HQAG0009, 05099HS004]; US National Science Foundation [0531779]; CNPq [490158/2009-9]; FAPESP [2010/50174-7] FX We thank Vicki Carr for initiating this research by sharing video and a description of the Bonaire banded box jelly in 2001, all of the many other citizen scientists who have shared their encounters with the BBJ, Johan van Blerk for collecting the first examined specimen of Tamoya ohboya n. sp., Jake Richter (from Bonaire) for outstanding photography, blogging, and communications about the Bonaire banded box jelly over several years, Ramone DeLeon (Director, STINAPA - Bonaire Marine Park) for research, scientific, and technical assistance, Frank van Slobbe (Sr. Executive, DROB/The Netherlands Ministry of the Environment), for research, governmental, and technical assistance, as well as Tice Dace and Dr. Pauline Keyes (both from Bonaire) for communications and technical assistance, and Sabrina Baroni (USP) for technical assistance. We are grateful to Jennifer Collins for the idea of involving the public in naming a species and for highlighting this work through COPUS and the 2009 Year of Science celebration. Rob Wilson is acknowledged for his able help in generating molecular sequence data as part of the National Systematics Laboratory's barcoding efforts. We also thank M. Nizinski for providing the specimen of Tamoya sp. from the Gulf of Mexico, collection of which was supported by the Department of the Interior U.S. Geological Survey under Cooperative Agreement No. 05HQAG0009, sub-agreement 05099HS004. The comments, suggestions, and observations of two referees greatly improved an earlier version of this paper. We thank Dale Calder for agreeing to handle the editing of this manuscript without the specific name of the new species of Tamoya being fully determined, and for being patient. This work is part of the US National Science Foundation Assembling the Tree of Life grant 0531779 (to AGC, P. Cartwright, and D. Fautin). ACMorandini was partly funded by CNPq (490158/2009-9) and FAPESP (2010/50174-7) and ACMarques by CNPq, CAPES, Fundacao O Boticario, and FAPESP. NR 30 TC 12 Z9 15 U1 0 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 31 PY 2011 IS 2753 BP 53 EP 68 PG 16 WC Zoology SC Zoology GA 712LS UT WOS:000286668900003 ER PT J AU Sterenborg, MG Cohen, O Drake, JJ Gombosi, TI AF Sterenborg, M. Glenn Cohen, O. Drake, J. J. Gombosi, T. I. TI Modeling the young Sun's solar wind and its interaction with Earth's paleomagnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID STELLAR CORONAL ABUNDANCES; MASS-LOSS RATES; DENSITY DIAGNOSTICS; MAGNETIC-FIELDS; ALPHA-CENTAURI; EMISSION-LINES; FE XI; EVOLUTION; TIME; STARS AB We present a focused parameter study of solar wind-magnetosphere interaction for the young Sun and Earth, similar to 3.5 Gyr ago, that relies on magnetohydrodynamic (MHD) simulations for both the solar wind and the magnetosphere. By simulating the quiescent young Sun and its wind we are able to propagate the MHD simulations up to Earth's magnetosphere and obtain a physically realistic solar forcing of it. We assess how sensitive the young solar wind is to changes in the coronal base density, sunspot placement and magnetic field strength, dipole magnetic field strength, and the Sun's rotation period. From this analysis we obtain a range of plausible solar wind conditions to which the paleomagnetosphere may have been subject. Scaling relationships from the literature suggest that a young Sun would have had a mass flux different from the present Sun. We evaluate how the mass flux changes with the aforementioned factors and determine the importance of this and several other key solar and magnetospheric variables with respect to their impact on the paleomagnetosphere. We vary the solar wind speed, density, interplanetary magnetic field strength, and orientation as well as Earth's dipole magnetic field strength and tilt in a number of steady state scenarios that are representative of young Sun-Earth interaction. This study is done as a first step of a more comprehensive effort toward understanding the implications of Sun-Earth interaction for planetary atmospheric evolution. C1 [Sterenborg, M. Glenn] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Cohen, O.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gombosi, T. I.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Sterenborg, MG (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM mgsteren@fas.harvard.edu RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215 FU SHINE through NSF [ATM-0823592]; NASA [NAS8-39073]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI; Harvard FAS Sciences Division Research Computing Group FX We are grateful to Dimitar Sasselov, Itay Halevy, and Alex Glocer for insightful discussions. O.C. is supported by SHINE through NSF grant ATM-0823592. J.J.D. was funded by NASA contract NAS8-39073 to the Chandra X-ray Center. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. The GM computations in this paper were run on the Odyssey cluster supported by the Harvard FAS Sciences Division Research Computing Group. NR 56 TC 16 Z9 16 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JAN 29 PY 2011 VL 116 AR A01217 DI 10.1029/2010JA016036 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 713VG UT WOS:000286764900002 ER PT J AU Sperhake, U Berti, E Cardoso, V Pretorius, F Yunes, N AF Sperhake, Ulrich Berti, Emanuele Cardoso, Vitor Pretorius, Frans Yunes, Nicolas TI Superkicks in ultrarelativistic encounters of spinning black holes SO PHYSICAL REVIEW D LA English DT Article ID NUMERICAL RELATIVITY; INITIAL DATA AB We study ultrarelativistic encounters of two spinning, equal-mass black holes through simulations in full numerical relativity. Two initial data sequences are studied in detail: one that leads to scattering and one that leads to a grazing collision and merger. In all cases, the initial black hole spins lie in the orbital plane, a configuration that leads to the so-called superkicks. In astrophysical, quasicircular inspirals, such kicks can be as large as similar to 3000 km/s; here, we find configurations that exceed similar to 15 000 km/s. We find that the maximum recoil is to a good approximation proportional to the total amount of energy radiated in gravitational waves, but largely independent of whether a merger occurs or not. This shows that the mechanism predominantly responsible for the superkick is not related to merger dynamics. Rather, a consistent explanation is that the "bobbing'' motion of the orbit causes an asymmetric beaming of the radiation produced by the in-plane orbital motion of the binary, and the net asymmetry is balanced by a recoil. We use our results to formulate some conjectures on the ultimate kick achievable in any black hole encounter. C1 [Sperhake, Ulrich] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, E-08193 Barcelona, Spain. [Sperhake, Ulrich; Berti, Emanuele] CALTECH, Pasadena, CA 91125 USA. [Sperhake, Ulrich; Berti, Emanuele; Cardoso, Vitor] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Cardoso, Vitor] Univ Tecn Lisboa, Inst Super Tecn, Dept Fis, CENTRA, P-1049 Lisbon, Portugal. [Pretorius, Frans; Yunes, Nicolas] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Yunes, Nicolas] MIT, Dept Phys, Cambridge, MA 02139 USA. [Yunes, Nicolas] MIT Kavli Inst, Cambridge, MA 02139 USA. [Yunes, Nicolas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sperhake, U (reprint author), Fac Ciencies, Inst Ciencies Espai CSIC IEEC, Campus UAB, E-08193 Barcelona, Spain. RI Berti, Emanuele/C-9331-2016; Cardoso, Vitor/K-1877-2015 OI Berti, Emanuele/0000-0003-0751-5130; Cardoso, Vitor/0000-0003-0553-0433 FU Ministry of Education and Science of Spain; NSF [PHY-0601459, PHY-0652995, PHY-0900735, PHY-0745779]; Fairchild Foundation to Caltech; Alfred P. Sloan Foundation; ERC [DyBHo-256667]; FCT-Portugal [PTDC/FIS/098025/2008, PTDC/FIS/098032/2008, PTDC/CTE-AST/098034/2008, CERN/FP/109306/2009, CERN/FP/109290/2009, loni_numrel05]; TeraGrid Advanced Support Program [PHY-090003]; Centro de Supercomputacion de Galicia (CESGA_ [ICTS-2009-40]; National Aeronautics and Space Administration [PF0-110080, NAS8-03060] FX We thank Pablo Laguna for useful discussions. U. S. acknowledges support from the Ramon y Cajal Programme of the Ministry of Education and Science of Spain, NSF Grants No. PHY-0601459, PHY-0652995, and the Fairchild Foundation to Caltech. E. B.'s research was supported by NSF Grant No. PHY-0900735. V. C. is supported by a "Ciencia 2007'' research contract. F. P. and N. Y. acknowledge support from NSF Grant No. PHY-0745779, and the Alfred P. Sloan Foundation (F. P.). This work was partially supported by the DyBHo-256667 ERC Starting Grant, by FCT-Portugal through Projects No. PTDC/FIS/098025/2008, PTDC/FIS/098032/2008, PTDC/CTE-AST/098034/2008, CERN/FP/109306/2009, CERN/FP/109290/2009, loni_numrel05, an allocation through the TeraGrid Advanced Support Program under Grant No. PHY-090003 on NICS' kraken cluster and the Centro de Supercomputacion de Galicia (CESGA, Project No. ICTS-2009-40). Computations were partially performed on the Woodhen Cluster at Princeton University. N. Y. acknowledges support from the National Aeronautics and Space Administration through Einstein Postdoctoral Fellowship Award Number PF0-110080 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under Contract No. NAS8-03060. The authors thankfully acknowledge the computer resources, technical expertise, and assistance provided by the Barcelona Supercomputing Centre, Centro Nacional de Supercomputacion. NR 41 TC 17 Z9 17 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JAN 28 PY 2011 VL 83 IS 2 AR 024037 DI 10.1103/PhysRevD.83.024037 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 714JC UT WOS:000286804900003 ER PT J AU Hoorn, C Wesselingh, FP Ter Steege, H Bermudez, MA Mora, A Sevink, J Sanmartin, I Sanchez-Meseguer, A Anderson, CL Figueiredo, JP Jaramillo, C Riff, D Negri, FR Hooghiemstra, H Lundberg, J Stadler, T Sarkinen, T Antonelli, A AF Hoorn, C. Wesselingh, F. P. Ter Steege, H. Bermudez, M. A. Mora, A. Sevink, J. Sanmartin, I. Sanchez-Meseguer, A. Anderson, C. L. Figueiredo, J. P. Jaramillo, C. Riff, D. Negri, F. R. Hooghiemstra, H. Lundberg, J. Stadler, T. Saerkinen, T. Antonelli, A. TI Origins of Biodiversity Response SO SCIENCE LA English DT Letter ID MOLECULAR PHYLOGENIES; EXTINCTION RATES; DIVERSIFICATION; SPECIATION C1 [Antonelli, A.] Gothenburg Bot Garden, S-41349 Gothenburg, Sweden. [Hoorn, C.; Sevink, J.; Hooghiemstra, H.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1098 XH Amsterdam, Netherlands. [Wesselingh, F. P.] Nederlands Ctr Biodiversiteit Nat, NL-2300 RA Leiden, Netherlands. [Ter Steege, H.] Univ Utrecht, Fac Sci, Dept Biol, Inst Environm Biol, NL-3584 CH Utrecht, Netherlands. [Bermudez, M. A.] Cent Univ Venezuela, Fac Ingn, Escuela Geol Minas & Geofis, Lab Termocronol & Geomatemat, Caracas 1053, Venezuela. [Mora, A.] Inst Colombiano Petr, ECOPETROL, Piedecuesta, Santander, Colombia. [Sanmartin, I.; Sanchez-Meseguer, A.; Anderson, C. L.] CSIC, E-28014 Madrid, Spain. [Figueiredo, J. P.] Petr Brasileiro SA Petrobras, BR-20031170 Rio De Janeiro, Brazil. [Jaramillo, C.] Smithsonian Trop Res Inst, Balboa, Panama. [Riff, D.] Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. [Negri, F. R.] Univ Fed Acre, Lab Paleontol, BR-69980000 Acre, AC, Brazil. [Lundberg, J.] Acad Nat Sci, Dept Ichthyol, Philadelphia, PA 19103 USA. [Stadler, T.] Swiss Fed Inst Technol, Inst Integrat Biol, CH-8092 Zurich, Switzerland. [Saerkinen, T.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Antonelli, A.] Univ Gothenburg, Dept Plant & Environm Sci, S-41349 Gothenburg, Sweden. RP Antonelli, A (reprint author), Gothenburg Bot Garden, Carl Skottsbergs Gata 22A, S-41349 Gothenburg, Sweden. EM alexandre.antonelli@vgregion.se RI Riff, Douglas/B-5183-2012; ter Steege, Amaz/B-5866-2011; Stadler, Tanja/J-4742-2013; Sanmartin, Isabel/G-3131-2015 OI Riff, Douglas/0000-0003-0805-2828; ter Steege, Amaz/0000-0002-8738-2659; Stadler, Tanja/0000-0001-6431-535X; Sanmartin, Isabel/0000-0001-6104-9658 NR 9 TC 12 Z9 14 U1 2 U2 22 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 28 PY 2011 VL 331 IS 6016 BP 399 EP 400 DI 10.1126/science.331.6016.399 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 712BB UT WOS:000286635900027 ER PT J AU Bovino, S Zhang, P Gianturco, FA Dalgarno, A Kharchenko, V AF Bovino, S. Zhang, P. Gianturco, F. A. Dalgarno, A. Kharchenko, V. TI Energy transfer in O collisions with He isotopes and Helium escape from Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID FAST NITROGEN-ATOMS; HOT OXYGEN; DISSOCIATIVE RECOMBINATION; NOBLE-GASES; DISTRIBUTIONS; THERMALIZATION; ATMOSPHERE; EVOLUTION; CORONA; VENUS AB Accurate data on energy-transfer collisions between hot oxygen atoms and the atmospheric helium gas on Mars, are reported. Anisotropic cross sections for elastic collisions of O((3)P) and O((1)D) atoms with helium gas have been calculated quantum mechanically and found to be surprisingly similar. Cross sections, computed for collisions with both helium isotopes, (3)He and (4)He, have been used to construct the kernel of the Boltzmann equation describing the energy relaxation of hot oxygen atoms. Computed rates of energy transfer in O+He collisions have been used to evaluate the flux of He atoms escaping from the Mars atmosphere. Atmospheric layers mostly responsible for production of the He escape flux are identified. Our results demonstrate that strong angular anisotropy of scattering cross sections increases the collisional ejection of light atoms and is critical in the evaluation of He escape from Mars, Venus and Earth. Citation: Bovino, S., P. Zhang, F. A. Gianturco, A. Dalgarno, and V. Kharchenko (2011), Energy transfer in O collisions with He isotopes and Helium escape from Mars, Geophys. Res. Lett., 38, L02203, doi: 10.1029/2010GL045763. C1 [Bovino, S.; Gianturco, F. A.] Univ Roma La Sapienza, Dept Chem, I-00185 Rome, Italy. [Zhang, P.; Dalgarno, A.; Kharchenko, V.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT USA. RP Bovino, S (reprint author), Univ Roma La Sapienza, Dept Chem, Ple A Moro 5, I-00185 Rome, Italy. EM sbovino@caspur.it; pezhang@cfa.harvard.edu; fa.gianturco@caspur.it; adalgarno@cfa.harvard.edu; vkharchenko@cfa.harvard.edu FU NASA [NNX09AF13G, NNX10AB88G]; U.S. Department of Energy FX For this research, V.K. was supported by NASA grants NNX09AF13G and NNX10AB88G, A.D. and P.Z. by U.S. Department of Energy and F.A.G. by the PRIN 2006 national project. S.B. thanks ITAMP visitor program. The computational support from NASA supercomputing center is also acknowledged. NR 33 TC 9 Z9 9 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JAN 26 PY 2011 VL 38 AR L02203 DI 10.1029/2010GL045763 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 713TE UT WOS:000286759500003 ER PT J AU Brown, JW Segura, R Santiago-Jimenez, Q Rota, J Heard, TA AF Brown, John W. Segura, Ricardo Santiago-Jimenez, Quiyari Rota, Jadranka Heard, Tim A. TI Tortricid moths reared from the invasive weed Mexican palo verde, Parkinsonia aculeata, with comments on their host specificity, biology, geographic distribution, and systematics SO JOURNAL OF INSECT SCIENCE LA English DT Article DE Australia; Amorbia; biological control; Cochylis; DNA sequences; host plants; Neotropics; Ofatulena; Playtnota; Rudenia; taxonomy ID LEPIDOPTERA AB As part of efforts to identify native herbivores of Mexican palo verde, Parkinsonia aculeata L. (Leguminosae: Caesalpinioideae), as potential biological control agents against this invasive weed in Australia, ten species of Tortricidae (Lepidoptera) were reared from Guatemala, Mexico, Nicaragua, and Venezuela: Amorbia concavana (Zeller), Platynota rostrana (Walker), Platynota helianthes (Meyrick), Platynota stultana Walsingham (all Tortricinae: Sparganothini), Rudenia leguminana (Busck), Cochylis sp. (both Tortricinae: Cochylini), Ofatulena duodecemstriata (Walsingham), O. luminosa Heinrich, Ofatulena sp. (all Olethreutinae: Grapholitini), and Crocidosema lantana Busck (Olethreutinae: Eucosmini). Significant geographic range extensions are provided for O. duodecemstriata and R. leguminana. These are the first documented records of P. aculeata as a host plant for all but O. luminosa. The four species of Sparganothini are polyphagous; in contrast, the two Cochylini and three Grapholitini likely are specialists on Leguminosae. Ofatulena luminosa is possibly host specific on P. aculeata. Host trials with Rudenia leguminana also provide some evidence of specificity, in contrast to historical rearing records. To examine the possibility that R. leguminana is a complex of species, two data sets of molecular markers were examined: (1) a combined data set of two mitochondrial markers (a 781-basepair region of cytochrome c oxidase I (COI) and a 685-basepair region of cytochrome c oxidase II) and one nuclear marker (a 531-basepair region of the 28S domain 2); and (2) the 650-basepair "barcode" region of COI. Analyses of both data sets strongly suggest that individuals examined in this study belong to more than one species. C1 [Brown, John W.] ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist, Washington, DC 20013 USA. [Segura, Ricardo; Santiago-Jimenez, Quiyari] CSIRO Ecosyst Sci, Mexican Field Stn, Boca Del Rio 94297, Veracruz, Mexico. [Rota, Jadranka] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Heard, Tim A.] CSIRO Ecosyst Sci, Brisbane, Qld, Australia. RP Brown, JW (reprint author), ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist, Washington, DC 20013 USA. EM john.brown@ars.usda.gov; csiromfs@prodigy.net.mx; quiyari@hotmail.com; jadranka.rota@gmail.com; tim.heard@csiro.au RI Rota, Jadranka/C-6702-2011; Heard, Tim/B-1125-2008 OI Rota, Jadranka/0000-0003-0220-3920; Heard, Tim/0000-0003-4975-7314 FU Australian Government Department of Agriculture, Fisheries and Forestry FX We thank Moises Martinez and Carlos Pascacio (both CSIRO) for assistance with field work in Mexico. Diane Hartley (CSIRO) provided sequence data. The following provided helpful reviews of the manuscript: Natalia Vandenberg and Thomas Henry, Systematic Entomology Laboratory, U.S. Department of Agricultural, National Museum of Natural History, Washington, D.C.; and John Heppner, Florida State Collection of Arthropods, Gainesville, Florida. The Australian Government Department of Agriculture, Fisheries and Forestry provided financial support. NR 41 TC 1 Z9 1 U1 4 U2 10 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1536-2442 EI 2250-2645 J9 J INSECT SCI JI J Insect Sci. PD JAN 24 PY 2011 VL 11 AR 7 PG 17 WC Entomology SC Entomology GA 710NQ UT WOS:000286518900001 PM 21521138 ER PT J AU Watters, TR Thomas, PC Robinson, MS AF Watters, Thomas R. Thomas, Peter C. Robinson, Mark S. TI Thrust faults and the near-surface strength of asteroid 433 Eros SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SMALL-SCALE FEATURES; LASER ALTIMETRY; 433-EROS; SHOEMAKER; TOPOGRAPHY; SHAPE; IMPACT AB NEAR Shoemaker images reveal widespread occurrence of tectonic landforms on asteroid 433 Eros. Hinks Dorsum is a ridge that extends for about 18 km around the asteroid and strongly resembles thrust fault structures on the terrestrial planets. Tectonic landforms can provide information on the mechanical properties of asteroids, a subject of much controversy. Modeling constrained by topographic data shows that Hinks Dorsum can be accounted for by a shallow rooted thrust fault no greater than 250 m in depth with similar to 90 m of cumulative slip. Strength envelopes based on frictional and rock mass strength criteria suggest the near-surface shear strength of Eros is from similar to 1 to 6 MPa. A spatial correlation is found between Shoemaker crater, a transition from low to high crater density, and Hinks Dorsum. This spatial relation along with the estimated strength of the asteroid suggests the thrust fault was formed by impact induced compression. Citation: Watters, T. R., P. C. Thomas, and M. S. Robinson (2011), Thrust faults and the near-surface strength of asteroid 433 Eros, Geophys. Res. Lett., 38, L02202, doi:10.1029/2010GL045302. C1 [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Thomas, Peter C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu FU National Aeronautics and Space Administration FX We thank the two anonymous reviewers for helpful comments that improved the manuscript. This work is supported by the National Aeronautics and Space Administration under grants issued through the Office of the Planetary Geology and Geophysics Program. NR 35 TC 6 Z9 6 U1 0 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 JAN 22 PY 2011 VL 38 AR L02202 DI 10.1029/2010GL045302 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 710NA UT WOS:000286517300001 ER PT J AU McCarthy, MC Gottlieb, CA Thaddeus, P Thorwirth, S Gauss, J AF McCarthy, Michael C. Gottlieb, Carl A. Thaddeus, Patrick Thorwirth, Sven Gauss, Juergen TI Rotational spectra and equilibrium structures of H2SiS and Si2S SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; COUPLED-CLUSTER THEORY; GAUSSIAN-BASIS SETS; AB-INITIO; 2ND DERIVATIVES; CARBON CHAINS; LINE SURVEY; MANY-BODY; PERTURBATION; SPECTROSCOPY AB The rotational spectra of two small silicon sulfides, silanethione H2SiS and the disilicon sulfide ring Si2S, have been detected in the centimeter band by Fourier transform microwave spectroscopy of a molecular beam; lines of H2SiS were also observed in the millimeter band up to 377 GHz in a glow discharge. Precise rotational and centrifugal distortionconstants have been determined for the normal and a number of the more abundant rare isotopic species of both closed-shell molecules. Theoretical equilibrium (r(e)) structures of H2SiS and Si2S were derived from coupled-cluster calculations that included triple and quadruple excitations, core correlation, and extrapolation to the basis-set limit. The r(e) structures agree to within 5 x 10(-4) angstrom and 0.1 degrees with empirical equilibrium (r(e)(emp)) structures derived from the experimental rotational constants, combined with theoretical vibrational and electronic corrections. Both H2SiS and Si2S are good candidates for radioastronomical detection in the circumstellar shells of evolved carbon-rich stars such as IRC+10216, because they are fairly polar and are similar in composition to the abundant astronomical molecule SiS. (C) 2011 American Institute of Physics. [doi:10.1063/1.3510732] C1 [McCarthy, Michael C.; Gottlieb, Carl A.; Thaddeus, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, Michael C.; Gottlieb, Carl A.; Thaddeus, Patrick] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Thorwirth, Sven] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Thorwirth, Sven] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Gauss, Juergen] Johannes Gutenberg Univ Mainz, Inst Phys Chem, D-55099 Mainz, Germany. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu; sthorwirth@ph1.uni-koeln.de; gauss@uni-mainz.de RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-0701204]; NASA [NNX08AE05G]; Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-1, GA 370/5-1]; Fonds der Chemischen Industrie FX We thank J. F. Stanton for helpful discussions and H. Gupta for communicating preliminary theoretical results. The work in Cambridge is supported by NSF Grant No. CHE-0701204 and NASA Grant No. NNX08AE05G. S.T. is grateful to the Deutsche Forschungsgemeinschaft (DFG) for financial support through Grant No. TH 1301/3-1, and J.G. acknowledges support from the Deutsche Forschungsgemeinschaft (GA 370/5-1) and the Fonds der Chemischen Industrie. NR 58 TC 11 Z9 11 U1 0 U2 10 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JAN 21 PY 2011 VL 134 IS 3 AR 034306 DI 10.1063/1.3510732 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 709WN UT WOS:000286472200032 PM 21261352 ER PT J AU Beerer, IM Knutson, HA Burrows, A Fortney, JJ Agol, E Charbonneau, D Cowan, NB Deming, D Desert, JM Langton, J Laughlin, G Lewis, NK Showman, AP AF Beerer, Ingrid M. Knutson, Heather A. Burrows, Adam Fortney, Jonathan J. Agol, Eric Charbonneau, David Cowan, Nicolas B. Deming, Drake Desert, Jean-Michel Langton, Jonathan Laughlin, Gregory Lewis, Nikole K. Showman, Adam P. TI SECONDARY ECLIPSE PHOTOMETRY OF WASP-4b WITH WARM SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; stars: individual (WASP-4b); techniques: photometric ID INFRARED-EMISSION SPECTRUM; PLANET HD 189733B; TRANSITING GIANT PLANETS; GROUND-BASED DETECTION; THERMAL EMISSION; EXTRASOLAR PLANET; HOT JUPITERS; TEMPERATURE INVERSION; MODEL ATMOSPHERES; BAND EMISSION AB We present photometry of the giant extrasolar planet WASP-4b at 3.6 and 4.5 mu m taken with the Infrared Array Camera on board the Spitzer Space Telescope as part of Spitzer's extended warm mission. We find secondary eclipse depths of 0.319% +/- 0.031% and 0.343% +/- 0.027% for the 3.6 and 4.5 mu m bands, respectively, and show model emission spectra and pressure-temperature profiles for the planetary atmosphere. These eclipse depths are well fit by model emission spectra with water and other molecules in absorption, similar to those used for TrES-3 and HD 189733b. Depending on our choice of model, these results indicate that this planet has either a weak dayside temperature inversion or no inversion at all. The absence of a strong thermal inversion on this highly irradiated planet is contrary to the idea that highly irradiated planets are expected to have inversions, perhaps due the presence of an unknown absorber in the upper atmosphere. This result might be explained by the modestly enhanced activity level of WASP-4b's G7V host star, which could increase the amount of UV flux received by the planet, therefore reducing the abundance of the unknown stratospheric absorber in the planetary atmosphere as suggested in Knutson et al. We also find no evidence for an offset in the timing of the secondary eclipse and place a 2 sigma upper limit on vertical bar e cos omega vertical bar of 0.0024, which constrains the range of tidal heating models that could explain this planet's inflated radius. C1 [Beerer, Ingrid M.; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Agol, Eric; Cowan, Nicolas B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Charbonneau, David; Desert, Jean-Michel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. [Lewis, Nikole K.; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Beerer, IM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Charbonneau, David/0000-0002-9003-484X FU NASA; Miller Institute for Basic Research Science; NSF [0645416] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Support for this work was provided by NASA. Heather A. Knutson is supported by a fellowship from the Miller Institute for Basic Research Science. Eric Agol acknowledges the support of NSF CAREER grant No. 0645416. NR 60 TC 32 Z9 32 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 23 DI 10.1088/0004-637X/727/1/23 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000023 ER PT J AU Kraft, RP Forman, WR Jones, C Nulsen, PEJ Hardcastle, MJ Raychaudhury, S Evans, DA Sivakoff, GR Sarazin, CL AF Kraft, R. P. Forman, W. R. Jones, C. Nulsen, P. E. J. Hardcastle, M. J. Raychaudhury, S. Evans, D. A. Sivakoff, G. R. Sarazin, C. L. TI THE GAS DYNAMICS OF NGC 4472 REVEALED BY XMM-NEWTON SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4472); galaxies: jets; hydrodynamics; X-rays: galaxies ID EARLY-TYPE GALAXIES; DEEP CHANDRA OBSERVATION; HOT INTERSTELLAR-MEDIUM; GIANT ELLIPTIC GALAXY; EMISSION-LINE REGION; X-RAY EVIDENCE; VIRGO CLUSTER; COOLING FLOWS; DARK-MATTER; INTRACLUSTER MEDIUM AB We present results from a 100 ks XMM-Newton observation of the hot gas in the Virgo cluster elliptical galaxy NGC 4472. We find a surface brightness discontinuity similar to 21 kpc north of the nucleus, consistent with being a contact discontinuity between two moving fluids. We also detect a >60 kpc long ram-pressure stripped tail. The pressure across the discontinuity implies an infall velocity, v(infall), of 1000 km s(-1) < v(infall) < 2200 km s(-1) depending on what assumptions are made about the density and pressure of the external gas. We suggest that the NGC 4472 group is falling into a collapsing filament, which is itself falling into the Virgo cluster. The gas of a collapsing filament is rapidly decelerated as it crosses the standoff shock, but the apparent high velocity of infall for NGC 4472 could be simply due to the fact that the gravitating potential of the NGC 4472 group is unaffected by this shock. While the group falls through the shock its gas will be stripped as it passes through the stalled gas of the filament. Additionally, we find two sets of cool filamentary arms to the east and the southwest of the nucleus. One of the southwest arms is coincident with a sharp filament seen with Chandra. We interpret these arms as filaments of cool gas that have been driven out from the center of the galaxy by the buoyant evolution of a radio bubble. The age of this outburst is similar to 10(8) yr assuming that the buoyant bubble rises with a velocity of similar to 0.4c(s) = 200 km s(-1); the energy of the outburst is a modest similar to 2 x 10(56) erg. C1 [Kraft, R. P.; Forman, W. R.; Jones, C.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Evans, D. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Sivakoff, G. R.; Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 4, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; Sivakoff, Gregory/G-9602-2011; OI Hardcastle, Martin/0000-0003-4223-1117; Sivakoff, Gregory/0000-0001-6682-916X; Nulsen, Paul/0000-0003-0297-4493 FU NASA [NAS8-03060]; Chandra X-ray Center; Smithsonian Astrophysical Observatory; Royal Society FX This work was supported by NASA contract NAS8-03060, the Chandra X-ray Center, and the Smithsonian Astrophysical Observatory. M.J.H. thanks the Royal Society for a research fellowship. We would also like to thank the anonymous referee for comments that improved this paper. NR 71 TC 24 Z9 24 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 JAN 20 PY 2011 VL 727 IS 1 AR 41 DI 10.1088/0004-637X/727/1/41 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000041 ER PT J AU Melnick, GJ Tolls, V Snell, RL Bergin, EA Hollenbach, DJ Kaufman, MJ Li, D Neufeld, DA AF Melnick, Gary J. Tolls, Volker Snell, Ronald L. Bergin, Edwin A. Hollenbach, David J. Kaufman, Michael J. Li, Di Neufeld, David A. TI DISTRIBUTION OF WATER VAPOR IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; radio lines: ISM ID WAVE-ASTRONOMY-SATELLITE; DENSE INTERSTELLAR CLOUDS; C-12/C-13 ISOTOPE RATIO; SPITZER-SPACE-TELESCOPE; MASS STAR-FORMATION; CHEMICAL-MODELS; DARK CLOUD; IC 5146; ORION; EMISSION AB We report the results of a large-area study of water vapor along the Orion Molecular Cloud ridge, the purpose of which was to determine the depth-dependent distribution of gas-phase water in dense molecular clouds. We find that the water vapor measured toward 77 spatial positions along the face-on Orion ridge, excluding positions surrounding the outflow associated with BN/KL and IRc2, display integrated intensities that correlate strongly with known cloud surface tracers such as CN, C2H, (CO)-C-13 J = 5-4, and HCN, and less well with the volume tracer N2H+. Moreover, at total column densities corresponding to A(V) < 15 mag, the ratio of H2O to (CO)-O-18 integrated intensities shows a clear rise approaching the cloud surface. We show that this behavior cannot be accounted for by either optical depth or excitation effects, but suggests that gas-phase water abundances fall at large AV. These results are important as they affect measures of the true water-vapor abundance in molecular clouds by highlighting the limitations of comparing measured water-vapor column densities with such traditional cloud tracers as (CO)-C-13 or (CO)-O-18. These results also support cloud models that incorporate freeze out of molecules as a critical component in determining the depth-dependent abundance of water vapor. C1 [Melnick, Gary J.; Tolls, Volker] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Snell, Ronald L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hollenbach, David J.] SETI Inst, Mountain View, CA 94043 USA. [Kaufman, Michael J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Li, Di] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gmelnick@cfa.harvard.edu; vtolls@cfa.harvard.edu; snell@astro.umass.edu; ebergin@umich.edu; dhollenbach@seti.org; mkaufman@email.sjsu.edu; dili@jpl.nasa.gov; neufeld@pha.jhu.edu FU Long Term Space Astrophysics (LTSA) [NNG06GB30G]; NSF [AST 08-38222] FX G.J.M., R.L.S., E.A.B., D.J.H., and M.J.K. gratefully acknowledge the financial support of NASA grant NNG06GB30G from the Long Term Space Astrophysics (LTSA) Research Program. The Five College Radio Astronomy Observatory was operated with support from the NSF through grant AST 08-38222. NR 71 TC 7 Z9 7 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 13 DI 10.1088/0004-637X/727/1/13 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000013 ER PT J AU Shinnaga, H Young, KH Tilanus, RPJ Chamberlin, R Gurwell, MA Wilner, D Hughes, AM Yoshida, H Peng, RS Force, B Friberg, P Bottinelli, S Van Dishoeck, EF Phillips, TG AF Shinnaga, Hiroko Young, Ken H. Tilanus, Remo P. J. Chamberlin, Richard Gurwell, Mark A. Wilner, David Hughes, A. Meredith Yoshida, Hiroshige Peng, Ruisheng Force, Brian Friberg, Per Bottinelli, Sandrine Van Dishoeck, Ewine F. Phillips, Thomas G. TI IRC+10216'S INNERMOST ENVELOPE-THE eSMA'S VIEW (vol 698, pg 1924, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction ID EXCITED VIBRATIONAL-STATES; WAVE SPECTROSCOPY; HCN C1 [Shinnaga, Hiroko; Chamberlin, Richard; Yoshida, Hiroshige; Peng, Ruisheng; Force, Brian; Phillips, Thomas G.] CALTECH, Submillimeter Observ CSO, Hilo, HI 96720 USA. [Young, Ken H.; Gurwell, Mark A.; Wilner, David; Hughes, A. Meredith] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tilanus, Remo P. J.; Friberg, Per] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, Remo P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Bottinelli, Sandrine; Van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Shinnaga, H (reprint author), CALTECH, Submillimeter Observ CSO, 111 Nowelo St, Hilo, HI 96720 USA. EM shinnaga@submm.caltech.edu NR 3 TC 0 Z9 0 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 60 DI 10.1088/0004-637X/727/1/60 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000060 ER PT J AU Massaro, F Grindlay, JE AF Massaro, F. Grindlay, J. E. TI SPECTRAL EVOLUTION OF LONG GAMMA-RAY BURST PROMPT EMISSION: ELECTROSTATIC ACCELERATION AND ADIABATIC EXPANSION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; gamma-ray burst: general; radiation mechanisms: non-thermal ID PARTICLE-ACCELERATION; BATSE; CATALOG; PULSES; ENERGY; BEPPOSAX; FIELD; BAND AB Despite the great variation in the light curves of gamma-ray burst (GRB) prompt emission, their spectral energy distribution (SED) is generally curved and broadly peaked. In particular, their spectral evolution is well described by the hardness-intensity correlation during a single pulse decay phase, when the SED peak height S-p decreases as its peak energy E-p decreases. We propose an acceleration scenario, based on electrostatic acceleration, to interpret the E-p distribution peak at similar to 0.25 MeV. We show that during the decay phase of individual pulses in the long GRB light curve, the adiabatic expansion losses likely dominate the synchrotron cooling effects. The energy loss as due to adiabatic expansion can also be used to describe the spectral evolution observed during their decay phase. The spectral evolution predicted by our scenario is consistent with that observed in single pulses of long BATSE GRBs. C1 [Massaro, F.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Massaro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Massaro, Francesco/L-9102-2016 OI Massaro, Francesco/0000-0002-1704-9850 FU Foundation BLANCEFLOR Boncompagni-Ludovisi, n'ee Bildt; NASA [NNX10AD50G] FX F.M. is grateful to R. Preece for comments to the manuscript. He also thanks M. Petrera, A. Cavaliere, and A. Paggi for helpful suggestions on the acceleration mechanisms. Finally, he is grateful to M. Salvati for providing useful suggestions that helped us to improve the presentation. F.M. acknowledges the Foundation BLANCEFLOR Boncompagni-Ludovisi, n'ee Bildt for the grant awarded him in 2010. His work at SAO is also supported by NASA grant NNX10AD50G. NR 28 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2011 VL 727 IS 1 AR L1 DI 10.1088/2041-8205/727/1/L1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703QG UT WOS:000285993800001 ER PT J AU Perets, HB AF Perets, Hagai B. TI BINARY PLANETESIMALS AND THEIR ROLE IN PLANET FORMATION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE minor planets, asteroids: general; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: physical evolution; protoplanetary disks ID KUIPER-BELT BINARIES; LOW-MASS INTRUDERS; DYNAMICAL EVOLUTION; MINOR PLANETS; GLOBULAR-CLUSTERS; HARD BINARIES; OBJECTS; ENCOUNTERS; ASTEROIDS; STARS AB One of the main evolutionary stages of planet formation is the dynamical evolution of planetesimal disks. These disks are thought to evolve through gravitational encounters and physical collisions between single planetesimals. In recent years, many binary planetesimals (BPs) have been observed in the solar system, indicating that the binarity of planetesimals is high. However, current studies of planetesimal disk formation and evolution do not account for the role of binaries. Here, we point out that gravitational encounters of BPs can have an important role in the evolution of planetesimal disks. BPs catalyze close encounters between planetesimals and can strongly enhance their collision rate. Binaries may also serve as an additional heating source of the planetesimal disk, through the exchange of the binaries gravitational potential energy into the kinetic energy of planetesimals in the disk. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hperets@cfa.harvard.edu RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X NR 38 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2011 VL 727 IS 1 AR L3 DI 10.1088/2041-8205/727/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703QG UT WOS:000285993800003 ER PT J AU Irwin, J Berta, ZK Burke, CJ Charbonneau, D Nutzman, P West, AA Falco, EE AF Irwin, Jonathan Berta, Zachory K. Burke, Christopher J. Charbonneau, David Nutzman, Philip West, Andrew A. Falco, Emilio E. TI ON THE ANGULAR MOMENTUM EVOLUTION OF FULLY CONVECTIVE STARS: ROTATION PERIODS FOR FIELD M-DWARFS FROM THE MEarth TRANSIT SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; stars: evolution; stars: low-mass; stars: rotation; starspots ID LOW-MASS STARS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; SCALE MAGNETIC TOPOLOGIES; ORION NEBULA CLUSTER; GUIDANCE SENSOR 3; T-TAURI STARS; STELLAR ROTATION; MONITOR PROJECT; BROWN DWARFS AB We present rotation period measurements for 41 field M-dwarfs, all of which have masses inferred (from their parallaxes and Two Micron All Sky Survey K-band magnitudes) to be between the hydrogen burning limit and 0.35 M-circle dot and thus should remain fully convective throughout their lifetimes. We measure a wide range of rotation periods, from 0.28 to 154 days, with the latter commensurate with the typical sensitivity limit of our observations. Using kinematics as a proxy for age, we find that the majority of objects likely to be thick disk or halo members (and hence, on average, older) rotate very slowly, with a median period of 92 days, compared with 0.7 days for those likely to be thin disk members (on average, younger), although there are still some rapid rotators in the thick disk sample. When combined with literature measurements for M-dwarfs, these results indicate an increase in spin-down times with decreasing stellar mass, in agreement with previous work, and that the spin-down time becomes comparable to the age of the thick disk sample below the fully convective boundary. We additionally infer that the spin-down must remove a substantial amount of angular momentum once it begins in order to produce the slow rotators we observe in the thick disk candidates, suggesting that fully convective M-dwarfs may still experience strong winds. C1 [Irwin, Jonathan; Berta, Zachory K.; Burke, Christopher J.; Charbonneau, David; Nutzman, Philip] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [West, Andrew A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Falco, Emilio E.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Irwin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jirwin@cfa.harvard.edu RI West, Andrew/H-3717-2014; OI Berta-Thompson, Zachory/0000-0002-3321-4924; Charbonneau, David/0000-0002-9003-484X FU David and Lucile Packard Fellowship for Science and Engineering; National Science Foundation [AST-0807690]; NASA; NSF; NASA's Astrophysics Data System (ADS) FX The MEarth team gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based upon work supported by the National Science Foundation under grant number AST-0807690. We thank Saurav Dhital for computing the Galactic model results along the sight lines to our M-dwarfs, Isabelle Baraffe for providing the stellar evolution model tracks used in Section 5.2 and for discussion of the location of the fully convective boundary as a function of time, and Jerome Bouvier, Marc Pinsonneault, and Alexander Scholz for assistance with the rotational evolution models and for helpful discussions regarding the interpretation. The anonymous referee is also thanked for a helpful report that significantly improved the manuscript. The MEarth team is greatly indebted to the staff at the Fred Lawrence Whipple Observatory for their efforts in construction and maintenance of the facility and thank Wayne Peters, Ted Groner, Karen Erdman-Myres, Grace Alegria, Rodger Harris, Bob Hutchins, Dave Martina, Dennis Jankovsky, and Tom Welsh for their support.; This research has made extensive use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF, NASA's Astrophysics Data System (ADS), and the SIMBAD database, operated at CDS, Strasbourg, France. NR 89 TC 108 Z9 108 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 56 DI 10.1088/0004-637X/727/1/56 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000056 ER PT J AU Kilic, M Brown, WR Prieto, CA Agueros, MA Heinke, C Kenyon, SJ AF Kilic, Mukremin Brown, Warren R. Allende Prieto, Carlos Agueeros, M. A. Heinke, Craig Kenyon, S. J. TI THE ELM SURVEY. II. TWELVE BINARY WHITE DWARF MERGER SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: low-mass; white dwarfs ID DIGITAL SKY SURVEY; EXTREMELY LOW-MASS; SPY PROJECT; NLTT 11748; SPECTROPHOTOMETRIC STANDARDS; MILLISECOND PULSARS; SDSS 1257+5428; IA SUPERNOVAE; NEUTRON-STAR; WILL MERGE AB We describe newradial velocity and X-ray observations of extremely low-masswhite dwarfs (ELM WDs, similar to 0.2 M-circle dot) in the Sloan Digital Sky Survey Data Release 4 and the MMT Hypervelocity Star survey. We identify four new short period binaries, including two merger systems. These observations bring the total number of short period binary systems identified in our survey to 20. No main-sequence or neutron star companions are visible in the available optical photometry, radio, and X-ray data. Thus, the companions are most likely WDs. Twelve of these systems will merge within a Hubble time due to gravitational wave radiation. We have now tripled the number of known merging WD systems. We discuss the characteristics of this merger sample and potential links to underluminous supernovae, extreme helium stars, AM CVn systems, and other merger products. We provide new observational tests of the WD mass-period distribution and cooling models for ELM WDs. We also find evidence for a new formation channel for single low-mass WDs through binary mergers of two lower mass objects. C1 [Kilic, Mukremin; Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Agueeros, M. A.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Heinke, Craig] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu RI Agueros, Marcel/K-7998-2014; OI Agueros, Marcel/0000-0001-7077-3664; Kenyon, Scott/0000-0003-0214-609X; Heinke, Craig/0000-0003-3944-6109 FU NASA; Caltech FX We thank G. Nelemans for providing his binary WD population synthesis model results, S. Geier for the latest results from the SPY survey, and D. Koester for WD model spectra. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. NR 68 TC 66 Z9 66 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 3 DI 10.1088/0004-637X/727/1/3 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000003 ER PT J AU Kuo, CY Braatz, JA Condon, JJ Impellizzeri, CMV Lo, KY Zaw, I Schenker, M Henkel, C Reid, MJ Greene, JE AF Kuo, C. Y. Braatz, J. A. Condon, J. J. Impellizzeri, C. M. V. Lo, K. Y. Zaw, I. Schenker, M. Henkel, C. Reid, M. J. Greene, J. E. TI THE MEGAMASER COSMOLOGY PROJECT. III. ACCURATE MASSES OF SEVEN SUPERMASSIVE BLACK HOLES IN ACTIVE GALAXIES WITH CIRCUMNUCLEAR MEGAMASER DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: ISM; galaxies: nuclei; galaxies: Seyfert ID WATER MASER EMISSION; X-RAY-ABSORPTION; GALACTIC NUCLEI; SEYFERT-GALAXIES; ACCRETION DISK; GEOMETRIC DISTANCE; CIRCINUS GALAXY; HUBBLE CONSTANT; INTRINSIC SCATTER; SPIRAL STRUCTURE AB Observations of H2O masers from circumnuclear disks in active galaxies for the Megamaser Cosmology Project (MCP) allow accurate measurement of the mass of supermassive black holes (BH) in these galaxies. We present the Very Long Baseline Interferometry images and kinematics of water maser emission in six active galaxies: NGC 1194, NGC 2273, NGC 2960 (Mrk 1419), NGC 4388, NGC 6264 and NGC 6323. We use the Keplerian rotation curves of these six megamaser galaxies, plus a seventh previously published, to determine accurate enclosed masses within the central similar to 0.3 pc of these galaxies, smaller than the radius of the sphere of influence of the central mass in all cases. We also set lower limits to the central mass densities of between 0.12 x 10(10) and 61 x 10(10) M-circle dot pc(-3). For six of the seven disks, the high central densities rule out clusters of stars or stellar remnants as the central objects, and this result further supports our assumption that the enclosed mass can be attributed predominantly to a supermassive BH. The seven BHs have masses ranging between 0.75 x 10(7) and 6.5 x 10(7) M-circle dot, with the mass errors dominated by the uncertainty of the Hubble constant. We compare the megamaser BH mass determination with BH mass measured from the virial estimation method. The virial estimation BH mass in four galaxies is consistent with the megamaser BH mass, but the virial mass uncertainty is much greater. Circumnuclear megamaser disks allow the best mass determination of the central BH mass in external galaxies and significantly improve the observational basis at the low-mass end of the M-sigma(star) relation. The M-sigma(star) relation may not be a single, low-scatter power law as originally proposed. MCP observations continue and we expect to obtain more maser BH masses in the future. C1 [Kuo, C. Y.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Braatz, J. A.; Condon, J. J.; Impellizzeri, C. M. V.; Lo, K. Y.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Zaw, I.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Zaw, I.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Schenker, M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Greene, J. E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Kuo, CY (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. FU Associated Universities, Inc. FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank Ed Fomalont for his kind help with our VLBI data reduction and Lincoln Greenhill for his substantial assistance for this project. C.Y.K. thanks Mark Whittle for his numerous insightful comments on our project. This research has made use of NASA's Astrophysics Data System Bibliographic Services, and the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 64 TC 84 Z9 84 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 20 DI 10.1088/0004-637X/727/1/20 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000020 ER PT J AU McNamara, BR Rohanizadegan, M Nulsen, PEJ AF McNamara, B. R. Rohanizadegan, Mina Nulsen, P. E. J. TI ARE RADIO ACTIVE GALACTIC NUCLEI POWERED BY ACCRETION OR BLACK HOLE SPIN? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: jets; galaxies: nuclei; X-rays: galaxies: clusters ID BRIGHTEST CLUSTER GALAXIES; COLD MOLECULAR GAS; ADVECTION-DOMINATED ACCRETION; ENERGETIC AGN OUTBURST; COOLING FLOW CLUSTERS; ELLIPTIC GALAXIES; JET POWER; ELECTROMAGNETIC EXTRACTION; INFRARED SURVEY; RAY CORRELATION AB We compare accretion and black hole spin as potential energy sources for outbursts from active galactic nuclei (AGNs) in brightest cluster galaxies (BCGs). Based on our adopted spin model, we find that the distribution of AGN power estimated from X-ray cavities is consistent with a broad range of both spin parameters and accretion rates. Sufficient quantities of molecular gas are available in most BCGs to power their AGNs by accretion alone. However, we find no correlation between AGN power and molecular gas mass over the range of jet power considered here. For a given AGN power, the BCG's gas mass and accretion efficiency, defined as the fraction of the available cold molecular gas that is required to power the AGN, both vary by more than two orders of magnitude. Most of the molecular gas in BCGs is apparently consumed by star formation or is driven out of the nucleus by the AGN before it reaches the nuclear black hole. Bondi accretion from hot atmospheres is generally unable to fuel powerful AGNs, unless their black holes are more massive than their bulge luminosities imply. We identify several powerful AGNs that reside in relatively gas-poor galaxies, indicating an unusually efficient mode of accretion, or that their AGNs are powered by another mechanism. If these systems are powered primarily by black hole spin rather than by accretion, spin must also be tapped efficiently in some systems, i.e., P-jet > (M) over dotc(2), or their black hole masses must be substantially larger than the values implied by their bulge luminosities. We constrain the (model-dependent) accretion rate at the transition from radiatively inefficient to radiatively efficient accretion flows to be a few percent of the Eddington rate, a value that is consistent with other estimates. C1 [McNamara, B. R.; Rohanizadegan, Mina] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McNamara, BR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. OI Nulsen, Paul/0000-0003-0297-4493 FU Natural Sciences and Engineering Research Council of Canada FX We thank M. Ruszkowski, D. Evans, and A. Babul for good suggestions. This research was supported in part by a generous grant from the Natural Sciences and Engineering Research Council of Canada. NR 66 TC 54 Z9 54 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 JAN 20 PY 2011 VL 727 IS 1 AR 39 DI 10.1088/0004-637X/727/1/39 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000039 ER PT J AU Mosleh, M Williams, RJ Franx, M Kriek, M AF Mosleh, Moein Williams, Rik J. Franx, Marijn Kriek, Mariska TI THE EVOLUTION OF THE MASS-SIZE RELATION TO z=3.5 FOR UV-BRIGHT GALAXIES AND SUBMILLIMETER GALAXIES IN THE GOODS-NORTH FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: structure ID STAR-FORMING GALAXIES; COMPACT QUIESCENT GALAXIES; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; ULTRA-DEEP-FIELD; ELLIPTIC GALAXIES; LUMINOSITY FUNCTION; PASSIVE GALAXIES; DISK GALAXIES; SPECTROSCOPIC SURVEY AB We study the evolution of the size-stellar mass relation for a large spectroscopic sample of galaxies in the GOODS-North field up to z similar to 3.5. The sizes of the galaxies are measured from K-s-band images (corresponding to rest-frame optical/NIR) from the Subaru 8 m telescope. We reproduce earlier results based on photometric redshifts that the sizes of galaxies at a given mass evolve with redshift. Specifically, we compare sizes of UV-bright galaxies at a range of redshifts: Lyman-break galaxies (LBGs) selected through the U-drop technique (z similar to 2.5-3.5), BM/BX galaxies at z similar to 1.5-2.5, and GALEX LBGs at low redshift (z similar to 0.6-1.5). The median sizes of these UV-bright galaxies evolve as (1 + z)(-1.11 +/- 0.13) between z similar to 0.5 and 3.5. The UV-bright galaxies are significantly larger than quiescent galaxies at the same mass and redshift by 0.45 +/- 0.09 dex. We also verify the correlation between color and stellar mass density of galaxies to high redshifts. The sizes of submillimeter galaxies in the same field are measured and compared with BM/BX galaxies. We find that the median half-light radius of SMGs is 2.90 +/- 0.45 kpc, and there is little difference in their size distribution to the UV-bright star-forming galaxies. C1 [Mosleh, Moein; Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Williams, Rik J.] Carnegie Observ, Pasadena, CA 91101 USA. [Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mosleh, M (reprint author), Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. EM mosleh@strw.leidenuniv.nl FU European Commission, Marie Curie Initial Training Network ELIXIR (Early unIverse eXploration with nIRspec) [PITN-GA-2008-214227]; Nederlandse Onderzoekschool voor Astronomie (NOVA); NSF [AST-0707417] FX We thank the anonymous referee for helpful comments and suggestions. We thank Rychard Bouwens for providing us K-band images. M.M. is supported by the Marie Curie Initial Training Network ELIXIR (Early unIverse eXploration with nIRspec), grant agreemnet PITN-GA-2008-214227 (from the European Commission). R.J.W. acknowledges support from the Nederlandse Onderzoekschool voor Astronomie (NOVA) and NSF grant AST-0707417. NR 63 TC 38 Z9 39 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 5 DI 10.1088/0004-637X/727/1/5 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000005 ER PT J AU Torres, G Fressin, F Batalha, NM Borucki, WJ Brown, TM Bryson, ST Buchhave, LA Charbonneau, D Ciardi, DR Dunham, EW Fabrycky, DC Ford, EB Gautier, TN Gilliland, RL Holman, MJ Howell, SB Isaacson, H Jenkins, JM Koch, DG Latham, DW Lissauer, JJ Marcy, GW Monet, DG Prsa, A Quinn, SN Ragozzine, D Rowe, JF Sasselov, DD Steffen, JH Welsh, WF AF Torres, Guillermo Fressin, Francois Batalha, Natalie M. Borucki, William J. Brown, Timothy M. Bryson, Stephen T. Buchhave, Lars A. Charbonneau, David Ciardi, David R. Dunham, Edward W. Fabrycky, Daniel C. Ford, Eric B. Gautier, Thomas N., III Gilliland, Ronald L. Holman, Matthew J. Howell, Steve B. Isaacson, Howard Jenkins, Jon M. Koch, David G. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Monet, David G. Prsa, Andrej Quinn, Samuel N. Ragozzine, Darin Rowe, Jason F. Sasselov, Dimitar D. Steffen, Jason H. Welsh, William F. TI MODELING KEPLER TRANSIT LIGHT CURVES AS FALSE POSITIVES: REJECTION OF BLEND SCENARIOS FOR KEPLER-9, AND VALIDATION OF KEPLER-9 d, A SUPER-EARTH-SIZE PLANET IN A MULTIPLE SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; planetary systems; stars: individual (Kepler-9, KIC 3323887, KOI-377); stars: statistics ID STAR; CANDIDATES; MASS; PARAMETERS; EVOLUTION AB Light curves from the Kepler Mission contain valuable information on the nature of the phenomena producing the transit-like signals. To assist in exploring the possibility that they are due to an astrophysical false positive, we describe a procedure (BLENDER) to model the photometry in terms of a "blend" rather than a planet orbiting a star. A blend may consist of a background or foreground eclipsing binary (or star-planet pair) whose eclipses are attenuated by the light of the candidate and possibly other stars within the photometric aperture. We apply BLENDER to the case of Kepler-9 (KIC 3323887), a target harboring two previously confirmed Saturn-size planets (Kepler-9 b and Kepler-9 c) showing transit timing variations, and an additional shallower signal with a 1.59 day period suggesting the presence of a super-Earth-size planet. Using BLENDER together with constraints from other follow-up observations we are able to rule out all blends for the two deeper signals and provide independent validation of their planetary nature. For the shallower signal, we rule out a large fraction of the false positives that might mimic the transits. The false alarm rate for remaining blends depends in part (and inversely) on the unknown frequency of small-size planets. Based on several realistic estimates of this frequency, we conclude with very high confidence that this small signal is due to a super-Earth-size planet (Kepler-9 d) in a multiple system, rather than a false positive. The radius is determined to be 1.64(-0.14)(+0.19) R-circle plus, and current spectroscopic observations are as yet insufficient to establish its mass. C1 [Torres, Guillermo; Fressin, Francois; Charbonneau, David; Fabrycky, Daniel C.; Holman, Matthew J.; Latham, David W.; Quinn, Samuel N.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Borucki, William J.; Bryson, Stephen T.; Koch, David G.; Lissauer, Jack J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Isaacson, Howard] San Francisco State Univ, San Francisco, CA 94132 USA. [Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Monet, David G.] USN, Observ, Flagstaff, AZ 86001 USA. [Prsa, Andrej] Villanova Univ, Villanova, PA 19085 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu RI Ragozzine, Darin/C-4926-2013; OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We are grateful to Leo Girardi for computing isochrones for this work in the Kepler passband, to Frederic Pont for very helpful discussions on false alarm probabilities, and to David Sing for advice on limb-darkening coefficients. We also thank the anonymous referee for insightful comments on the original version of this paper. NR 44 TC 117 Z9 119 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2011 VL 727 IS 1 AR 24 DI 10.1088/0004-637X/727/1/24 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703PT UT WOS:000285992000024 ER PT J AU Munoz-Jaramillo, A Nandy, D Martens, PCH AF Munoz-Jaramillo, Andres Nandy, Dibyendu Martens, Petrus C. H. TI MAGNETIC QUENCHING OF TURBULENT DIFFUSIVITY: RECONCILING MIXING-LENGTH THEORY ESTIMATES WITH KINEMATIC DYNAMO MODELS OF THE SOLAR CYCLE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: dynamo; Sun: interior ID FLUX-TRANSPORT DYNAMO; FULL-SPHERE SIMULATIONS; MERIDIONAL FLOW; PARITY ISSUE; CONVECTION; TACHOCLINE; REGIONS; MECHANISM; SHEAR; FIELD AB The turbulent magnetic diffusivity in the solar convection zone is one of the most poorly constrained ingredients of mean-field dynamo models. This lack of constraint has previously led to controversy regarding the most appropriate set of parameters, as different assumptions on the value of turbulent diffusivity lead to radically different solar cycle predictions. Typically, the dynamo community uses double-step diffusivity profiles characterized by low values of diffusivity in the bulk of the convection zone. However, these low diffusivity values are not consistent with theoretical estimates based on mixing-length theory, which suggest much higher values for turbulent diffusivity. To make matters worse, kinematic dynamo simulations cannot yield sustainable magnetic cycles using these theoretical estimates. In this work, we show that magnetic cycles become viable if we combine the theoretically estimated diffusivity profile with magnetic quenching of the diffusivity. Furthermore, we find that the main features of this solution can be reproduced by a dynamo simulation using a prescribed (kinematic) diffusivity profile that is based on the spatiotemporal geometric average of the dynamically quenched diffusivity. This bridges the gap between dynamically quenched and kinematic dynamo models, supporting their usage as viable tools for understanding the solar magnetic cycle. C1 [Munoz-Jaramillo, Andres; Martens, Petrus C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Munoz-Jaramillo, Andres; Martens, Petrus C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nandy, Dibyendu] Indian Inst Sci Educ & Res, Mohampur 741252, W Bengal, India. RP Munoz-Jaramillo, A (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM amunoz@cfa.harvard.edu; dnandi@iiserkol.ac.in; martens@solar.physics.montana.edu OI Munoz-Jaramillo, Andres/0000-0002-4716-0840 FU NASA [NNG05GE47G]; Government of India FX We are grateful to Dana Longcope and Paul Charbonneau for vital discussions during the development of this work. We thank Jorgen Christensen-Dalsgaard for providing us with Solar Model S data and useful counsel regarding its use. We also thank anonymous referees for very thorough reviews which led to an overall improvement of this Letter. The computations required for this work were performed using the resources of Montana State University and the Harvard-Smithsonian Center for Astrophysics. We thank Keiji Yoshimura at MSU, and Alisdair Davey and Henry (Trae) Winter at the CfA for much appreciated technical support. This research was funded by NASA Living With a Star grant NNG05GE47G and has made extensive use of NASA's Astrophysics Data System. D.N. acknowledges support from the Government of India through the Ramanujan Fellowship. NR 37 TC 16 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2011 VL 727 IS 1 AR L23 DI 10.1088/2041-8205/727/1/L23 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 703QG UT WOS:000285993800023 ER PT J AU Harasewych, MG AF Harasewych, M. G. TI The Living Columbariinae (Gastropoda: Neogastropoda: Turbinellidae) of New Zealand SO ZOOTAXA LA English DT Article DE Neogastropoda; Turbinellidae; Columbariinae; Columbarium; Coluzea; Fulgurofusus; bathyal; new species; biogeography; New Zealand ID PSYCHROSPHERE AB The Columbariinae have been represented in the fauna of New Zealand from the Paleocene until the Recent, providing the longest known continuous record for the subfamily. Seven living species, representing the genera Columbarium, Coluzea, and Fulgurofusus, are recognized, and include two species, Fulgurofusus maxwelli and Fulgurofusus marshalli that are described as new. The New Zealand columbariine fauna is unusually diverse at the generic level, and includes the largest members of the subfamily, as well as the only primarily sublittoral species. The morphology, anatomy, and distribution of the living species are discussed, as are their relationships to living and fossil congeners. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM HARASEWYCH@si.edu NR 85 TC 0 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 JAN 19 PY 2011 IS 2744 BP 1 EP 33 PG 33 WC Zoology SC Zoology GA 707ZX UT WOS:000286331200001 ER PT J AU Kassi, S Leshchishina, O Gordon, IE Yu, SS Campargue, A AF Kassi, Samir Leshchishina, Olga Gordon, Iouli E. Yu, Shanshan Campargue, Alain TI Hyperfine structure of the a(1)Delta(g) - X-3 Sigma(-)(g) transitions of (OO)-O-16-O-17, (OO)-O-17-O-18 and O-17(2) by CRDS at 80 K SO CHEMICAL PHYSICS LETTERS LA English DT Article ID CAVITY RINGDOWN SPECTROSCOPY; 1.5 MU-M; RESONANCE-SPECTRUM; ISOTOPOLOGUES; OXYGEN AB The high sensitivity absorption spectrum of the a(1)Delta(g) - X-3 Sigma(-)(g) band of O-16(17), (OO)-O-17-O-18 and O-17(2) has been recorded by CW-Cavity Ring Down Spectroscopy near 1.27 mu m. The spectra were obtained between 7640 and 7917 cm (1) with a O-17-enriched sample at room temperature and at 80 K. Due to the I = 5/2 nuclear spin of the O-17 atom, the nuclear hyperfine structure of the transitions could be partly resolved at low temperature. The parameter coupling of the nuclear spin to the electronic angular momentum in the a(1)Delta(g) state has been derived for the three studied isotopologues of oxygen. (C) 2010 Elsevier B.V. All rights reserved. C1 [Kassi, Samir; Leshchishina, Olga; Campargue, Alain] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. [Leshchishina, Olga] Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia. [Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Campargue, A (reprint author), Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. EM Alain.CAMPARGUE@ujf-grenoble.fr RI Yu, Shanshan/D-8733-2016 FU ANR [NT09_436466]; National Aeronautics and Space Administration FX Part of this work was performed at Grenoble University under the ANR project 'IDEO' (NT09_436466). A portion of this research was performed at Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 21 TC 5 Z9 5 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 EI 1873-4448 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD JAN 18 PY 2011 VL 502 IS 1-3 BP 37 EP 41 DI 10.1016/j.cplett.2010.12.017 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 703PY UT WOS:000285992600005 ER PT J AU Kiers, ET Denison, RF Kawakita, A Herre, EA AF Kiers, E. Toby Denison, R. Ford Kawakita, Atsushi Herre, Edward Allen TI The biological reality of host sanctions and partner fidelity SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID MUTUALISM C1 [Kiers, E. Toby] Vrije Univ Amsterdam, Inst Ecol Sci, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. [Denison, R. Ford] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Kawakita, Atsushi] Kyoto Univ, Ctr Ecol Res, Shiga 5202113, Japan. [Herre, Edward Allen] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Kiers, ET (reprint author), Vrije Univ Amsterdam, Inst Ecol Sci, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. EM ekiers@falw.vu.nl NR 5 TC 14 Z9 14 U1 4 U2 39 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 18 PY 2011 VL 108 IS 3 BP E7 EP E7 DI 10.1073/pnas.1014546108 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 707TF UT WOS:000286310300001 PM 21220350 ER PT J AU Zhao, L Duan, WH Yelin, SF AF Zhao, L. Duan, Wenhui Yelin, S. F. TI All-optical Fresnel lens in coherent media: controlling image with image SO OPTICS EXPRESS LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; LIQUID-CRYSTAL; DIFFRACTIVE LENS; DESORPTION AB We theoretically explore an all-optical method for generating tunable diffractive Fresnel lenses in coherent media based on electromagnetically induced transparency. In this method, intensity-modulated images in coupling light fields can pattern the coherent media to induce the desired modulo-2 pi quadratic phase profiles for the lenses to diffract probe light fields. We characterize the focusing and imaging properties of the induced lenses. In particular, we show that the images in coupling fields can flexibly control the images in probe fields by diffraction, where large focal length tunability from 1 m to infinity and high output (similar to 88% diffraction efficiency) can be achieved. Additionally, we also find that the induced Fresnel lenses can be rapidly modulated with megahertz refresh rates using image-bearing square pulse trains in coupling fields. Our proposed lenses may find a wide range of applications for multimode all-optical signal processing in both the classical and quantum regimes. (C) 2011 Optical Society of America C1 [Zhao, L.; Duan, Wenhui] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Zhao, L (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM zhaol@phys.tsinghua.edu.cn RI Duan, Wenhui /H-4992-2011 OI Duan, Wenhui /0000-0001-9685-2547 FU Ministry of Science and Technology of China [2011CB921901, 2011CB606405]; China Postdoctoral Science Foundation [20100470362]; NSF [PHY-0970055] FX L.Z. thanks R. Zhou and F. Peng for helpful discussions. L.Z. and W.D. acknowledge the financial support from the Ministry of Science and Technology of China (Grants No. 2011CB921901 and 2011CB606405) and China Postdoctoral Science Foundation (Grant No. 20100470362). S.F.Y. acknowledges funding from NSF through award PHY-0970055. NR 34 TC 4 Z9 4 U1 2 U2 11 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JAN 17 PY 2011 VL 19 IS 2 BP 981 EP 993 DI 10.1364/OE.19.000981 PG 13 WC Optics SC Optics GA 707US UT WOS:000286314600057 PM 21263636 ER PT J AU Xiao, JF Zhuang, QL Law, BE Baldocchi, DD Chen, JQ Richardson, AD Melillo, JM Davis, KJ Hollinger, DY Wharton, S Oren, R Noormets, A Fischer, ML Verma, SB Cook, DR Sun, G McNulty, S Wofsy, SC Bolstad, PV Burns, SP Curtis, PS Drake, BG Falk, M Foster, DR Gu, LH Hadley, JL Katulk, GG Litvak, M Ma, SY Martinz, TA Matamala, R Meyers, TP Monson, RK Munger, JW Oechel, WC Paw, UKT Schmid, HP Scott, RL Starr, G Suyker, AE Torn, MS AF Xiao, Jingfeng Zhuang, Qianlai Law, Beverly E. Baldocchi, Dennis D. Chen, Jiquan Richardson, Andrew D. Melillo, Jerry M. Davis, Kenneth J. Hollinger, David Y. Wharton, Sonia Oren, Ram Noormets, Asko Fischer, Marc L. Verma, Shashi B. Cook, David R. Sun, Ge McNulty, Steve Wofsy, Steven C. Bolstad, Paul V. Burns, Sean P. Curtis, Peter S. Drake, Bert G. Falk, Matthias Foster, David R. Gu, Lianhong Hadley, Julian L. Katulk, Gabriel G. Litvak, Marcy Ma, Siyan Martinz, Timothy A. Matamala, Roser Meyers, Tilden P. Monson, Russell K. Munger, J. William Oechel, Walter C. Paw, U. Kyaw Tha Schmid, Hans Peter Scott, Russell L. Starr, Gregory Suyker, Andrew E. Torn, Margaret S. TI Assessing net ecosystem carbon exchange of U.S. terrestrial ecosystems by integrating eddy covariance flux measurements and satellite observations SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Net ecosystem carbon exchange; Eddy covariance; MODIS; Carbon sink; U S; Interannual variability; Drought; Disturbance ID SURFACE-TEMPERATURE; SOIL RESPIRATION; DIOXIDE EXCHANGE; UNITED-STATES; WATER-VAPOR; FORESTS; MODIS; VEGETATION; CO2; DISTURBANCE AB More accurate projections of future carbon dioxide concentrations in the atmosphere and associated climate change depend on improved scientific understanding of the terrestrial carbon cycle. Despite the consensus that U.S. terrestrial ecosystems provide a carbon sink, the size, distribution, and interannual variability of this sink remain uncertain. Here we report a terrestrial carbon sink in the conterminous U.S. at 0.63 pg C yr(-1) with the majority of the sink in regions dominated by evergreen and deciduous forests and savannas. This estimate is based on our continuous estimates of net ecosystem carbon exchange (NEE) with high spatial (1 km) and temporal (8-day) resolutions derived from NEE measurements from eddy covariance flux towers and wall-to-wall satellite observations from Moderate Resolution Imaging Spectroradiometer (MODIS). We find that the U.S. terrestrial ecosystems could offset a maximum of 40% of the fossil-fuel carbon emissions Our results show that the U.S. terrestrial carbon sink varied between 0.51 and 0.70 pg C yr(-1) over the period 2001-2006. The dominant sources of interannual variation of the carbon sink Included extreme climate events and disturbances. Droughts in 2002 and 2006 reduced the U.S. carbon sink by similar to 20% relative to a normal year. Disturbances including wildfires and hurricanes reduced carbon uptake or resulted in carbon release at regional scales. Our results provide an alternative, independent, and novel constraint to the U.S. terrestrial carbon sink. (C) 2010 Elsevier B.V. All rights reserved C1 [Zhuang, Qianlai] Purdue Univ, Dept Earth & Atmospher Sci, Purdue Climate Change Res Ctr, Dept Agron, W Lafayette, IN 47907 USA. [Law, Beverly E.] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Baldocchi, Dennis D.; Ma, Siyan] Univ Calif Berkeley, Ecosyst Sci Div, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Chen, Jiquan] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA. [Richardson, Andrew D.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Melillo, Jerry M.] Marine Biol Lab, Ctr Ecosyst, Woods Hole, MA 02543 USA. [Davis, Kenneth J.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Hollinger, David Y.] US Forest Serv, USDA, NE Res Stn, Durham, NH 03824 USA. [Wharton, Sonia; Falk, Matthias; Paw, U. Kyaw Tha] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Oren, Ram; Katulk, Gabriel G.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Noormets, Asko] N Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Noormets, Asko] N Carolina State Univ, So Global Change Program, Raleigh, NC 27695 USA. [Fischer, Marc L.] Lawrence Berkeley Natl Lab, Environm Energy Technol Div, Dept Atmospher Sci, Berkeley, CA 94720 USA. [Verma, Shashi B.; Suyker, Andrew E.] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68583 USA. [Cook, David R.] Argonne Natl Lab, Div Environm Sci, Argonne, IL 60439 USA. [Sun, Ge; McNulty, Steve] US Forest Serv, USDA, So Res Stn, Raleigh, NC 27606 USA. [Wofsy, Steven C.] Harvard Univ, Div Engn & Appl Sci, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Bolstad, Paul V.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Burns, Sean P.; Monson, Russell K.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Curtis, Peter S.] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Drake, Bert G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Foster, David R.] Harvard Univ, Dept Organism & Evolutionary Biol, Petersham, MA 01366 USA. [Gu, Lianhong] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. [Foster, David R.; Hadley, Julian L.] Harvard Univ, Harvard Forest, Petersham, MA 01366 USA. [Litvak, Marcy] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Martinz, Timothy A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Matamala, Roser] Argonne Natl Lab, Biosci Div, Argonne, IL 60439 USA. [Meyers, Tilden P.] NOAA ARL, Atmospher Turbulence & Diffus Div, Oak Ridge, TN 37831 USA. [Oechel, Walter C.] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Schmid, Hans Peter] Indiana Univ, Dept Geol, Bloomington, IN 47405 USA. [Schmid, Hans Peter] Res Ctr Karlsruhe FZK IMK IFU, Inst Meteorol & Climate Res, D-82467 Garmisch Partenkirchen, Germany. [Scott, Russell L.] ARS, USDA, SW Watershed Res Ctr, Tucson, AZ 85719 USA. [Starr, Gregory] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Torn, Margaret S.] Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA. RP Xiao, JF (reprint author), Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA. RI Richardson, Andrew/F-5691-2011; Zhuang, Qianlai/A-5670-2009; Hollinger, David/G-7185-2012; Schmid, Hans Peter/I-1224-2012; Oechel, Walter/F-9361-2010; Garmisch-Pa, Ifu/H-9902-2014; Baldocchi, Dennis/A-1625-2009; Torn, Margaret/D-2305-2015; Meyers, Tilden/C-6633-2016; Munger, J/H-4502-2013; Chen, Jiquan/D-1955-2009; Burns, Sean/A-9352-2008; Noormets, Asko/A-7257-2009; Gu, Lianhong/H-8241-2014; Law, Beverly/G-3882-2010; OI Richardson, Andrew/0000-0002-0148-6714; Schmid, Hans Peter/0000-0001-9076-4466; Oechel, Walter/0000-0002-3504-026X; Baldocchi, Dennis/0000-0003-3496-4919; Munger, J/0000-0002-1042-8452; Burns, Sean/0000-0002-6258-1838; Noormets, Asko/0000-0003-2221-2111; Gu, Lianhong/0000-0001-5756-8738; Law, Beverly/0000-0002-1605-1203; Martin, Timothy/0000-0002-7872-4194 FU National Science Foundation (NSF); Department of Energy (DOE) FX This study was supported by grants from the National Science Foundation (NSF) and Department of Energy (DOE) We thank the principal investigators and contributors of the MODIS data products the Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center (DACCC) and the Earth Observing System (EOS) Data Gateway for making these MODIS data products available The Level I Ecoregions map of North America was obtained from Environmental Protection Agency (EPA) the Biscuit fire severity data from J Thompson Harvard University and the PRISM climate database from the PRISM Group Oregon State University Computing support was provided by the Rosen Center for Advanced Computing Purdue University We also thank anonymous reviewers and Dr Anne Verhoef for their valuable comments on earlier versions of the manuscript [The EC-MOD dataset is available upon request] NR 54 TC 80 Z9 84 U1 2 U2 77 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 EI 1873-2240 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD JAN 15 PY 2011 VL 151 IS 1 BP 60 EP 69 DI 10.1016/j.agrformet.2010.09.002 PG 10 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 694UV UT WOS:000285325400006 ER PT J AU Norrbom, AL Korytkowski, CA AF Norrbom, Allen L. Korytkowski, Cheslavo A. TI New species of and taxonomic notes on Anastrepha (Diptera: Tephritidae) SO ZOOTAXA LA English DT Article DE fruit flies; taxonomy AB Seven new species of Anastrepha are described and illustrated: A. conflua (Costa Rica), A. levefasciata (Peru), A. nolazcoae (Peru), A. paradentata (Mexico), A. raveni (Peru), A. trivittata (Brazil: Amazonas), and A. woodleyi (Bolivia). Anastrepha nunezae Steyskal, 1977, is recognized as a synonym of A. mucronota Stone, 1942, and A. pseudanomala Norrbom is recorded for the first time from Ecuador. C1 [Norrbom, Allen L.] Smithsonian Inst, ARS, Systemat Entomol Lab, USDA, Washington, DC 20013 USA. [Korytkowski, Cheslavo A.] Univ Panama, Programa Maestria Entomol Vice Rectoria Invest &, Panama City, Panama. RP Norrbom, AL (reprint author), Smithsonian Inst, ARS, Systemat Entomol Lab, USDA, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov; cheslavok@cableonda.net NR 24 TC 18 Z9 18 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 14 PY 2011 IS 2740 BP 1 EP 23 PG 23 WC Zoology SC Zoology GA 707JQ UT WOS:000286282700001 ER PT J AU Henry, AG Brooks, AS Piperno, DR AF Henry, Amanda G. Brooks, Alison S. Piperno, Dolores R. TI Microfossils in calculus demonstrate consumption of plants and cooked foods in Neanderthal diets (Shanidar III, Iraq; Spy I and II, Belgium) SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID NORTHERN IRAQ; STARCH GRAINS; ISOTOPIC EVIDENCE; DENTAL CALCULUS; FLOWER BURIAL; MODERN HUMANS; KEBARA CAVE; MIDDLE; PHYTOLITHS; ISRAEL AB The nature and causes of the disappearance of Neanderthals and their apparent replacement by modern humans are subjects of considerable debate. Many researchers have proposed biologically or technologically mediated dietary differences between the two groups as one of the fundamental causes of Neanderthal disappearance. Some scenarios have focused on the apparent lack of plant foods in Neanderthal diets. Here we report direct evidence for Neanderthal consumption of a variety of plant foods, in the form of phytoliths and starch grains recovered from dental calculus of Neanderthal skeletons from Shanidar Cave, Iraq, and Spy Cave, Belgium. Some of the plants are typical of recent modern human diets, including date palms (Phoenix spp.), legumes, and grass seeds (Triticeae), whereas others are known to be edible but are not heavily used today. Many of the grass seed starches showed damage that is a distinctive marker of cooking. Our results indicate that in both warm eastern Mediterranean and cold northwestern European climates, and across their latitudinal range, Neanderthals made use of the diverse plant foods available in their local environment and transformed them into more easily digestible foodstuffs in part through cooking them, suggesting an overall sophistication in Neanderthal dietary regimes. C1 [Henry, Amanda G.; Brooks, Alison S.] Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Henry, Amanda G.; Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Archaeobiol Lab, Dept Anthropol, Washington, DC 20013 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Balboa, Panama. RP Henry, AG (reprint author), Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. EM ahenry@gwmail.gwu.edu; pipernod@si.edu OI Henry, Amanda/0000-0002-2923-4199 FU National Science Foundation; Smithsonian Predoctoral Fellowship; Wenner Gren Dissertation Fieldwork Grant; National Museum of Natural History; George Washington University; Smithsonian Tropical Research Institute FX We thank three reviewers for their insightful comments. We also thank M. Zeder for information about Shanidar Cave; R. Potts, J. Clark, and the Smithsonian Institution for access to the Shanidar fossils; P. Semal, R. Orban, and the Institute Royal des Sciences Naturelles de Belgique for access to the Spy fossils; R. and R. Solecki for support; H. F. Hudson and C. Foltz for laboratory assistance; the US Department of Agriculture National Plant Germplasm System, including the North Central Regional Plant Introduction Station, Ames, Iowa, the Plant Genetic Resources Unit, Geneva, New York, the National Small Grains Collection including Barley and Wheat Genetic Stocks, Aberdeen, Idaho, and the Woody Landscape Plant Germplasm Repository, Beltsville, MD, for supplying many plant seeds; and the Smithsonian National Herbarium for permission to sample their folders. The Spy fossils were donated to the Institute Royal des Sciences Naturelles de Belgique by the family of Professor Max Lohest (1857-1926). A. G. H. was supported by a National Science Foundation Integrative Graduate Education and Research Traineeship (IGERT) grant, a Smithsonian Predoctoral Fellowship, a Wenner Gren Dissertation Fieldwork Grant, and the Archaeobiology Program of the National Museum of Natural History. A. S. B. was supported in part by a selective excellence grant from the George Washington University and a National Science Foundation Human Origins Moving in New Directions (HOMINID) grant to the Smithsonian Institution. D. R. P. is supported by the National Museum of Natural History and the Smithsonian Tropical Research Institute. NR 71 TC 136 Z9 145 U1 6 U2 67 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 11 PY 2011 VL 108 IS 2 BP 486 EP 491 DI 10.1073/pnas.1016868108 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 704ZU UT WOS:000286097700015 PM 21187393 ER PT J AU Koutroumpa, D Smith, RK Edgar, RJ Kuntz, KD Plucinsky, PP Snowden, SL AF Koutroumpa, Dimitra Smith, Randall K. Edgar, Richard J. Kuntz, Kip D. Plucinsky, Paul P. Snowden, Steven L. TI XMM-NEWTON OBSERVATIONS OF MBM 12: MORE CONSTRAINTS ON THE SOLAR WIND CHARGE EXCHANGE AND LOCAL BUBBLE EMISSIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: bubbles; ISM: supernova remnants; solar wind; Sun: heliosphere; X-rays: diffuse background; X-rays: ISM ID X-RAY-EMISSION; EXTREME-ULTRAVIOLET EMISSION; INTERSTELLAR-MEDIUM; MOLECULAR CLOUD; HOT BUBBLE; GAS; NEUTRALS; SUZAKU; MAPS; SPECTRA AB We present the first analysis of an XMM-Newton observation of the nearby molecular cloud MBM 12. We find that in the direction of MBM 12 the total OVII (0.57 keV) triplet emission is 1.8(-0.6)(+0.5) photons cm(-2) s(-1) sr(-1) (or line units, LU) while for the OVIII (0.65 keV) line emission we find a 3 sigma upper limit of < 1 LU. We use a heliospheric model to calculate the OVII and OVIII emission generated by Solar Wind Charge-eXchange (SWCX) which we compare to the XMM-Newton observations. This comparison provides new constraints on the relative heliospheric and Local Bubble contributions to the local diffuse X-ray background. The heliospheric SWCX model predicts 0.82 LU for OVII, which accounts for similar to 46% +/- 15% of the observed value, and 0.33 LU for the OVIII line emission consistent with the XMM-Newton observed value. We discuss our results in combination with previous observations of MBM 12 with Chandra and Suzaku. C1 [Koutroumpa, Dimitra; Snowden, Steven L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, Randall K.; Edgar, Richard J.; Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuntz, Kip D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. RP Koutroumpa, D (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RI XRAY, SUZAKU/A-1808-2009 FU NASA [NAS5-00132]; Goddard Space Flight Center FX We thank the MIT Space Plasma Group (K.W. Ogilvie and A.J. Lazarus) for the WIND data, and the STEREO/PLASTIC Investigation (A.B. Galvin, PI) and NASA Contract NAS5-00132 for the PLASTIC Level 2 data used in this study. We also thank the ACE/SWICS-SWIMS instrument teams (J. Raines, S. Lepri, and T. Zurbuchen) and the ACE Science Center for providing the ACE data, and the Ulysses/SWICS team (G. Gloeckler, T. Zurbuchen, and R. von Steiger) for the Ulysses/SWICS data. Finally, we are grateful to our referee, Jeffrey Linsky, for his constructive remarks that considerably improved the manuscript.; This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 45 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2011 VL 726 IS 2 AR 91 DI 10.1088/0004-637X/726/2/91 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698WB UT WOS:000285623600035 ER PT J AU Alves, FO Girart, JM Lai, SP Rao, R Zhang, QZ AF Alves, Felipe O. Girart, Josep M. Lai, Shih-Ping Rao, Ramprasad Zhang, Qizhou TI THE MAGNETIC FIELD IN THE NGC 2024 FIR 5 DENSE CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (NGC 2024); ISM: magnetic fields; polarization; stars: formation; techniques: interferometric ID FAR-INFRARED POLARIMETRY; FORMING MOLECULAR CLOUDS; MASS STAR-FORMATION; ORION-B; AMBIPOLAR-DIFFUSION; DARK CLOUDS; PROTOSTELLAR CONDENSATIONS; SUBMILLIMETER ARRAY; RADIATIVE TORQUES; GRAIN ALIGNMENT AB We used the Submillimeter Array to observe the thermal polarized dust emission from the protostellar source NGC 2024 FIR 5. The polarized emission outlines a partial hourglass morphology for the plane-of-sky component of the core magnetic field. Our data are consistent with previous BIMA maps, and the overall magnetic field geometries obtained with both instruments are similar. We resolve the main core into two components, FIR 5A and FIR 5B. A possible explanation for the asymmetrical field lies in depolarization effects due to the lack of internal heating from the FIR 5B source, which may be in a prestellar evolutionary state. The field strength was estimated to be 2.2 mG, in agreement with previous BIMA data. We discuss the influence of a nearby H II region over the field lines at scales of similar to 0.01 pc. Although the hot component is probably compressing the molecular gas where the dust core is embedded, it is unlikely that the radiation pressure exceeds the magnetic tension. Finally, a complex outflow morphology is observed in CO (3 -> 2) maps. Unlike previous maps, several features associated with dust condensations other than FIR 5 are detected. C1 [Alves, Felipe O.; Girart, Josep M.] Inst Ciencies Espai IEEC CSIC, Fac Ciencies, Bellaterra 08193, Catalunya, Spain. [Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30043, Taiwan. [Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30043, Taiwan. [Rao, Ramprasad] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Alves, FO (reprint author), Inst Ciencies Espai IEEC CSIC, Fac Ciencies, Campus UAB,Torre C5 Parell 2, Bellaterra 08193, Catalunya, Spain. EM oliveira@ice.cat; girart@ice.cat; slai@phys.nthu.edu.tw; rrao@sma.hawaii.edu; qzhang@cfa.harvard.edu RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 FU MICINN [AYA2008-06189-C03]; AGAUR [2009SGR1172] FX F.O.A. thanks all the staff at the SMA in Hawaii and Cambridge, MA. F.O.A. and J.M.G. are supported by the MICINN AYA2008-06189-C03 and the AGAUR 2009SGR1172 grants. NR 63 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 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2011 VL 726 IS 2 AR 63 DI 10.1088/0004-637X/726/2/63 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698WB UT WOS:000285623600007 ER PT J AU Christiansen, JL Ballard, S Charbonneau, D Deming, D Holman, MJ Madhusudhan, N Seager, S Wellnitz, DD Barry, RK Livengood, TA Hewagama, T Hampton, DL Lisse, CM A'Hearn, MF AF Christiansen, Jessie L. Ballard, Sarah Charbonneau, David Deming, Drake Holman, Matthew J. Madhusudhan, Nikku Seager, Sara Wellnitz, Dennis D. Barry, Richard K. Livengood, Timothy A. Hewagama, Tilak Hampton, Don L. Lisse, Carey M. A'Hearn, Michael F. TI SYSTEM PARAMETERS, TRANSIT TIMES, AND SECONDARY ECLIPSE CONSTRAINTS OF THE EXOPLANET SYSTEMS HAT-P-4, TrES-2, TrES-3, and WASP-3 FROM THE NASA EPOXI MISSION OF OPPORTUNITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; stars: individual (HAT-P-4, WASP-3, TrES-2, TrES-3) ID PLANET SYSTEMS; LIGHT CURVES; HOT JUPITER; DEEP IMPACT; ATMOSPHERES; EMISSION; STELLAR; PROJECT; KEPLER; ORBIT AB As part of the NASA EPOXI Mission of Opportunity, we observed seven known transiting extrasolar planet systems in order to construct time series photometry of extremely high phase coverage and precision. Here we present the results for four "hot-Jupiter systems" with near-solar stars-HAT-P-4, TrES-3, TrES-2, and WASP-3. We observe 10 transits of HAT-P-4, estimating the planet radius R-p = 1.332 +/- 0.052 R-Jup, the stellar radius R-* = 1.602 +/- 0.061 R-circle dot, the inclination i = 89.67 +/- 0.30 deg, and the transit duration from first to fourth contact tau = 255.6 +/- 1.9 minutes. For TrES-3, we observe seven transits and find R-p = 1.320 +/- 0.057 R-Jup, R-* = 0.817 +/- 0.022 R-circle dot, i = 81.99 +/- 0.30 deg, and tau = 81.9 +/- 1.1 minutes. We also note a long-term variability in the TrES-3 light curve, which may be due to star spots. We observe nine transits of TrES-2 and find R-p = 1.169 +/- 0.034 R-Jup, R-* = 0.940 +/- 0.026 R-circle dot, i = 84.15 +/- 0.16 deg, and tau = 107.3 +/- 1.1 minutes. Finally, we observe eight transits of WASP-3, finding R-p = 1.385 +/- 0.060 R-Jup, R-* = 1.354 +/- 0.056 R-circle dot, i = 84.22 +/- 0.81 deg, and tau = 167.3 +/- 1.3 minutes. We present refined orbital periods and times of transit for each target. We state 95% confidence upper limits on the secondary eclipse depths in our broadband visible bandpass centered on 650 nm. These limits are 0.073% for HAT-P-4, 0.062% for TrES-3, 0.16% for TrES-2, and 0.11% for WASP-3. We combine the TrES-3 secondary eclipse information with the existing published data and confirm that the atmosphere likely does not have a temperature inversion. C1 [Christiansen, Jessie L.; Ballard, Sarah; Charbonneau, David; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deming, Drake; Barry, Richard K.; Livengood, Timothy A.; Hewagama, Tilak] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Madhusudhan, Nikku; Seager, Sara] MIT, Cambridge, MA 02159 USA. [Wellnitz, Dennis D.; Hewagama, Tilak] Univ Maryland, College Pk, MD 20742 USA. [Hampton, Don L.] Univ Alaska Fairbanks, Fairbanks, AK 99775 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Christiansen, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jchristi@cfa.harvard.edu RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X FU National Aeronautics and Space Administration [NNX08AB64A, NNX08AD05A] FX Support for this work was provided by the EPOXI Project of the National Aeronautics and Space Administration's Discovery Program via funding to the Goddard Space Flight Center, and to Harvard University via Co-operative Agreement NNX08AB64A, and to the Smithsonian Astrophysical Observatory via Co-operative Agreement NNX08AD05A. The authors acknowledge and are grateful for the use of publicly available transit modeling routines by Eric Agol and Kaisey Mandel, and also the Levenberg-Marquardt least-squares minimization routine MPFITFUN by Craig Markwardt. This work has used data obtained by various observers collected in the Exoplanet Transit Database, http://var.astro.cz/ETD. NR 36 TC 20 Z9 21 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2011 VL 726 IS 2 AR 94 DI 10.1088/0004-637X/726/2/94 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698WB UT WOS:000285623600038 ER PT J AU Cisternas, M Jahnke, K Inskip, KJ Kartaltepe, J Koekemoer, AM Lisker, T Robaina, AR Scodeggio, M Sheth, K Trump, JR Andrae, R Miyaji, T Lusso, E Brusa, M Capak, P Cappelluti, N Civano, F Ilbert, O Impey, CD Leauthaud, A Lilly, SJ Salvato, M Scoville, NZ Taniguchi, Y AF Cisternas, Mauricio Jahnke, Knud Inskip, Katherine J. Kartaltepe, Jeyhan Koekemoer, Anton M. Lisker, Thorsten Robaina, Aday R. Scodeggio, Marco Sheth, Kartik Trump, Jonathan R. Andrae, Rene Miyaji, Takamitsu Lusso, Elisabeta Brusa, Marcella Capak, Peter Cappelluti, Nico Civano, Francesca Ilbert, Olivier Impey, Chris D. Leauthaud, Alexie Lilly, Simon J. Salvato, Mara Scoville, Nick Z. Taniguchi, Yoshi TI THE BULK OF THE BLACK HOLE GROWTH SINCE z similar to 1 OCCURS IN A SECULAR UNIVERSE: NO MAJOR MERGER-AGN CONNECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: interactions; quasars: general ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; ULTRALUMINOUS INFRARED GALAXIES; WIDE-FIELD SURVEY; DIGITAL-SKY-SURVEY; X-RAY; HOST GALAXIES; COSMOS FIELD; MASSIVE GALAXIES; STAR-FORMATION AB What is the relevance of major mergers and interactions as triggering mechanisms for active galactic nuclei (AGNs) activity? To answer this long-standing question, we analyze 140 XMM-Newton-selected AGN host galaxies and a matched control sample of 1264 inactive galaxies over z similar to 0.3-1.0 and M-* < 10(11.7) M-circle dot with high-resolution Hubble Space Telescope/Advanced Camera for Surveys imaging from the COSMOS field. The visual analysis of their morphologies by 10 independent human classifiers yields a measure of the fraction of distorted morphologies in the AGN and control samples, i.e., quantifying the signature of recent mergers which might potentially be responsible for fueling/triggering the AGN. We find that (1) the vast majority (>85%) of the AGN host galaxies do not show strong distortions and (2) there is no significant difference in the distortion fractions between active and inactive galaxies. Our findings provide the best direct evidence that, since z similar to 1, the bulk of black hole (BH) accretion has not been triggered by major galaxy mergers, therefore arguing that the alternative mechanisms, i.e., internal secular processes and minor interactions, are the leading triggers for the episodes of major BH growth. We also exclude an alternative interpretation of our results: a substantial time lag between merging and the observability of the AGN phase could wash out the most significant merging signatures, explaining the lack of enhancement of strong distortions on the AGN hosts. We show that this alternative scenario is unlikely due to (1) recent major mergers being ruled out for the majority of sources due to the high fraction of disk-hosted AGNs, (2) the lack of a significant X-ray signal in merging inactive galaxies as a signature of a potential buried AGN, and (3) the low levels of soft X-ray obscuration for AGNs hosted by interacting galaxies, in contrast to model predictions. C1 [Cisternas, Mauricio; Jahnke, Knud; Inskip, Katherine J.; Robaina, Aday R.; Andrae, Rene] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kartaltepe, Jeyhan] Natl Opt Astron Observ, Tucson, AZ 85721 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Lisker, Thorsten] Univ Heidelberg, Astron Rech Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Robaina, Aday R.] Univ Barcelona IEEC, ICC, E-08028 Barcelona, Spain. [Scodeggio, Marco] IASF INAF, I-20133 Milan, Italy. [Sheth, Kartik] CALTECH, Spitzer Space Ctr, Pasadena, CA 91125 USA. [Trump, Jonathan R.; Impey, Chris D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Miyaji, Takamitsu] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Miyaji, Takamitsu] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Lusso, Elisabeta] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Brusa, Marcella; Cappelluti, Nico] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Civano, Francesca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ilbert, Olivier] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Leauthaud, Alexie] Univ Calif Berkeley, LBNL, Berkeley, CA 94720 USA. [Leauthaud, Alexie] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Lilly, Simon J.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Salvato, Mara] Max Planck Inst Plasma Phys, D-85741 Garching, Germany. [Taniguchi, Yoshi] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. RP Cisternas, M (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM cisternas@mpia.de OI Scodeggio, Marco/0000-0002-2282-5850; Jahnke, Knud/0000-0003-3804-2137; Cappelluti, Nico/0000-0002-1697-186X; Koekemoer, Anton/0000-0002-6610-2048 FU NASA [NAS 5-26555]; ESA FX Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; European Southern Observatory under Large Program 175.A-0839; and the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. NR 144 TC 174 Z9 174 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2011 VL 726 IS 2 AR 57 DI 10.1088/0004-637X/726/2/57 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698WB UT WOS:000285623600001 ER PT J AU Deming, D Knutson, H Agol, E Desert, JM Burrows, A Fortney, JJ Charbonneau, D Cowan, NB Laughlin, G Langton, J Showman, AP Lewis, NK AF Deming, Drake Knutson, Heather Agol, Eric Desert, Jean-Michel Burrows, Adam Fortney, Jonathan J. Charbonneau, David Cowan, Nicolas B. Laughlin, Gregory Langton, Jonathan Showman, Adam P. Lewis, Nikole K. TI WARM SPITZER PHOTOMETRY OF THE TRANSITING EXOPLANETS CoRoT-1 AND CoRoT-2 AT SECONDARY ECLIPSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric ID PLANET HD 189733B; INFRARED-EMISSION SPECTRUM; IRRADIATED GIANT PLANETS; EXTRASOLAR PLANET; THERMAL EMISSION; TEMPERATURE INVERSION; SPACE-TELESCOPE; HOT JUPITERS; LIGHT CURVES; MU-M AB We measure secondary eclipses of the hot giant exoplanets CoRoT-1 at 3.6 and 4.5 mu m, and CoRoT-2 at 3.6 mu m, both using Warm Spitzer. We find that the Warm Spitzer mission is working very well for exoplanet science. For consistency of our analysis we also re-analyze archival cryogenic Spitzer data for secondary eclipses of CoRoT-2 at 4.5 and 8 mu m. We compare the total data for both planets, including optical eclipse measurements by the CoRoT mission, and ground-based eclipse measurements at 2 mu m, to existing models. Both planets exhibit stronger eclipses at 4.5 than at 3.6 mu m, which is often indicative of an atmospheric temperature inversion. The spectrum of CoRoT-1 is best reproduced by a 2460 K blackbody, due either to a high altitude layer that strongly absorbs stellar irradiance, or an isothermal region in the planetary atmosphere. The spectrum of CoRoT-2 is unusual because the 8 mu m contrast is anomalously low. Non-inverted atmospheres could potentially produce the CoRoT-2 spectrum if the planet exhibits line emission from CO at 4.5 mu m, caused by tidal-induced mass loss. However, the viability of that hypothesis is questionable because the emitting region cannot be more than about 30% larger than the planet's transit radius, based on the ingress and egress times at eclipse. An alternative possibility to account for the spectrum of CoRoT-2 is an additional opacity source that acts strongly at wavelengths less than 5 mu m, heating the upper atmosphere while allowing the deeper atmosphere seen at 8 mu m to remain cooler. We obtain a similar result as Gillon et al. for the phase of the secondary eclipse of CoRoT-2, implying an eccentric orbit with e cos(omega) = -0.0030 +/- 0.0004. C1 [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Knutson, Heather] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Agol, Eric; Cowan, Nicolas B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. [Showman, Adam P.; Lewis, Nikole K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Deming, D (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RI Agol, Eric/B-8775-2013; OI Charbonneau, David/0000-0002-9003-484X; Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354 FU NASA [NNX07AG80G]; Miller Institute for Basic Research in Science; NSF [0645416, PHY05-51164]; JPL/Spitzer [1328092, 1348668, 1312647] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA. H.K. is supported by a fellowship from the Miller Institute for Basic Research in Science. E.A. acknowledges support under NSF CAREER grant no. 0645416. A.B. was supported by NASA grant NNX07AG80G and under JPL/Spitzer Agreements 1328092, 1348668, and 1312647. He is also pleased to note that part of this work was performed while in residence at the Kavli Institute for Theoretical Physics, funded by the NSF through grant no. PHY05-51164. We thank Dr. Rory Barnes for informative conversations regarding the tidal evolution of CoRoT-2, and an anonymous referee for a very thorough review that improved this paper significantly. NR 53 TC 46 Z9 46 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2011 VL 726 IS 2 AR 95 DI 10.1088/0004-637X/726/2/95 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698WB UT WOS:000285623600039 ER PT J AU Longmore, SN Pillai, T Keto, E Zhang, Q Qiu, K AF Longmore, S. N. Pillai, T. Keto, E. Zhang, Q. Qiu, K. TI IS PROTOSTELLAR HEATING SUFFICIENT TO HALT FRAGMENTATION? A CASE STUDY OF THE MASSIVE PROTOCLUSTER G8.68-0.37 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: molecules; stars: early-type; stars: formation; stars: pre-main sequence ID INFRARED DARK CLOUDS; STAR-FORMATION REGIONS; ULTRACOMPACT HII-REGIONS; H-II REGIONS; MILLIMETER CONTINUUM OBSERVATIONS; METHANOL MASERS; SUBMILLIMETER ARRAY; MOLECULAR OUTFLOWS; RADIATIVE-TRANSFER; MAGNETIC-FIELDS AB If star formation proceeds by thermal fragmentation and the subsequent gravitational collapse of the individual fragments, how is it possible to form fragments massive enough for O and B stars in a typical star-forming molecular cloud where the Jeans mass is about 1 M-circle dot at the typical densities (10(4) cm(-3)) and temperatures (10 K)? We test the hypothesis that a first generation of low-mass stars may heat the gas enough that subsequent thermal fragmentation results in fragments >= 10M(circle dot), sufficient to form B stars. We combine ATCA and Submillimeter Array observations of the massive star-forming region G8.68-0.37 with radiative transfer modeling to derive the present-day conditions in the region and use this to infer the conditions in the past, at the time of core formation. Assuming that the current mass/separation of the observed cores equals the fragmentation Jeans mass/length and the region's average density has not changed requires the gas temperature to have been 100 K at the time of fragmentation. The postulated first generation of low-mass stars would still be around today, but the number required to heat the cloud exceeds the limits imposed by the observations. Several lines of evidence suggest the observed cores in the region should eventually form O stars yet none have sufficient raw material. Even if feedback may have suppressed fragmentation, it was not sufficient to halt it to this extent. To develop into O stars, the cores must obtain additional mass from outside their observationally defined boundaries. The observations suggest that they are currently fed via infall from the very massive reservoir (similar to 1500 M-circle dot) of gas in the larger parsec scale cloud around the star-forming cores. This suggests that massive stars do not form in the collapse of individual massive fragments, but rather in smaller fragments that themselves continue to gain mass by accretion from larger scales. C1 [Longmore, S. N.] European So Observ, D-85748 Garching, Germany. [Pillai, T.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Keto, E.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Qiu, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Longmore, SN (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM slongmore@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; Academia Sinica FX S.N.L. thanks Stella Offner, Phil Myers, David Wilner, Tyler Bourke, Rowan Smith, and Paul Ho for thoughtful comments, Roberto Galvan-Madrid for comments on a draft of the paper, and Mark Krumholz for a stimulating discussion on the analysis. S.N.L. gratefully acknowledges support of this research through funding as a Submillimeter Array Fellow. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research has made use of NASA's Astrophysics Data System. NR 89 TC 35 Z9 35 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 JAN 10 PY 2011 VL 726 IS 2 AR 97 DI 10.1088/0004-637X/726/2/97 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698WB UT WOS:000285623600041 ER PT J AU Randall, SW Forman, WR Giacintucci, S Nulsen, PEJ Sun, M Jones, C Churazov, E David, LP Kraft, R Donahue, M Blanton, EL Simionescu, A Werner, N AF Randall, S. W. Forman, W. R. Giacintucci, S. Nulsen, P. E. J. Sun, M. Jones, C. Churazov, E. David, L. P. Kraft, R. Donahue, M. Blanton, E. L. Simionescu, A. Werner, N. TI SHOCKS AND CAVITIES FROM MULTIPLE OUTBURSTS IN THE GALAXY GROUP NGC 5813: A WINDOW TO ACTIVE GALACTIC NUCLEUS FEEDBACK SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: groups: individual (NGC 5813); galaxies: individual (NGC 5813); X-rays: galaxies ID X-RAY GAS; ELLIPTIC GALAXIES; COOLING-FLOW; XMM-NEWTON; STAR-FORMATION; JET POWER; CHANDRA OBSERVATION; GASEOUS ATMOSPHERE; SOLAR ABUNDANCES; PERSEUS CLUSTER AB We present results from new Chandra, GMRT, and SOAR observations of NGC 5813, the dominant central galaxy in a nearby galaxy group. The system shows three pairs of collinear cavities at 1 kpc, 8 kpc, and 20 kpc from the central source, from three distinct outbursts of the central active galactic nucleus (AGN), which occurred 3 x 10(6), 2 x 10(7), and 9 x 10(7) yr ago. The Ha and X-ray observations reveal filaments of cool gas that has been uplifted by the X-ray cavities. The inner two cavity pairs are filled with radio-emitting plasma, and each pair is associated with an elliptical surface brightness edge, which we unambiguously identify as shocks (with measured temperature jumps) with Mach numbers of M approximate to 1.7 and M approximate to 1.5 for the inner and outer shocks, respectively. Such clear signatures from three distinct AGN outbursts in an otherwise dynamically relaxed system provide a unique opportunity to study AGN feedback and outburst history. The mean power of the two most recent outbursts differs by a factor of six, from (1.5-10) x 10(42) erg s(-1), indicating that the mean jet power changes significantly over long (similar to 10(7) yr) timescales. The total energy output of the most recent outburst is also more than an order of magnitude less than the total energy of the previous outburst (1.5 x 10(56) erg versus 4 x 10(57) erg), which may be a result of the lower mean power, or may indicate that the most recent outburst is ongoing. The outburst interval implied by both the shock and cavity ages (similar to 10(7) yr) indicates that, in this system, shock heating alone is sufficient to balance radiative cooling close to the central AGN, which is the relevant region for regulating feedback between the intracluster medium and the central supermassive black hole. C1 [Randall, S. W.; Forman, W. R.; Giacintucci, S.; Nulsen, P. E. J.; Jones, C.; David, L. P.; Kraft, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giacintucci, S.] INAF IRA, I-40129 Bologna, Italy. [Sun, M.] Univ Virginia, Dept Astron, Charlottesville, VA 22901 USA. [Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.] Space Res Inst IKI, Moscow 117810, Russia. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Blanton, E. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Blanton, E. L.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Simionescu, A.; Werner, N.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. RP Randall, SW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM srandall@cfa.harvard.edu RI Donahue, Megan/B-5361-2012; Churazov, Eugene/A-7783-2013; Blanton, Elizabeth/H-4501-2014; OI Randall, Scott/0000-0002-3984-4337; Nulsen, Paul/0000-0003-0297-4493 FU Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution; National Aeronautics and Space Administration [NAS8-03060, PF9-00070, PF8-90056] FX The financial support for this work was partially provided for by the Chandra X-ray Center through NASA contract NAS8-03060, and the Smithsonian Institution. We thank the staff of the GMRT for their help during the observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. The SOAR Telescope is a joint project of Conselho Nacional des Pesquisas Cientficas e Tecnologicas CNPq-Brazil, The University of North Carolina Chapel Hill, Michigan State University, and the National Optical Astronomy Observatory. AS and NW are supported by the National Aeronautics and Space Administration through Chandra/Einstein Postdoctoral Fellowship Award Numbers PF9-00070 and PF8-90056 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. We thank the referee for useful comments. NR 67 TC 78 Z9 78 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2011 VL 726 IS 2 AR 86 DI 10.1088/0004-637X/726/2/86 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698WB UT WOS:000285623600030 ER PT J AU Chang, AL Blakeslee, AMH Miller, AW Ruiz, GM AF Chang, Andrew L. Blakeslee, April M. H. Miller, A. Whitman Ruiz, Gregory M. TI Establishment Failure in Biological Invasions: A Case History of Littorina littorea in California, USA SO PLOS ONE LA English DT Article ID MARINE SPECIES INTRODUCTION; SAN-FRANCISCO BAY; NORTH-AMERICA; GENETIC DIVERSITY; CARCINUS-MAENAS; INTERTIDAL ZONE; GREEN CRAB; SNAIL; ATLANTIC; POPULATION AB Background: The early stages of biological invasions are rarely observed, but can provide significant insight into the invasion process as well as the influence vectors have on invasion success or failure. Methodology/Principal Findings: We characterized three newly discovered populations of an introduced gastropod, Littorina littorea (Linne, 1758), in California, USA, comparing them to potential source populations in native Europe and the North American East Coast, where the snail is also introduced. Demographic surveys were used to assess spatial distribution and sizes of the snail in San Francisco and Anaheim Bays, California. Mitochondrial DNA was sequenced and compared among these nascent populations, and various populations from the North American East Coast and Europe, to characterize the California populations and ascertain their likely source. Demographic and genetic data were considered together to deduce likely vectors for the California populations. We found that the three large California L. littorea populations contained only adult snails and had unexpectedly high genetic diversity rather than showing an extreme bottleneck as typically expected in recent introductions. Haplotype diversity in Californian populations was significantly reduced compared to European populations, but not compared to East Coast populations. Genetic analyses clearly suggested the East Coast as the source region for the California introductions. Conclusions and Significance: The California L. littorea populations were at an early, non-established phase of invasion with no evidence of recruitment. The live seafood trade is the most likely invasion vector for these populations, as it preferentially transports large numbers of adult L. littorea, matching the demographic structure of the introduced California L. littorea populations. Our results highlight continued operation of live seafood trade vectors and the influence of vectors on the demographic and genetic structure of the resulting populations, especially early stages of the invasion process. C1 [Chang, Andrew L.; Blakeslee, April M. H.; Miller, A. Whitman; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Chang, AL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM changal@si.edu RI Chang, Andrew/J-8058-2016; OI Chang, Andrew/0000-0002-7870-285X; Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X FU National Science Foundation; Smithsonian Institution; Smithsonian Marine Science Network FX Financial support was provided by a National Science Foundation Graduate Research Fellowship to ALC, Smithsonian Institution Postdoctoral Fellowships to ALC and AMHB, and a Smithsonian Marine Science Network Postdoctoral Fellowship to AMHB. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 54 TC 8 Z9 10 U1 1 U2 25 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 10 PY 2011 VL 6 IS 1 AR e16035 DI 10.1371/journal.pone.0016035 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 710LL UT WOS:000286513100025 PM 21264336 ER PT J AU Latimer, E Zong, JC Heaggans, SY Richman, LK Hayward, GS AF Latimer, Erin Zong, Jian-Chao Heaggans, Sarah Y. Richman, Laura K. Hayward, Gary S. TI Detection and evaluation of novel herpesviruses in routine and pathological samples from Asian and African elephants: Identification of two new probosciviruses (EEHV5 and EEHV6) and two new gammaherpesviruses (EGHV3B and EGHV5) SO VETERINARY MICROBIOLOGY LA English DT Article DE Probosciviruses; Gamma herpesviruses; Hemorrhagic disease; Mixed infections; Viral load ID NEWLY RECOGNIZED DISEASE; ENDOTHELIOTROPIC HERPESVIRUSES; MAXIMUS; INFECTION; VARIANTS; PCR AB Systemic infections with elephant endotheliotropic herpesviruses (EEHV) cause a rapid onset acute hemorrhagic disease with an 85% mortality rate. More than 60 cases have been confirmed worldwide occurring predominantly in juvenile Asian elephants. Originally, three virus types EEHV1A, EEHV1B and EEHV2 were identified, all members of the Proboscivirus genus within the Betaherpesvirinae. However, four elephant gammaherpesviruses (EGHV) have also been found by DNA PCR approaches in eye and genital secretions of asymptomatic animals, and two more versions of the probosciviruses, EEHV3 and EEHV4, were recently detected in acute hemorrhagic disease cases. To ask whether even more species of elephant herpesviruses may exist, we have developed several new diagnostic DNA PCR assays using multiple round primers in the DNA POL region. These have been used routinely for nearly three years to screen samples submitted to the Elephant Herpesvirus Laboratory for diagnosis of possible cases of EEHV disease in blood and necropsy tissue, as well as in biopsies of other suspicious lesions or growths. Several more cases of EEHV1-associated hemorrhagic disease were confirmed, but in addition, we describe here eleven examples of other known and novel herpesviruses detected and evaluated with these reagents. They include the prototypes of four new elephant herpesviruses, two more within the proboscivirus group EEHV5 and EEHV6, plus two more gammaherpesviruses EGHV3B and EGHV5. We also report initial semi-quantitative PCR assays demonstrating very high viral loads in the blood of the EEHV3 and EEHV4-associated hemorrhagic disease cases. (C) 2010 Elsevier B.V. All rights reserved. C1 [Zong, Jian-Chao; Heaggans, Sarah Y.; Hayward, Gary S.] Johns Hopkins Sch Med, Viral Oncol Program, Baltimore, MD 21231 USA. [Latimer, Erin; Richman, Laura K.] Smithsonian Natl Zool Pk, Elephant Herpesyirus Lab, Washington, DC 20008 USA. RP Hayward, GS (reprint author), Johns Hopkins Sch Med, Viral Oncol Program, 3M09 Bunting Blaustein Bldg,1650 Orleans St, Baltimore, MD 21231 USA. EM latimere@si.edu; jczong@yahoo.com; sheagga1@jhmi.edu; RichmanL@comcast.net; ghayward@jhmi.edu FU Smithsonian Institution; Morris Animal Foundation; International Elephant Foundation; Ringling Bros.; Barnum and Bailey Center for Elephant Conservation; NIH [R01 AI24576] FX Studies at the National Zoological Park in Washington DC were funded by Research grants to LKR from the Smithsonian Institution, the Morris Animal Foundation, the International Elephant Foundation, and Ringling Bros. and Barnum and Bailey Center for Elephant Conservation. Studies at the Johns Hopkins School of Medicine were funded through NIH research grant R01 AI24576 to GSH. Protocols for collection of elephant clinical samples were reviewed and approved by the both local and/or National Zoological Park IACUC. The financial sponsors had no involvement in the experimental design, analysis or interpretation of the data. NR 21 TC 33 Z9 33 U1 1 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1135 EI 1873-2542 J9 VET MICROBIOL JI Vet. Microbiol. PD JAN 10 PY 2011 VL 147 IS 1-2 BP 28 EP 41 DI 10.1016/j.vetmic.2010.05.042 PG 14 WC Microbiology; Veterinary Sciences SC Microbiology; Veterinary Sciences GA 704FW UT WOS:000286037500004 PM 20579821 ER PT J AU Wray, JJ Milliken, RE Dundas, CM Swayze, GA Andrews-Hanna, JC Baldridge, AM Chojnacki, M Bishop, JL Ehlmann, BL Murchie, SL Clark, RN Seelos, FP Tornabene, LL Squyres, SW AF Wray, J. J. Milliken, R. E. Dundas, C. M. Swayze, G. A. Andrews-Hanna, J. C. Baldridge, A. M. Chojnacki, M. Bishop, J. L. Ehlmann, B. L. Murchie, S. L. Clark, R. N. Seelos, F. P. Tornabene, L. L. Squyres, S. W. TI Columbus crater and other possible groundwater-fed paleolakes of Terra Sirenum, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL EMISSION SPECTROMETER; YELLOWSTONE-NATIONAL-PARK; SCIENCE EXPERIMENT HIRISE; MERIDIANI-PLANUM; CLAY-MINERALS; REFLECTANCE SPECTROSCOPY; OMEGA/MARS EXPRESS; MARTIAN HIGHLANDS; INFRARED-SPECTROSCOPY; SOUTHERN HIGHLANDS AB Columbus crater in the Terra Sirenum region of the Martian southern highlands contains light-toned layered deposits with interbedded sulfate and phyllosilicate minerals, a rare occurrence on Mars. Here we investigate in detail the morphology, thermophysical properties, mineralogy, and stratigraphy of these deposits; explore their regional context; and interpret the crater's aqueous history. Hydrated mineral-bearing deposits occupy a discrete ring around the walls of Columbus crater and are also exposed beneath younger materials, possibly lava flows, on its floor. Widespread minerals identified in the crater include gypsum, polyhydrated and monohydrated Mg/Fe-sulfates, and kaolinite; localized deposits consistent with montmorillonite, Fe/Mg-phyllosilicates, jarosite, alunite, and crystalline ferric oxide or hydroxide are also detected. Thermal emission spectra suggest abundances of these minerals in the tens of percent range. Other craters in northwest Terra Sirenum also contain layered deposits and Al/Fe/Mg-phyllosilicates, but sulfates have so far been found only in Columbus and Cross craters. The region's intercrater plains contain scattered exposures of Al-phyllosilicates and one isolated mound with opaline silica, in addition to more common Fe/Mg-phyllosilicates with chlorides. A Late Noachian age is estimated for the aqueous deposits in Columbus, coinciding with a period of inferred groundwater upwelling and evaporation, which (according to model results reported here) could have formed evaporites in Columbus and other craters in Terra Sirenum. Hypotheses for the origin of these deposits include groundwater cementation of crater-filling sediments and/or direct precipitation from subaerial springs or in a deep (similar to 900 m) paleolake. Especially under the deep lake scenario, which we prefer, chemical gradients in Columbus crater may have created a habitable environment at this location on early Mars. Citation: Wray, J. J., et al. (2011), Columbus crater and other possible groundwater-fed paleolakes of Terra Sirenum, Mars, J. Geophys. Res., 116, E01001, doi:10.1029/2010JE003694. C1 [Wray, J. J.; Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Milliken, R. E.] Univ Notre Dame, Dept Civil Engn & Geol Sci, Notre Dame, IN 46556 USA. [Dundas, C. M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Swayze, G. A.; Clark, R. N.] US Geol Survey, Denver, CO 80225 USA. [Andrews-Hanna, J. C.] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA. [Baldridge, A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chojnacki, M.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Bishop, J. L.] SETI Inst, Mountain View, CA 94043 USA. [Ehlmann, B. L.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Murchie, S. L.; Seelos, F. P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Tornabene, L. L.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20024 USA. RP Wray, JJ (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM jwray@astro.cornell.edu RI Wray, James/B-8457-2008; Chojnacki, Matthew/A-4245-2013; Murchie, Scott/E-8030-2015; Seelos, Frank/C-7875-2016 OI Wray, James/0000-0001-5559-2179; Dundas, Colin/0000-0003-2343-7224; Chojnacki, Matthew/0000-0001-8497-8994; Murchie, Scott/0000-0002-1616-8751; Seelos, Frank/0000-0001-9721-941X FU Fannie & John Hertz Foundation; NSF FX We thank S. Mattson and A. Dumke for their efforts producing HiRISE and HRSC DEMs, respectively. Early reviews by J. K. Crowley, G. A. Desborough, and S. A. Wilson Purdy as well as discussions with J. F. Mustard, M. P. Golombek, N. A. Cabrol, J. A. Grant, D. J. Des Marais, V. F. Chevrier, T. S. Altheide, and S. Karunatillake improved the paper. We thank R. P. Irwin III and an anonymous reviewer for their thorough attention to the manuscript. J.J.W. thanks the Fannie & John Hertz Foundation and the NSF Graduate Research Fellowship for support. We thank the HiRISE and CRISM science and operations teams for acquiring the data most critical to our observations and interpretations. NR 223 TC 69 Z9 69 U1 5 U2 31 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JAN 5 PY 2011 VL 116 AR E01001 DI 10.1029/2010JE003694 PG 41 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 704NI UT WOS:000286059300001 ER PT J AU Greenberg, R Demarest, DW Matsuoka, SM Mettke-Hofmann, C Evers, D Hamel, PB Luscier, J Powell, LL Shaw, D Avery, ML Hobson, KA Blancher, PJ Niven, DK AF Greenberg, Russell Demarest, Dean W. Matsuoka, Steven M. Mettke-Hofmann, Claudia Evers, David Hamel, Paul B. Luscier, Jason Powell, Luke L. Shaw, David Avery, Michael L. Hobson, Keith A. Blancher, Peter J. Niven, Daniel K. BE Wells, JV TI Understanding Declines in Rusty Blackbirds SO BOREAL BIRDS OF NORTH AMERICA: A HEMISPHERIC VIEW OF THEIR CONSERVATION LINKS AND SIGNIFICANCE SE Studies in Avian Biology LA English DT Article; Book Chapter DE contaminants; Euphagus carolinus; habitat use; limiting factors; population decline; population movements; Rusty Blackbird ID ESTIMATING SITE OCCUPANCY; ALLUVIAL VALLEY; UNITED-STATES; COMMON LOONS; FOREST; MERCURY; CONSERVATION; CONTAMINATION; ECOSYSTEMS; RESPONSES AB The Rusty Blackbird (Euphagus carolinus), a formerly common breeding species of boreal wetlands, has exhibited the most marked decline of any North American landbird. North American Breeding Bird Survey (BBS) trends in abundance are estimated to be -12.5%/yr over the last 40 years, which is tantamount to a >95% cumulative decline. Trends in abundance calculated from Christmas Bird Counts (CBC) for a similar period indicate a range-wide decline of -5.6%/yr. Qualitative analyses of ornithological accounts suggest the species has been declining for over a century. Several studies document range retraction in the southern boreal forest, whereas limited data suggest that abundance may be more stable in more northerly areas. The major hypotheses for the decline include degradation of boreal habitats from logging and agricultural development, mercury contamination, and wetland desiccation resulting from global warming. Other likely reasons for decline include loss or degradation of wooded wetlands of the southeastern U. S and mortality associated with abatement efforts targeting nuisance blackbirds. In addition, the patchy breeding distribution of this species may inhibit population consolidation, causing local populations to crash when reduced to low levels. Progress in understanding the causes and mechanisms for observed declines has remained limited until recently. Here we present initial attempts to understand the habitat requirements of Rusty Blackbirds and offer specific predictions associated with each of the hypotheses for decline as a way of guiding future research. C1 [Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Evers, David] BioDivers Res Inst, Gorham, ME 04038 USA. [Hamel, Paul B.] US Forest Serv, USDA, So Hardwoods Lab, Stoneville, MS 38776 USA. [Hobson, Keith A.] Canada Canadian Wildlife Serv, Saskatoon, SK S7N 0X4, Canada. [Luscier, Jason] Univ Arkansas, Dept Biol Sci, Fayetteville, AR 72701 USA. [Matsuoka, Steven M.] US Fish & Wildlife Serv, Anchorage, AK 99503 USA. [Mettke-Hofmann, Claudia] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Liverpool L3 3AF, Merseyside, England. [Powell, Luke L.] Univ Maine, Dept Biol Sci, Orono, ME 04469 USA. [Shaw, David] Alaska Bird Observ, Fairbanks, AK 99701 USA. [Niven, Daniel K.] Natl Audubon Soc, Illinois Nat Hist Survey, Champaign, IL 61820 USA. [Avery, Michael L.] Natl Wildlife Res Ctr, Wildlife Serv, Gainesville, FL 32641 USA. [Blancher, Peter J.] Environm Canada, Natl Wildlife Res Ctr, Ottawa, ON K1A 0H3, Canada. [Demarest, Dean W.] US Fish & Wildlife Serv, Atlanta, GA 30345 USA. RP Greenberg, R (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. EM greenbergr@si.edu; dean_demarest@fws.gov; steve_matsuoka@fws.gov; mettke@erl.orn.mpg.de; david.evers@briloon.org; phamel@fs.fed.us; jluscie@uark.edu; luke.l.powell@gmail.com; dshaw@alaskabird.org; michael.l.avery@aphis.usda.gov; keith.hobson@ec.gc.ca; peter.blancher@ec.gc.ca; dniven@audubon.org NR 91 TC 7 Z9 7 U1 4 U2 18 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-95058-0 J9 STUD AVIAN BIOL JI Stud. Avian Biol. PY 2011 IS 41 BP 107 EP 125 PG 19 WC Ornithology SC Zoology GA BXG81 UT WOS:000296090000010 ER PT J AU Martin, K Wilson, S Hannon, SJ AF Martin, Kathy Wilson, Scott Hannon, Susan J. BE Sandercock, BK Martin, K Segelbacher, G TI Mechanisms Underlying Variation in Renesting Ability of Willow Ptarmigan SO ECOLOGY, CONSERVATION, AND MANAGEMENT OF GROUSE SE Studies in Avian Biology LA English DT Article; Book Chapter DE arctic tundra; bet-hedging; clutch replacement; follicle development; gonadal recrudescence; Lagopus lagopus; renest clutch size; renest interval; renesting propensity; survival-fecundity trade-off ID MALLARDS ANAS-PLATYRHYNCHOS; CLUTCH SIZE VARIATION; SPRING BODY CONDITION; NEST PREDATION; EXTREME ENVIRONMENTS; ALPINE PTARMIGAN; BLUE-GROUSE; BIRDS; REPRODUCTION; FECUNDITY AB Like many ground-nesting birds, ptarmigan are not capable of defending their clutches from most predators, relying instead on cryptic plumage and secretive behaviors to escape predation. Despite these adaptations, ptarmigan experience heavy reproductive losses (40 to 80% of first clutches) but are able to recoup some fecundity by renesting (replacing a clutch after the failure of a previous attempt). We studied two populations of Willow Ptarmigan (Lagopus lagopus) that varied in their probability of replacing a clutch, renest interval, and clutch size of renests. At the Chilkat Pass (CP) in subalpine tundra in northwestern British Columbia, where renests accounted for 14% of annual fecundity, renesting ability varied with female age-class (adult or yearling) and stage of loss. At La Perouse Bay (LPB) in subarctic tundra in Manitoba, where 23% of annual fecundity resulted from renests, probability of renesting was similar for adults and yearlings, and declined when the clutch was lost later in the incubation period. When clutches were lost during laying, females in both populations had a high probability of renesting, with LPB females able to achieve continuation laying in contrast to deterministic egg-laying for CP females. The latest stage of loss of first clutches after which females renested was day 14 of incubation at CP and day 19 at LPB. The renest interval increased with later stage of failure of first clutches at CP but not at LPB. At both sites, females that laid larger first clutches also produced larger renest clutches. Renest clutch size declined after longer renest intervals at both sites, and also with later dates of failure at LPB. Variation in renesting ability within Willow Ptarmigan populations was based mostly on stage of loss of first clutches, and not to individual traits, except for female age at CP, and with little annual variation in either population. We found no support for a bet-hedging strategy either within or between populations, as larger first clutches were correlated positively with renesting in both populations, and CP birds had lower renesting ability than LPB despite lower daily nest survival of first clutches. We found support for a survival-fecundity trade-off in renesting ability between populations since LPB females with the lower annual survival and higher dependence on annual fecundity were more able to replace their clutches after one or multiple failures. Thus, renesting ability may be under stronger selection at LPB than at CP, but in both populations, Willow Ptarmigan exhibited well-developed renesting abilities. C1 [Martin, Kathy] Univ British Columbia, Dept Forest Sci, Vancouver, BC V6T 1Z4, Canada. [Hannon, Susan J.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Wilson, Scott] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Martin, K (reprint author), Univ British Columbia, Dept Forest Sci, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM kathy.martin@ubc.ca; wilsonsd@si.edu; sue.hannon@ualberta.ca NR 54 TC 1 Z9 1 U1 0 U2 6 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-95057-3 J9 STUD AVIAN BIOL JI Stud. Avian Biol. PY 2011 IS 39 BP 233 EP 246 PG 14 WC Ornithology SC Zoology GA BZU73 UT WOS:000303012700018 ER PT J AU Touwaide, A AF Touwaide, Alain TI Ibn Baklarish's Book of Simples. Medical Remedies between Three Faiths in Twelfth-Century Spain SO EARLY SCIENCE AND MEDICINE LA English DT Book Review C1 [Touwaide, Alain] Inst Preservat Med Tradit, Washington, DC USA. [Touwaide, Alain] Smithsonian Inst, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Inst Preservat Med Tradit, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 1383-7427 J9 EARLY SCI MED JI Early Sci. Med. PY 2011 VL 16 IS 6 BP 600 EP 602 DI 10.1163/157338211X607808 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 032GE UT WOS:000310701000004 ER PT J AU Giani, VC Yamaguchi, E Boyle, MJ Seaver, EC AF Giani, Vincent C., Jr. Yamaguchi, Emi Boyle, Michael J. Seaver, Elaine C. TI Somatic and germline expression of piwi during development and regeneration in the marine polychaete annelid Capitella teleta SO EVODEVO LA English DT Article ID STEM-CELL SYSTEM; SP-I; PLATYNEREIS-DUMERILII; SEA-URCHIN; VASA; GENE; LINE; SEGMENTATION; PROTEINS; ELEGANS AB Background: Stem cells have a critical role during adult growth and regeneration. Germline stem cells are specialized stem cells that produce gametes during sexual reproduction. Capitella teleta (formerly Capitella sp. I) is a polychaete annelid that reproduces sexually, exhibits adult growth and regeneration, and thus, is a good model to study the relationship between somatic and germline stem cells. Results: We characterize expression of the two C. teleta orthologs of piwi, genes with roles in germline development in diverse organisms. Ct-piwi1 and Ct-piwi2 are expressed throughout the life cycle in a dynamic pattern that includes both somatic and germline cells, and show nearly identical expression patterns at all stages examined. Both genes are broadly expressed during embryonic and larval development, gradually becoming restricted to putative primordial germ cells (PGCs) and the posterior growth zone. In juveniles, Ct-piwi1 is expressed in the presumptive gonads, and in reproductive adults, it is detected in gonads and the posterior growth zone. In addition, Ct-piwi1 is expressed in a population of putative PGCs that persist in sexually mature adults, likely in a stem cell niche. Ct-piwi1 is expressed in regenerating tissue, and once segments differentiate, it becomes most prominent in the posterior growth zone and immature oocytes in regenerating ovaries of regenerating segments. Conclusions: In C. teleta, piwi genes may have retained an ancestral role as genetic regulators of both somatic and germline stem cells. It is likely that piwi genes, and associated stem cell co-regulators, became restricted to the germline in some taxa during the course of evolution. C1 [Giani, Vincent C., Jr.; Yamaguchi, Emi; Seaver, Elaine C.] Univ Hawaii, PBRC, Kewalo Marine Lab, Honolulu, HI 96813 USA. [Boyle, Michael J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Seaver, EC (reprint author), Univ Hawaii, PBRC, Kewalo Marine Lab, 41 Ahui St, Honolulu, HI 96813 USA. EM seaver@hawaii.edu FU National Science Foundation (REU) [10B05-44869] FX We thank Dr. Neva Meyer for confocal imaging and generation of Z-stack projection, and the following members of the Seaver lab for their continued support of this project: Dr. Neva Meyer, Dr. Aldine Amiel, and Tyler Smith. This work was supported by the National Science Foundation (REU Supplement of 10B05-44869 to E.C.S.). NR 49 TC 40 Z9 40 U1 0 U2 16 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2041-9139 J9 EVODEVO JI EvoDevo PY 2011 VL 2 AR 10 DI 10.1186/2041-9139-2-10 PG 18 WC Evolutionary Biology; Developmental Biology SC Evolutionary Biology; Developmental Biology GA 032DY UT WOS:000310693900010 PM 21545709 ER PT J AU Polyakov, YS Neilsen, J Timashev, SF AF Polyakov, Yuriy S. Neilsen, Joseph Timashev, Serge F. BE Deen, MJ Chen, CH TI Anomalous Diffusion in the Dynamics of X-ray Emission of Astrophysical Objects SO 2011 21ST INTERNATIONAL CONFERENCE ON NOISE AND FLUCTUATIONS (ICNF) LA English DT Proceedings Paper CT 21st International Conference on Noise and Fluctuations (ICNF) CY JUN 12-16, 2011 CL Toronto, CANADA SP McMaster Univ, Ryerson Univ, Univ Texas, IEEE Hamilton Sect, IEEE Elect Devices Soc, IEEE Toronto Sect, IEEE DE anomalous diffusion; flicker-noise spectroscopy; astrophysics; GRS 1915+105 ID FLICKER NOISE SPECTROSCOPY; GRS 1915+105; GRS-1915+105; VARIABILITY AB We use the anomalous-diffusion interpolation and parameterization procedure developed within the framework of flicker-noise spectroscopy (FNS) to characterize the stochastic variability of X-ray emission from accreting black hole GRS 1915+105. Our analysis of the lightcurves with a sampling frequency of 16 Hz in soft and hard X-ray energy bands shows that the stochastic variability of soft-band lightcurves is mostly subdiffusive while the hard X-ray emission is characterized primarily by fractional Gaussian noise. The comparison of FNS parameters between the soft and hard energy bands (corresponding roughly to different X-ray emission mechanisms) implies that hard X-rays have more relative variability at higher frequencies and are characterized by shorter diffusion timescales than soft X-rays. We suggest that the differences in the stochastic variabilities may be attributed to changes in either the viscosity law in the accretion disk or the geometry of the accretion flow. C1 [Polyakov, Yuriy S.] USPolyResearch, Ashland, PA USA. [Neilsen, Joseph] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Timashev, Serge F.] Inst Laser & Informat Technol, Troitsk, Russia. [Timashev, Serge F.] Karpov Inst Phys Chem, Moscow, Russia. RP Polyakov, YS (reprint author), USPolyResearch, Ashland, PA USA. EM ypolyakov@uspolyresearch.com NR 15 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4577-0192-4 PY 2011 BP 115 EP 118 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA BCC62 UT WOS:000309730300028 ER PT J AU Gibbons, TR Concepcion, GT Bachvaroff, TR Delwiche, CF AF Gibbons, Theodore R. Concepcion, Gregory T. Bachvaroff, Tsvetan R. Delwiche, Charles F. TI Evaluating short-read sequence data from the highly redundant, novel transcriptome of Polarella glacialis SO GENOME BIOLOGY LA English DT Meeting Abstract ID NUMBER C1 [Gibbons, Theodore R.; Concepcion, Gregory T.; Delwiche, Charles F.] Univ Maryland, Dept Cell Biol & Mol Genet, College Pk, MD 20742 USA. [Bachvaroff, Tsvetan R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. OI Delwiche, Charles/0000-0001-7854-8584 NR 4 TC 0 Z9 0 U1 0 U2 1 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1474-7596 J9 GENOME BIOL JI Genome Biol. PY 2011 VL 12 SU 1 MA P5 BP 6 EP 6 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA 002QH UT WOS:000308546700020 ER PT S AU Citterio, O Civitani, MM Arnold, J Campana, S Combrinck, H Conconi, P Cotroneo, V Freeman, R Mattaini, E Morton, R Motta, G Pareschi, G Parodi, G Proserpio, L Schuler, S Simpson, P Tagliaferri, G Walker, D AF Citterio, O. Civitani, M. M. Arnold, J. Campana, S. Combrinck, H. Conconi, P. Cotroneo, V. Freeman, R. Mattaini, E. Morton, R. Motta, G. Pareschi, G. Parodi, G. Proserpio, L. Schuler, S. Simpson, P. Tagliaferri, G. Walker, D. BE ODell, SL Pareschi, G TI Progress on precise grinding and polishing of thin glass monolithic shell (towards WFXT) SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 23-25, 2011 CL San Diego, CA SP SPIE DE X-Ray Telescopes; Wolter; Mirror Shells; X-Ray Shells; Grazing-Incidence; Deterministic Polishing ID RAY; TELESCOPE; OPTICS AB The next generation wide-field X-ray telescope (WFXT) will require an angular resolution of similar to 5-10 arcsec almost constant across a wide field of view (similar to 1 deg(2) diameter). To achieve this goal, the design of the optical system has to be based on mirrors characterized by short length and polynomial profiles, as well as focal plane curvature and plate scale corrections. These concepts guarantee an improved angular resolution at large off-axis angle with respect to the normally used Wolter-I configuration. These telescopes are therefore optimal for survey purposes. A significant increase of effective area and grasp with respect to previous missions must also be achieved. This is possible with high precision but at the same time thin (2-3 mm thickness for mirror diameters of 30-110 cm) glass mirror shells. To achieve the goal of 5 arcsec and improve further the technology, we are considering different materials. Fused silica, a well-known material with good thermo-mechanical and polishability characteristics provide the best choice. To bring the mirror shells to the needed accuracy, we are adopting a deterministic direct polishing method (already used for past missions as Einstein, Rosat, Chandra). The technological challenge now is to apply it for almost ten times thinner shells. C1 [Citterio, O.; Civitani, M. M.; Campana, S.; Conconi, P.; Cotroneo, V.; Mattaini, E.; Motta, G.; Pareschi, G.; Proserpio, L.; Tagliaferri, G.] INAF OAB Astron Observ Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy. [Civitani, M. M.; Proserpio, L.] Insubria Univ, I-22100 Como, Italy. [Arnold, J.; Schuler, S.] LT Ultra Precis Technol GmbH, D-88634 Schonch, Germany. [Combrinck, H.; Freeman, R.; Morton, R.; Simpson, P.; Walker, D.] ZEEKO Ltd, Leicestershire LE673FW, England. [Cotroneo, V.] Harvard Smithsonian, Ctr Astrophys, Cambridge, MA 02138 USA. [Parodi, G.] BCV Progetti, I-20123 Milan, Italy. [Mattaini, E.] INAF, IASF Milano, I-20133 Milan, Italy. RP Citterio, O (reprint author), INAF OAB Astron Observ Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy. EM oberto.citterio@brera.inaf.it OI Campana, Sergio/0000-0001-6278-1576; Pareschi, Giovanni/0000-0003-3967-403X; Walker, David/0000-0002-6687-024X; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU ASI; INAF FX This work is supported by ASI and INAF grants. We are grateful to the WFXT collaboration and, in particular, to S. Murray and R. Giacconi, for supporting this work and many useful discussions. We acknowledge Heraeus Quarzglas mbH & Co KG for the manufacturing of the raw glass shells. NR 7 TC 3 Z9 3 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8757-5 J9 PROC SPIE PY 2011 VL 8147 AR 814714 DI 10.1117/12.895309 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BBA80 UT WOS:000306321500038 ER PT S AU Cotroneo, V Davis, WN Reid, PB Schwartz, DA Trolier-McKinstry, S Wilke, RHT AF Cotroneo, Vincenzo Davis, William N. Reid, Paul B. Schwartz, Daniel A. Trolier-McKinstry, Susan Wilke, Rudeger H. T. BE ODell, SL Pareschi, G TI Adjustable grazing incidence x-ray optics: measurement of actuator influence functions and comparison with modeling SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 23-25, 2011 CL San Diego, CA SP SPIE DE X-ray telescopes; Adaptive Optics; X-ray Mirrors; PZT; Figure Correction AB The present generation of X-ray telescopes emphasizes either high image quality (e.g. Chandra with sub-arc second resolution) or large effective area (e.g. XMM-Newton), while future observatories under consideration (e.g. Athena, AXSIO) aim to greatly enhance the effective area, while maintaining moderate (similar to 10 arc-seconds) image quality. To go beyond the limits of present and planned missions, the use of thin adjustable optics for the control of low-order figure error is needed to obtain the high image quality of precisely figured mirrors along with the large effective area of thin mirrors. The adjustable mirror prototypes under study at Smithsonian Astrophysical Observatory are based on two different principles and designs: 1) thin film lead-zirconate-titanate (PZT) piezoelectric actuators directly deposited on the mirror back surface, with the strain direction parallel to the glass surface (for sub-arc-second angular resolution and large effective area), and 2) conventional lead-magnesium-niobate (PMN) electrostrictive actuators with their strain direction perpendicular to the mirror surface (for 3-5 arc second resolution and moderate effective area). We have built and operated flat test mirrors of these adjustable optics. We present the comparison between theoretical influence functions as obtained by finite element analysis and the measured influence functions obtained from the two test configurations. C1 [Cotroneo, Vincenzo; Davis, William N.; Reid, Paul B.; Schwartz, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cotroneo, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vcotroneo@cfa.harvard.edu OI Trolier-McKinstry, Susan/0000-0002-7267-9281 NR 11 TC 3 Z9 3 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8757-5 J9 PROC SPIE PY 2011 VL 8147 AR 81471R DI 10.1117/12.895475 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BBA80 UT WOS:000306321500060 ER PT S AU Gorenstein, P AF Gorenstein, Paul BE ODell, SL Pareschi, G TI Large-angle OBServaTory with Energy Resolution for Synoptic X-ray Studies (LOBSTER-SXS) SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 23-25, 2011 CL San Diego, CA SP SPIE DE X-ray telescopes; lobster-eye telescopes; X-ray variability ID EMISSION; BURSTS; SUPERNOVA; REDSHIFT; MISSION AB The soft X-ray band hosts a larger, more diverse range of variable sources than any other region of the electromagnetic spectrum. They are stars, compact binaries, SMBH's, the X-ray components of Gamma-Ray Bursts, their X-ray afterglows, and soft X-ray flares from supernova. We describe a concept for a very wide field (similar to 4 ster) modular hybrid X-ray telescope system that can measure positions of bursts and fast transients with as good as arc second accuracy, the precision required to identify fainter and increasingly more distant events. The dimensions and materials of all telescope modules are identical. All but two are part of a cylindrical lobster-eye telescope with flat double sided mirrors that focus in one dimension and utilize a coded mask for resolution in the other. Their positioning accuracy is about an arc minute. The two remaining modules are made from the same materials but configured as a Kirkpatrick-Baez telescope with longer focal length that focuses in two dimensions. When pointed it refines the hybrid telescope's arc minute positions to an arc second and provides larger effective area for spectral and temporal measurements. Above 10 keV the mirrors act as an imaging collimator with positioning capability. For short duration events this hybrid focusing/coded mask system is more sensitive and versatile than either a 2D coded mask or a 2D lobster-eye telescope. Very wide field X-ray telescopes have become feasible as the ability to fabricate large area arrays of CCD and CMOS detectors has improved. This instrument's function in the soft X-ray band is similar to that of Swift in hard X-ray band and there is a larger variety of fast transients in the soft X-ray band. An instrument with considerably more sensitivity than current wide field X-ray detectors would be compatible with a modest NASA Explorer mission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-4, Cambridge, MA 02138 USA. EM goren@cfa.harvard.edu NR 38 TC 2 Z9 2 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8757-5 J9 PROC SPIE PY 2011 VL 8147 AR 81471O DI 10.1117/12.890247 PG 15 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BBA80 UT WOS:000306321500057 ER PT S AU Romaine, S Boike, J Bruni, R Engelhaupt, D Gorenstein, P Ramsey, B AF Romaine, S. Boike, J. Bruni, R. Engelhaupt, D. Gorenstein, P. Ramsey, B. BE ODell, SL Pareschi, G TI Improved release coatings for electroformed X-ray optics SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 23-25, 2011 CL San Diego, CA SP SPIE DE X-ray optics; TiN; electroformed optics; release layer; multilayers AB X-ray astronomy grazing incidence telescopes use the principle of nested shells to maximize the collecting area. Some of the more recent missions, such as XMM-Newton [1], have used an electroformed nickel replication (ENR) process [2] to fabricate the mirror shells. Upcoming missions, such as Spectrum-Rontgen-Gamma [3] and Focusing Optics X-ray Solar Imager([4]), also use the electroforming process to fabricate nested shell grazing incidence X-ray telescopes. We present recent results on fabrication of replicas with multilayer coatings from Wolter-1 mandrels using a new hardcoat release material to simplify and improve this electroforming process. C1 [Romaine, S.; Bruni, R.; Gorenstein, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romaine, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sromaine@cfa.harvard.edu NR 10 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8757-5 J9 PROC SPIE PY 2011 VL 8147 AR 81470W DI 10.1117/12.896000 PG 6 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BBA80 UT WOS:000306321500030 ER PT S AU Schwartz, DA Cotroneo, V Davis, W Freeman, M Reid, P AF Schwartz, Daniel A. Cotroneo, Vincenzo Davis, William Freeman, Mark Reid, Paul BE ODell, SL Pareschi, G TI Adjustable X-ray optics: correction for gravity-induced figure errors SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 23-25, 2011 CL San Diego, CA SP SPIE DE X-ray optics; grazing incidence telescopes; adjustable optics; X-ray astronomy AB To extend the effective collecting area for future X-ray astronomy observatories, it is necessary to use highly nested, very thin glass shells. The capability to adjust the figure of these shells on-orbit is essential in order to achieve the present X-ray imaging capability, of order 1/2 arcsec resolution, which is provided to astronomers world-wide by the Chandra X-ray Observatory. We are pursuing concepts to carry out this adjustment using piezoelectric crystals deposited directly on the back sides of the reflectors, and divided into a pattern of discrete actuators by individually controlled electrodes. In this paper we carry out a simulation of how well gravity induced errors might be corrected by this process. We consider a conical glass piece 205 mm axially by 410 mm azimuthally, and with 1 m radius of curvature. We do a finite element analysis to calculate the influence function of each of a set of 20 x 20 piezo pixels. Then we apply a 1g force axially, using various constraint conditions, and calculate the coefficients of the set of influence functions such that the adjusted shape minimizes the slope errors. C1 [Schwartz, Daniel A.; Cotroneo, Vincenzo; Davis, William; Freeman, Mark; Reid, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@cfa.harvard.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8757-5 J9 PROC SPIE PY 2011 VL 8147 AR 81471S DI 10.1117/12.895557 PG 9 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BBA80 UT WOS:000306321500061 ER PT S AU Kenter, AT Kraft, R Murray, SS Alcock, C Gauron, T AF Kenter, A. T. Kraft, R. Murray, S. S. Alcock, C. Gauron, T. BE MacEwen, HA Breckinridge, JB TI Laboratory Prototype Camera for the Whipple Mission: a Mission to Detect and Categorize Small Objects in our Solar System SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES AND CONCEPTS V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on UV/Optical/IR Space Telescopes and Instruments - Innovative Technologies and Concepts V CY AUG 21-24, 2011 CL San Diego, CA SP SPIE DE CMOS image detector; HyViSI; blind Occultation ID KUIPER-BELT OBJECTS; STELLAR OCCULTATIONS AB The proposed Whipple mission is intended to detect Trans-Neptunian Objects (TNOs) via the "blind" occultation technique. The size, number and spatial distribution of these objects provides critical input to evolutionary models of our solar system. The Whipple project was proposed as a NASA Discovery class mission in 2010 and though not selected, it was funded to continue technology development. As part of the proposal preparation, a functional segment of the focal plane was instrumented in the laboratory. The purpose of this test segment was to verify basic detector parameters such as read noise and to detect simulated occultation events. We describe the operation of the detector and a simulator to test and verify the candidate focal plane for the proposed Whipple mission. This paper describes the design, construction and operation of the Whipple event simulator and operation of the laboratory detector. C1 [Kenter, A. T.; Kraft, R.; Alcock, C.; Gauron, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kenter, AT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM akenter@cfa.harvard.edu NR 12 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8756-8 J9 PROC SPIE PY 2011 VL 8146 AR 814612 DI 10.1117/12.894626 PG 9 WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic Technology GA BBA82 UT WOS:000306323000037 ER PT S AU Allen, B Hong, J Grindlay, J Burke, M Barthelmy, S Baker, R Harrison, F Mao, P Cook, W AF Allen, Branden Hong, Jaesub Grindlay, Jonathan Burke, Michael Barthelmy, Scott Baker, Robert Harrison, Fiona Mao, Peter Cook, William GP IEEE TI Development of the ProtoEXIST2 Advanced CZT Detector Plane SO 2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC) SE IEEE Nuclear Science Symposium Conference Record LA English DT Proceedings Paper CT IEEE Nuclear Science Symposium/Medical Imaging Conference (NSS/MIC)/18th International Workshop on Room-Temperature Semiconductor X-Ray and Gamma-Ray Detectors CY OCT 23-29, 2011 CL Valencia, SPAIN SP IEEE, Inst Elect & Elect Engineers Nucl & Plasma Sci Soc (IEEE NPSS) DE CdZnTe; Astronomy; X-ray; Gamma-ray; Radiation Detection; Pixel Distortion; Distortion Mapping ID MISSION; ISGRI; BAT AB The ProtoEXIST program was conceived for the development of a highly scalable detector plane architecture utilizing pixilated CdZnTe (CZT) detectors for eventual deployment in a large scale (1-4 m(2) active area) coded aperture X-ray telescope. Development is now underway for ProtoEXIST2, which ultimately will be comprised of a closely tiled 8x8 array of 19.9 mm x 19.9 mm, 5 mm thick Redlen CZT crystals, analogous to ProtoEXIST1, but will now utilize the NuASIC which accommodates the direct bonding of CZT detectors with a 32x32 pixilated anode with a 604.8 mu m pixel pitch and a guard ring surrounding the perimeter of the anode pattern. Currently 6 prototype detectors have been fabricated and tested. An energy threshold of approximately 6 keV and energy resolutions of 2.5 keV FWHM at 122.0 keV and 2.1 keV at 59.6 keV have been achieved with individual detectors. The performance and energy resolution of the individual prototype detectors is discussed in detail. In addition, during preliminary testing of the prototype ProtoEXIST2 detectors reduced photopeak efficiency and pixel distortions were observed for pixels within approximately 3 mm of the CZT edge. These distortions have been largely corrected with two independent techniques: the application of an 73 mm x 73 mm extended cathode centered directly above the detector and the use of a grounded, 6mm tall, electrostatic side shield surrounding the perimeter of the detector. The effects of the side shield and extended cathode are covered in detail. C1 [Allen, Branden; Hong, Jaesub; Grindlay, Jonathan; Burke, Michael] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Barthelmy, Scott; Baker, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Harrison, Fiona; Mao, Peter; Cook, William] CALTECH, Pasadena, CA 91125 USA. RP Allen, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ballen@cfa.harvard.edu FU NASA grants to Harvard [NNX09A076G, NNX11AF35G] FX We thank Alexi Bolitinokov for discussion in the early phases of testing. This work was supported by NASA grants to Harvard, NNX09A076G and NNX11AF35G. NR 21 TC 5 Z9 5 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1082-3654 BN 978-1-4673-0120-6 J9 IEEE NUCL SCI CONF R PY 2011 BP 4470 EP 4480 PG 11 WC Engineering, Electrical & Electronic; Physics, Applied; Imaging Science & Photographic Technology; Radiology, Nuclear Medicine & Medical Imaging SC Engineering; Physics; Imaging Science & Photographic Technology; Radiology, Nuclear Medicine & Medical Imaging GA BAM64 UT WOS:000304755604149 ER PT B AU West, CF AF West, Catherine Foster BE Taylor, AK Stein, JK TI Bone and Antler Tools SO IS IT A HOUSE? ARCHAEOLOGICAL EXCAVATIONS AT ENGLISH CAMP, SAN JUAN ISLAND, WASHINGTON SE Burke Museum of Natural History and Culture Research Report LA English DT Article; Book Chapter C1 Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP West, CF (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM foster.west@gmail.com NR 18 TC 0 Z9 0 U1 0 U2 0 PU BURKE MUSEUM NATURAL HISTORY & CULTURE PI SEATTLE PA UNIV WASHINGTON, BOX 353010, SEATTLE, WA 98195 USA BN 978-0-295-99147-4 J9 BURKE MUS NAT HIS PY 2011 VL 9 BP 95 EP 101 PG 7 WC Archaeology SC Archaeology GA BZV28 UT WOS:000303027300008 ER PT S AU Oberg, KI Boogert, ACA Pontoppidan, KM van den Broek, S van Dishoeck, EF Bottinelli, S Blake, GA Evans, NJ AF Oeberg, Karin I. Boogert, A. C. Adwin Pontoppidan, Klaus M. van den Broek, Saskia van Dishoeck, Ewine F. Bottinelli, Sandrine Blake, Geoffrey A. Evans, Neal J., II BE Cernicharo, J Bachiller, R TI Ices in Starless and Starforming Cores SO MOLECULAR UNIVERSE SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 280th Symposium of the International Astronomical Union CY MAY 30-JUN 03, 2011 CL Toledo, SPAIN SP Int Astronom Union, Minist Ciencia & Technologia, Consejo Superior Investigac Cientificas, Inst Nacl Tecnica Aeoroespacial, Inst Geograf Nacl, Univ Castilla Mancha DE astrochemistry; astrobiology; line: identification; line: profiles; molecular processes; circumstellar matter; ISM: molecules; infrared: ISM ID SPITZER SPECTROSCOPIC SURVEY; YOUNG STELLAR OBJECTS; LOW-MASS STARS; GRAIN-SURFACE-CHEMISTRY; CARBON-DIOXIDE; MU-M; INTERSTELLAR ICES; MOLECULAR OUTFLOW; COMPLEX CHEMISTRY; FORMING REGIONS AB Icy grain mantles are commonly observed through infrared spectroscopy toward dense clouds, cloud cores; protostellar envelopes and protoplanetary disks. Up to 80% of the available oxygen, carbon and nitrogen are found in such ices; the most common ice constituents - H2O, CO2 and CO - are second in abundance only to H-2 in many star forming regions. In addition to being a molecular reservoir, ice chemistry is responsible for much of the chemical evolution from H2O to complex, prebiotic molecules. Combining the exisiting ISO, Spitzer, VLT and Keck ice data results in a. large sample of ice sources (similar to 80) that span all stages of star formation and a large range of protostellar luminosities (<0.1-10(5) L-circle dot). Here we summarize the different techniques that have been applied to mine this ice data set on information on typical ice compositions in different environments and what this implies about how ices form and evolve during star and planet formation. The focus is on how to maximize the use of empirical constraints from ice observations; followed by the application of information from experiments and models. This strategy is used to identify ice bands and to constrain which ices form early during cloud formation, which form later in the prestellar core and which require protostellar heat and/or UV radiation to form. The utility of statistical tests, survival analysis and ice maps is highlighted; the latter directly reveals that the prestellar ice formation takes place in two phases, associated with H2O and CO ice formation, respectively, and that most protostellar ice variation can be explained by differences in the prestellar CO ice formation stage. Finally, special attention is paid to the difficulty of observing complex ices directly and how gas observations, experiments and models help in constraining this ice chemistry stage. C1 [Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02139 USA. EM koberg@efa.harvard.edu; ewine@strw.leidenuniv.nl; sandrine.bottinelli@cesr.fr; gab@gps.caltech.edu NR 61 TC 2 Z9 2 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01980-5 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 IS 280 BP 65 EP 78 DI 10.1017/S1743921311024872 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAT30 UT WOS:000305449300007 ER PT S AU Galvan-Madrid, R Zhang, Q Keto, ER Rodriguez, LF Ho, PTP AF Galvan-Madrid, R. Zhang, Q. Keto, E. R. Rodriguez, L. F. Ho, P. T. P. BE Henney, WJ TorresPeimbert, S TI ON THE FORMATION OF THE MOST MASSIVE STARS IN THE GALAXY SO XIII LATIN AMERICAN REGIONAL IAU MEETING SE Revista Mexicana de Astronomia y Astrofisica-Serie de Conferencias LA English DT Proceedings Paper CT 13th Latin American Regional Meeting of the International Astronomical Union CY NOV 08-12, 2010 CL Morelia, MEXICO SP Int Astronom Union, Univ Nacl Autonoma Mexico, Coordinac Invest Cientif, Univ Nacl Autonoma Mexico, Ctr Radioastronimia Astrofis, Mexican Natl Sci & Technol Council, Michoacan State Govt, Michoacan State Sci & Technol Council DE H II regions; ISM: individual objects (W33A, G12.91-0.26, G20.08-0.14); stars: formation ID REGIONS AB We present results of Submillimeter Array (SMA) and Very Large Array (VLA) studies of massive-star formation regions in the early stages of ionization. Molecular-line and ionized-gas observations at resolutions down to 0.3 '' reveal the presence of rotation, infall, and/or outflow from parsec scales to < 0.05 pc. The centers of star formation harbor small groups of massive (proto)stars at different evolutionary stages. These observations favor a picture in which: (i) Stars with M-star > 15 M-circle dot form by accretion processes similar to those of lower-mass stars, but with significant ionization. (ii) The molecular cores from which these stars form continue accreting from their environment. (iii) Accretion to the star can continue past the onset of ionization. C1 [Galvan-Madrid, R.; Zhang, Q.; Keto, E. R.; Ho, P. T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Galvan-Madrid, R (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM rgal-van@cfa.harvard.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 BN 978-607-02-2653-3 J9 REV MEX AST ASTR PY 2011 VL 40 BP 239 EP 240 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAR34 UT WOS:000305259300122 ER PT S AU Galvan-Madrid, R Peters, T Keto, ER Mac Low, MM Banerjee, R Klessen, RS AF Galvan-Madrid, R. Peters, T. Keto, E. R. Mac Low, M. -M. Banerjee, R. Klessen, R. S. BE Henney, WJ TorresPeimbert, S TI TIME VARIABILITY IN SIMULATED ULTRACOMPACT AND HYPERCOMPACT H II REGIONS SO XIII LATIN AMERICAN REGIONAL IAU MEETING SE Revista Mexicana de Astronomia y Astrofisica-Serie de Conferencias LA English DT Proceedings Paper CT 13th Latin American Regional Meeting of the International Astronomical Union CY NOV 08-12, 2010 CL Morelia, MEXICO SP Int Astronom Union, Univ Nacl Autonoma Mexico, Coordinac Invest Cientif, Univ Nacl Autonoma Mexico, Ctr Radioastronimia Astrofis, Mexican Natl Sci & Technol Council, Michoacan State Govt, Michoacan State Sci & Technol Council ID MASSIVE STARS; MORPHOLOGIES; ACCRETION AB Observations of ultracompact and hypercompact H II regions have shown time variations in their radio-continuum flux (Franco-Hernandez & Rodriguez 2004; Galvan-Madrid et al. 2008), suggesting that (some of) these ionized regions harbor stars that-are still accreting from an infalling neutral accretion flow that becomes ionized in its innermost part (Keto 2007). We present an analysis of the flux variation of H II regions formed in the simulations incorporating self-gravity and both ionizing and non-ionizing radiation presented by Peters et al. (2010a,b,c). According to this model, a small but non-negligible fraction (similar to 10%) of observed H II regions should have detectable flux variations (larger than 10%) in timescales of 10 years. C1 [Galvan-Madrid, R.; Keto, E. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Galvan-Madrid, R (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM rgal-van@cfa.harvard.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 BN 978-607-02-2653-3 J9 REV MEX AST ASTR PY 2011 VL 40 BP 273 EP 273 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAR34 UT WOS:000305259300144 ER PT S AU Offner, SSR AF Offner, Stella S. R. BE Alves, J Elmegreen, BG Girart, JM Trimble, V TI The Effects of Radiation Feedback on Early Fragmentation and Stellar Multiplicity SO COMPUTATIONAL STAR FORMATION SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 270th Symposium of the International-Astronomical-Union on Computational Star Formation CY MAY 31-JUN 04, 2010 CL Barcelona, SPAIN SP Int Astron Union, Ctr Astron Hispano Aleman Calar Alto, Minist Ciencia & Innovac, Consejo Superior Investigac Cientificas, AGAUR, Generalitat Catalunya, Univ Barcelona DE stars:formation; binaries; hydrodynamics; turbulence; radiative transfer ID INITIAL MASS FUNCTION; STAR-FORMATION; DISKS; SYSTEMS; ORIGIN; CORES AB Forming stars emit a. significant amount of radiation into their natal environment. While the importance of radiation feedback from high-mass stars is widely accepted, radiation has generally been ignored in simulations of low-mass star formation. I use ORION, an adaptive mesh refinement (AMR) three-dimensional gravito-radiation-hydrodynamics code, to model low-mass star formation in a turbulent molecular cloud. I demonstrate that including radiation feedback has a profound effect on fragmentation and protostellar multiplicity. Although heating is mainly confined within the core envelope, it is sufficient to suppress disk fragmentation that would otherwise result in low-mass companions or brown dwarfs. As a consequence, turbulent fragmentation, not disk fragmentation, is likely the origin of low-mass binaries. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Offner, SSR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM soffner@cfa.harvard.edu NR 15 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-52176-643-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 IS 270 BP 231 EP 234 DI 10.1017/S1743921311000433 PG 4 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA BAQ12 UT WOS:000305161200035 ER PT S AU Goodman, AA AF Goodman, Alyssa A. BE Alves, J Elmegreen, BG Girart, JM Trimble, V TI A Guide to Comparisons of Star Formation Simulations with Observations SO COMPUTATIONAL STAR FORMATION SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 270th Symposium of the International-Astronomical-Union on Computational Star Formation CY MAY 31-JUN 04, 2010 CL Barcelona, SPAIN SP Int Astron Union, Ctr Astron Hispano Aleman Calar Alto, Minist Ciencia & Innovac, Consejo Superior Investigac Cientificas, AGAUR, Generalitat Catalunya, Univ Barcelona DE star formation; simulations; statistical comparisons ID FORMING MOLECULAR CLOUDS; MASS FUNCTION; MAGNETIC-FIELDS; DARK CLOUDS; SUPERSONIC TURBULENCE; INTERSTELLAR CLOUDS; THEORETICAL-MODELS; GRAIN ALIGNMENT; SPECTRAL INDEX; COLUMN DENSITY AB We review an approach to observation-theory comparisons we call "Taste-Testing." In this approach, synthetic observations are made of numerical simulations, and then both real and synthetic observations are "tasted" (compared) using a variety of statistical tests. We first lay out arguments for bringing theory to observational space rather than observations to theory space. Next, we explain that generating synthetic observations is only a step along the way to the quantitative, statistical, taste tests that offer the most insight. We offer a set of examples focused on polarimetry, scattering and emission by dust, and spectral-line mapping in star-forming regions. We conclude with a discussion of the connection between statistical tests used to date and the physics we seek to understand. In particular, we suggest that the "lognormal" nature of molecular clouds can be created by the interaction of many random processes, as can the lognormal nature of the IMF, so that the fact that both the "Clump Mass Function" (CMT') and IMF appear lognormal does not necessarily imply a direct relationship between them. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA. RP Goodman, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02318 USA. EM agoodman@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 46 TC 1 Z9 1 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-52176-643-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 IS 270 BP 511 EP 519 DI 10.1017/S1743921311000901 PG 9 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA BAQ12 UT WOS:000305161200082 ER PT S AU Perets, HB Murray-Clay, R AF Perets, Hagai B. Murray-Clay, Ruth BE Sozzetti, A Lattanzi, MG Boss, AP TI Wind-shearing in gaseous protoplanetary disks SO ASTROPHYSICS OF PLANETARY SYSTEMS: FORMATION, STRUCTURE, AND DYNAMICAL EVOLUTION SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 276th Symposium of the International-Astronomical-Union on Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution CY OCT 10-15, 2010 CL Torino, ITALY SP Int Astronom Union Div 3, Int Astronom Union Commiss 51, Int Astronom Union Commiss 53, Ist Nazl Astrofis, Osservatorio Astronom Torino DE planets and satellites: dynamical evolution and stability; planets and satellites: formation; planetary systems: protoplanetary disks ID PLANET FORMATION AB One of the first stages of planet formation is the growth of small planetesimals and their accumulation into large planetesimals and planetary embryos. This early stage occurs much before the dispersal of most of the gas from the protoplanetary disk. Due to their different aerodynamic properties, planetesimals of different sizes/shapes experience different drag forces from the gas at these stage. Such differential forces produce a wind-shearing effect between close by, different size planetesimals. For any two planetesimals, a wind-shearing radius can be considered, at which the differential acceleration due to the wind becomes greater than the mutual gravitational pull between the planetesimals. We find that the wind-shearing radius could be much smaller than the gravitational shearing radius by the Sun (the Hill radius), i.e. during the gas-phase of the disk wind-shearing could play a more important role than tidal perturbations by the Sun. Here we study the wind-shearing radii for planetesimal pairs of different; sizes and compare it with gravitational shearing (drag force vs. gravitational tidal forces). We then discuss the role of wind-shearing for the stability and survival of binary planetesimals, and provide stability criteria, for binary planetesimals embedded in a gaseous disk. C1 [Perets, Hagai B.; Murray-Clay, Ruth] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02338 USA. RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02338 USA. EM hperets@cfa.harvard.edu RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X NR 4 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-19652-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 VL 276 BP 453 EP 454 DI 10.1017/S174392131102076X PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAN65 UT WOS:000304838200091 ER PT S AU Pe'er, A Casella, P AF Pe'er, Asaf Casella, Piergiorgio BE Romero, GE Sunyaev, RA Belloni, TM TI A new model of emission from microquasar jets, and possible explanation to the outliers of the fundamental plane SO JETS AT ALL SCALES SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 275th Symposium of the International-Astronomical-Union on Jets at All Scales CY SEP 13-17, 2010 CL Buenos Aires, ARGENTINA SP IAU Div 10, IAU Div 11, Inst Argentino Radioastronomia DE plasmas; radiation mechanisms: non-thermal; stars: winds; outflows; X-rays: binaries AB We present a new model of emission from jets in microquasars, which implements elements from the study of jets in gamma-ray bursts to these objects. By assuming that electrons are accelerated once at the base of the jet to a power law distribution above a, low energy Maxwellian, and are cooled by synchrotron emission and possible adiabatic energy losses along the jet, a wealth of spectra can be obtained. We show our theoretical results which can explain some of the key observations. In particular, we show that: (I) a flat radio spectrum, as is frequently seen, is a natural outcome of the model; (II) Strong magnetic field results in a flux decay in the optical/UV band as F-nu similar to nu(-1/2), irrespective of many of the uncertainties of the model. (III) Arm increase of the magnetic field above a critical value of similar to 10(5) G leads to a, sharp decrease in the flux at the radio band, while the flux at higher frequencies saturates to a constant value. We conclude that scatter in the values of the magnetic field may provide a natural explanation to the observed scatter in the radio/X. ray luminosity correlation seen in these objects. C1 [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pe'er, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apeer@cfa.harvard.edu OI Casella, Piergiorgio/0000-0002-0752-3301 NR 5 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-52176-607-4 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 VL 275 BP 303 EP 304 DI 10.1017/S1743921310016212 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAP08 UT WOS:000304974800064 ER PT S AU Dupree, AK AF Dupree, Andrea K. BE Choudhary, DP Strassmeier, KG TI Spots on Betelgeuse, what are they? SO PHYSICS OF SUN AND STAR SPOTS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 273th Symposium of the International-Astronomical-Union CY AUG 22-26, 2010 CL Ventura, CA SP IAU Div 2, California State Univ, Dept Phys & Astron DE stars: supergiants; stars: imaging ID ALPHA-ORIONIS; EXTENDED ATMOSPHERE; CONVECTION; SUPERGIANTS; STARS AB The supergiant star Alpha Orionis (Betelgeuse) is the only star other than the Sun to be spatially resolved either through direct imaging or through reconstruction of interferometric observations. Centimeter-radio wavelength, infrared and ultraviolet images reveal a few bright hot spots in the photosphere and chromosphere that possess characteristics different from sunspots. Large photospheric spots on Betelgeuse appear to result from convective motions, consistent with radiative hydrodynamic modeling; the chromospheric hot spots may be produced by shock waves in the chromosphere excited by the convective motions or pulsation in the photosphere. Bright chromospheric spots that cluster around the pole of Betelgeuse could be a natural result of shock breakout in a rotating star. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM dupree@cfa.harvard.edu NR 25 TC 2 Z9 2 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-76062-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 VL 273 BP 188 EP 194 DI 10.1017/S1743921311015225 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAO38 UT WOS:000304890800031 ER PT S AU Gingerich, O AF Gingerich, Owen BE VallsGabaud, D Boksenberg, A TI Kepler, Galileo and the birth of modern astronomy SO ROLE OF ASTRONOMY IN SOCIETY AND CULTURE SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 260th Symposium of the International-Astronomical-Union CY JAN 19-23, 2009 CL UNESCO, Paris, FRANCE SP Observ Paris, Int Astronom Union, Acad Sci Paris, Inst Natl Sci Univ, Region Ile France HO UNESCO DE Kepler; Galileo; ellipse; telescope; Astronomia nova; Sidereus nuncius AB The International Year of Astronomy marks the 400th anniversary of Kepler's Astronomia nova and the first use of the telescope for astronomy, most notably leading to Galileo's Sidereus nuncius (1610). Kepler's book for the first time argued strongly for a physical basis to astronomical explanations. Galileo's work showed that a coherent understanding was more important for scientific progress than specific proofs. The efforts of both astronomers undermined the traditional geocentric cosmology and essentially brought about the birth of modern astronomy. C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ginger@cfa.harvard.edu NR 6 TC 0 Z9 0 U1 0 U2 4 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-76477-3 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 IS 260 BP 172 EP 181 DI 10.1017/S1743921311002250 PG 10 WC Astronomy & Astrophysics; History & Philosophy Of Science; Social Sciences, Interdisciplinary SC Astronomy & Astrophysics; History & Philosophy of Science; Social Sciences - Other Topics GA BAM51 UT WOS:000304684000021 ER PT B AU Matthews, LD Gerard, E Johnson, MC Le Bertre, T Libert, Y Reid, MJ AF Matthews, L. D. Gerard, E. Johnson, M. C. Le Bertre, T. Libert, Y. Reid, M. J. BE Kerschbaum, F Lebzelter, T Wing, RF TI Tails of Stellar Mass-Loss: VLA Imaging of H I in Circumstellar Envelopes SO WHY GALAXIES CARE ABOUT AGB STARS II: SHINING EXAMPLES AND COMMON INHABITANTS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Why Galaxies Care About AGB Stars II: Shining Examples and Common Inhabitants CY AUG 16-20, 2010 CL Univ Campus, Vienna, AUSTRIA HO Univ Campus ID ASYMPTOTIC GIANT BRANCH; LOSS HISTORY; EVOLVED STARS; DISCOVERY; HYDROGEN; MIRA; WAKE; GAS; AGB AB Because neutral atomic hydrogen (H I) is not destroyed by the interstellar radiation field in circumstellar environments, its 21-cm line transition can be used to trace circumstellar envelopes at significantly larger distances from the star than molecular lines (up to a parsec or more), thereby probing the stellar mass-loss history over very extended time-scales. The H I line also supplies unique kinematic information on the interaction between the CSE and its interstellar environment. During the past several years, our group has been using the Very Large Array (VLA) to study the mass-loss histories of evolved stars via their H I 21-cm line emission. Here we highlight some recent results from our on-going VLA surveys, including the discovery of extended H I "tails," shells, and other structures associated with a number of well-known AGB stars. We also describe how our results can be used to place new constraints on mass-loss time-scales during the AGB, as well as on the interplay between mass-losing stars and the interstellar medium. C1 [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. [Gerard, E.] GEPI, Observ Paris, Meudon, France. [Johnson, M. C.] Wesleyan Univ, Dept Astron, Middletown, CT USA. [Le Bertre, T.] Domaine Univ, IRAM, St Martin Dheres, France. [Libert, Y.] LERMA, Observ Paris, Paris, France. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Matthews, LD (reprint author), MIT, Haystack Observ, Westford, MA 01886 USA. NR 15 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-770-4 J9 ASTR SOC P PY 2011 VL 445 BP 305 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAH05 UT WOS:000304132300056 ER PT B AU Brickhouse, NS AF Brickhouse, Nancy S. BE JohnsKrull, CMJ Browning, MK West, AA TI Accretion Makes a Splash on TW Hydrae SO 16TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 16th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY AUG 28-SEP 03, 2010 CL Univ Washington, Seattle, WA SP Natl Sci Fdn, NASA Astrobiol Inst, European Space Agcy, Astrophys Res Consortium/Apache Point Observ, Univ Washington Coll Arts & Sci, Univ Washington Dept Astron HO Univ Washington ID EMISSION-LINE DIAGNOSTICS; TAURI-STARS; MAGNETOSPHERIC ACCRETION; DISK ACCRETION; VARIABILITY; CHANDRA; PLASMA; WINDS AB The Chandra Large Program on the Classical T Tauri star TW Hydrae (489 ksec, obtained over the course of one month) brings a wealth of spectral diagnostics to the study of X-ray emission from a young star. The emission measure distribution shows two components separated by a gap (i.e. no emission measure in between). Light curves for the two components can then be constructed from the summed light curves of the appropriate individual lines. The two light curves show uncorrelated variability, with one large flare occurring only in the hot component. We associate the hotter component with the corona, since its peak temperature is similar to 10 MK. Ne IX line ratio diagnostics for temperature and density indicate that the source of the cooler component is indeed the accretion shock, as originally reported by Kastner et al. (2002). The temperature and density of the accretion shock are in excellent agreement with models using mass accretion rates derived from the optical. We require a third component, which we call the "post-shock region," from line ratio diagnostics of O VII. The density derived from 0 VII is lower than the density derived from Ne IX, contrary to standard one-dimensional model expectations and from hydrodynamics simulations to date. The column densities derived from the two ions are also significantly different, with the column density from 0 VII lower than that from Ne IX. This post-shock region cannot be the settling flow expected from the cooling of the shock column, since its mass is 30 times the mass of material that passes through the shock. Instead this region is the splash of stellar atmosphere that has been hit by the accretion stream and heated by the accretion process (Brickhouse et al. 2010). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-776-6 J9 ASTR SOC P PY 2011 VL 448 BP 23 EP 30 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAK14 UT WOS:000304381600003 ER PT B AU Biller, B Allers, K Liu, MC Close, LM Dupuy, T AF Biller, Beth Allers, Katelyn Liu, Michael Close, Laird M. Dupuy, Trent BE JohnsKrull, CMJ Browning, MK West, AA TI Constraining the Evolution of Brown Dwarf Binarity as a Function of Age: A Keck LGS AO Search for Brown Dwarf and Planetary Mass Companions to Upper Scorpius Brown Dwarfs SO 16TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 16th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY AUG 28-SEP 03, 2010 CL Univ Washington, Seattle, WA SP Natl Sci Fdn, NASA Astrobiol Inst, European Space Agcy, Astrophys Res Consortium/Apache Point Observ, Univ Washington Coll Arts & Sci, Univ Washington Dept Astron HO Univ Washington ID OB ASSOCIATION; WIDE BINARIES; ADAPTIVE OPTICS; STAR-FORMATION; YOUNG; MULTIPLICITY; DISCOVERY; TAURUS; FRAGMENTATION; SPECTROGRAPH AB We searched for binary companions to 20 brown dwarfs in Upper Scorpius (145 pc, 5 Myr, nearest OB association) with the facility infrared camera NIRC2 and the Laser Guide Star adaptive optics system on the 10 m Keck II telescope. We discovered a close companion (0.14 '', 20.9 +/- 0.4 AU) to the very low mass object SCH J16091837-20073523. From spectral deconvolution of integrated-light near-IR spectroscopy of SCH1609 using the SpeX spectrograph (Rayner et al. 2003), we estimate primary and secondary spectral types of M6 +/- 0.5 and M7 +/- 1.0, corresponding to masses of 79 17 M-Jup and 55 +/- 25 M-Jup at an age of 5 Myr and masses of 84 +/- 15 M-Jup and 60 +/- 25 M-Jup at an age of 10 Myr. For our survey objects with spectral types later than M8, we find an upper limit on the binary fraction of <9% (1-sigma) at separations greater than 10 AU. We combine the results of our survey with previous surveys of Upper Sco and similar young regions to set the strongest constraints to date on binary fraction for young substellar objects and very low mass stars. The binary fraction for low mass (<40 M-Jup) brown dwarfs in Upper Sco is similar to that for T dwarfs in the field; for higher mass brown dwarfs and very low mass stars, there is an excess of medium-separation (10-50 AU projected separation) young binaries with respect to the field. These medium separation binaries will likely survive to late ages. C1 [Biller, Beth; Liu, Michael; Dupuy, Trent] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Allers, Katelyn] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. [Close, Laird M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Biller, Beth] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Biller, Beth; Dupuy, Trent] Hubble Fellow, Washington, DC USA. [Dupuy, Trent] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Biller, B (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. NR 37 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-776-6 J9 ASTR SOC P PY 2011 VL 448 BP 31 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAK14 UT WOS:000304381600004 ER PT B AU Stassun, KG Hebb, L Covey, K West, AA Irwin, J Jackson, R Jardine, M Morin, J Mullan, D Reid, IN AF Stassun, Keivan G. Hebb, Leslie Covey, Kevin West, Andrew A. Irwin, Jonathan Jackson, Richard Jardine, Moira Morin, Julien Mullan, Dermott Reid, I. Neill BE JohnsKrull, CMJ Browning, MK West, AA TI The M4 Transition: Toward a Comprehensive Understanding of the Transition into the Fully Convective Regime SO 16TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 16th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY AUG 28-SEP 03, 2010 CL Univ Washington, Seattle, WA SP Natl Sci Fdn, NASA Astrobiol Inst, European Space Agcy, Astrophys Res Consortium/Apache Point Observ, Univ Washington Coll Arts & Sci, Univ Washington Dept Astron HO Univ Washington ID LOW-MASS STARS; SCALE MAGNETIC TOPOLOGIES; LOWER MAIN-SEQUENCE; M-DWARFS; BROWN DWARFS; SOLAR-TYPE; EVOLUTION; GYROCHRONOLOGY; TEMPERATURES; MODELS AB The difference in stellar structure above and below spectral type similar to M4 is expected to be a very important one, connected directly or indirectly to a variety of observational phenomena in cool stars-such as rotation, activity, magnetic field generation and topology, timescales for evolution of these, and even the basic mass-radius relationship. In this Cool Stars XVI Splinter Session, we aimed to use the M4 transition as an opportunity for discussion about the interiors of low-mass stars and the mechanisms which determine their fundamental properties. By the conclusion of the session, several key points were elucidated. Although M dwarfs exhibit significant changes across the fully convective boundary, this "M4 transition" is not observationally sharp or discrete. Instead, the properties of M dwarfs (radius, effective temperature, rotation, activity lifetime, magnetic field strength and topology) show smooth changes across M3-M6 spectral types. In addition, a wide range of stellar masses share similar spectral types around the fully convective transition. There appears to be a second transition at M6-M8 spectral types, below which there exists a clear dichotomy of magnetic field topologies. Finally, we used the information and ideas presented in the session to construct a framework for how the structure of an M dwarf star, born with specific mass and chemical composition, responds to the presence of its magnetic field, itself driven by a feedback process that links the star's rotation, interior structure, and field topology. C1 [Stassun, Keivan G.; Hebb, Leslie] Vanderbilt Univ, Dept Phys & Astron, VU Stn B 1807, Nashville, TN 37235 USA. [Covey, Kevin] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [West, Andrew A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Irwin, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jackson, Richard] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Jardine, Moira] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Mullan, Dermott] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Morin, Julien] Dublin Inst Adv Studies, Dublin, Ireland. [Reid, I. Neill] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Stassun, KG (reprint author), Vanderbilt Univ, Dept Phys & Astron, VU Stn B 1807, Nashville, TN 37235 USA. RI West, Andrew/H-3717-2014; OI Morin, Julien/0000-0002-4996-6901 NR 28 TC 5 Z9 5 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-776-6 J9 ASTR SOC P PY 2011 VL 448 BP 505 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAK14 UT WOS:000304381600049 ER PT B AU Baeza, JA AF Antonio Baeza, J. BE Poore, GCB Ahyong, ST Taylor, J TI Squat lobsters as symbionts and in chemo-autotrophic environments SO BIOLOGY OF SQUAT LOBSTERS LA English DT Article; Book Chapter DE Symbiosis; chemo-autotrophic communities; soft corals; black corals ID CRAB ALLOPETROLISTHES-SPINIFRONS; DECAPODA-ANOMURA-GALATHEIDAE; COLD-SEEP COMMUNITIES; GULF-OF-MEXICO; HYDROTHERMAL VENT; MUNIDOPSIS DECAPODA; CRUSTACEA-DECAPODA; PROTANDRIC HERMAPHRODITISM; GORGONIAN CORALS; WESTERN PACIFIC AB Some squat lobsters have adopted a symbiotic lifestyle and others colonised chemo-synthetic communities in the deep sea. Prior to 2010, 42 species of squat lobsters were reported to engage in putative partnerships with a variety of macro-invertebrates but most commonly with soft and black corals. Twenty-one species of Galatheoidea and 23 of Chirostyloidea are reported to establish some form of symbiotic association with other invertebrates. Thirty-three identified species of squat lobsters, most of them members of the Galatheoidea, are reported from chemo-autotrophic communities in the deep sea. Given the depth at which most squat lobsters occur, the paucity of information on many aspects of their lifestyle, life history, behaviour and ecology is not surprising. C1 [Antonio Baeza, J.] Old Dominion Univ, Norfolk, VA 23529 USA. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Univ Catolica Norte, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. RP Baeza, JA (reprint author), Old Dominion Univ, Norfolk, VA 23529 USA. EM baezaa@si.edu NR 92 TC 3 Z9 4 U1 1 U2 6 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA BN 978-0-643-10434-1; 978-0-643-10172-2 PY 2011 BP 249 EP 270 PG 22 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA BAC59 UT WOS:000303804600010 ER PT B AU Reinfeld, EL Dussault, ME Sienkiewicz, FF Glass, M AF Reinfeld, Erika L. Dussault, Mary E. Sienkiewicz, Frank F. Glass, Margaret BE Jensen, JB Manning, JG Gibbs, MG TI Astrophotography for All: Capturing the Colorful Cosmos with Online Telescopes SO EARTH AND SPACE SCIENCE: MAKING CONNECTIONS IN EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 122nd Annual Meeting of the Astronomical Society of the Pacific (ASP) CY JUL 31-AUG 04, 2010 CL Geolog Soc Amer, Boulder, CO SP NASA Lunar Sci Inst, IPAC, NASA Herschel Sci Ctr, Spitzer Sci Ctr, WH Freeman & Co, Collaborat Astron Teach Scholars, Ctr Astron Educ, Sky Skan, NASA, NRAO, Stratopher Observ Infrared Astron, Planck, Univ Chicago Press, I Clicker, Aerospace, Capitol Coll, CAPER Team, AAS, Windows Universe, Seiler, Celestron, Explore Sci, MWT Assoc Inc, Boulder Beer HO Geolog Soc Amer AB This workshop will introduce astronomy educators to the Capture the Colorful Cosmos astrophotography project through direct engagement with robotic telescopes, astronomical image processing, and hands-on activities. Participants will learn how to use these resources to develop visitor-created exhibits for public display and educational programming. C1 [Reinfeld, Erika L.; Dussault, Mary E.; Sienkiewicz, Frank F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02131 USA. [Glass, Margaret] Assoc Sci Technol Ctr, Washington, DC 20005 USA. RP Reinfeld, EL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02131 USA. FU NASA [NCC5-706, NNX08AG36G] FX Education events resources associated with this work were suported by NASA Science Mission DIrectorate's International Year of Astronomy initiatives through awards NCC5-706 and NNX08AG36G NR 1 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-766-7 J9 ASTR SOC P PY 2011 VL 443 BP 99 EP + PG 2 WC Astronomy & Astrophysics; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BAH68 UT WOS:000304180400019 ER PT B AU Gould, RR Sunbury, S Sienkiewicz, F Deutsch, F Ibrahim, A Dussault, M Krumhansl, R AF Gould, Roy R. Sunbury, Susan Sienkiewicz, Frank Deutsch, Freeman Ibrahim, Aladdin Dussault, Mary Krumhansl, Ruth BE Jensen, JB Manning, JG Gibbs, MG TI The Other Worlds Project: Students Detect Exoplanets Using the MicroObservatory Online Telescopes SO EARTH AND SPACE SCIENCE: MAKING CONNECTIONS IN EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 122nd Annual Meeting of the Astronomical Society of the Pacific (ASP) CY JUL 31-AUG 04, 2010 CL Geolog Soc Amer, Boulder, CO SP NASA Lunar Sci Inst, IPAC, NASA Herschel Sci Ctr, Spitzer Sci Ctr, WH Freeman & Co, Collaborat Astron Teach Scholars, Ctr Astron Educ, Sky Skan, NASA, NRAO, Stratopher Observ Infrared Astron, Planck, Univ Chicago Press, I Clicker, Aerospace, Capitol Coll, CAPER Team, AAS, Windows Universe, Seiler, Celestron, Explore Sci, MWT Assoc Inc, Boulder Beer HO Geolog Soc Amer AB One of the outstanding goals of science education is to modernize the science classroom by engaging students in cutting-edge science. The availability of online telescopes, such as MicroObservatory, makes it possible for students to participate in one of the most exciting of current research frontiers: the search for extrasolar planets. Here we report the successful detection of transiting exoplanets by 862 students from middle and high schools in seven states, as part of the Other Worlds project. The project advances a number of educational goals, including improving students' science inquiry skills. C1 [Gould, Roy R.; Sunbury, Susan; Sienkiewicz, Frank; Deutsch, Freeman; Ibrahim, Aladdin; Dussault, Mary] Harvard Univ, Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Krumhansl, Ruth] Educ Dev Ctr Inc, Newton, MA 02458 USA. RP Gould, RR (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-766-7 J9 ASTR SOC P PY 2011 VL 443 BP 162 EP + PG 3 WC Astronomy & Astrophysics; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BAH68 UT WOS:000304180400030 ER PT B AU Kratter, KM AF Kratter, Kaitlin M. BE Schmidtobreick, L Schreiber, MR Tappert, C TI The Formation of Close Binaries SO EVOLUTION OF COMPACT BINARIES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on the Evolution of Compact Binary Stars CY MAY 06-11, 2011 CL Vina del Mar, CHILE ID INITIAL MASS FUNCTION; ECCENTRIC GRAVITATIONAL INSTABILITIES; ANGULAR-MOMENTUM EVOLUTION; ROTATING ISOTHERMAL CLOUDS; BROWN DWARF DESERT; SOLAR-TYPE STARS; PROTOSTELLAR DISKS; TURBULENT FRAGMENTATION; STELLAR MULTIPLICITY; CIRCUMBINARY DISKS AB Binary stars produce an array of dramatic astrophysical phenomena. They allow us to probe stellar structure, nuclear physics, and gravitational wave physics. They also produce the powerful supernovae that allow us to measure the scale of the universe. Despite their importance and ubiquity, many questions remain unanswered as to how the star formation process produces the wide array of stellar multiples that we observe. A complete model for binary formation encompasses three main components. We must know: (1) the primordial population of systems, (2) the influence of the dynamical processes that reshape this distribution as stars form and natal clusters disperse, and (3) the role of binary stellar evolution. In this article, I review the most prominent theories for binary formation: turbulent core fragmentation, disc fragmentation, and competitive accretion. I argue that turbulent core fragmentation at all masses, with disc fragmentation added in at the upper end of the mass spectrum, might explain the trend towards increasing multiplicity for higher mass stars. In addition, I provide a brief overview of the observational statistics and of some of the important processes that modify the primordial distribution of stellar orbits. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kratter, KM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 80 TC 9 Z9 9 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-774-2 J9 ASTR SOC P PY 2011 VL 447 BP 47 EP 60 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAG94 UT WOS:000304125600004 ER PT B AU Perets, HB Kratter, KM AF Perets, Hagai B. Kratter, Kaitlin M. BE Schmidtobreick, L Schreiber, MR Tappert, C TI Formation of Compact Binaries in Destabilised Evolved Triples SO EVOLUTION OF COMPACT BINARIES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on the Evolution of Compact Binary Stars CY MAY 06-11, 2011 CL Vina del Mar, CHILE ID GLOBULAR-CLUSTERS; TIDAL INTERACTIONS; BLUE STRAGGLERS; WHITE-DWARFS; BARIUM STARS; SYSTEMS; EVOLUTION; ECCENTRICITIES; MULTIPLICITY; COLLISIONS AB Although 10-15 percents of all stars reside in triple systems, the stellar evolution of such systems is not well understood. Here we explore some aspects of the coupled stellar and dynamical evolution of such systems. We find that the stellar evolution of a triple systems can lead to its dynamical destabilisation. The chaotic evolution of such a system could than result in a close tidal encounter or a stellar collision between the triple components, possibly followed by the formation of a compact binary. Triple evolution therefore provides a novel channel for collisional and tidal capture formation of compact binaries in the field, outside dense stellar clusters. C1 [Perets, Hagai B.; Kratter, Kaitlin M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02338 USA. RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02338 USA. NR 31 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-774-2 J9 ASTR SOC P PY 2011 VL 447 BP 61 EP 66 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAG94 UT WOS:000304125600005 ER PT B AU Linden, T Kalogera, V Sepinsky, J Prestwich, A Zezas, A Gallagher, J AF Linden, Tim Kalogera, Vicky Sepinsky, Jeremy Prestwich, Andrea Zezas, Andreas Gallagher, Jay BE Schmidtobreick, L Schreiber, MR Tappert, C TI The Effect of Common Envelope Evolution on the Formation of High Mass X-Ray Binaries SO EVOLUTION OF COMPACT BINARIES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on the Evolution of Compact Binary Stars CY MAY 06-11, 2011 CL Vina del Mar, CHILE ID STELLAR EVOLUTION; BLACK-HOLE; GALAXIES; METALLICITY; POPULATION; MODELS AB Common Envelope (CE) phases serve a critical role in the creation of high mass X-Ray binaries (HMXBs) as the primary force which moves initially loosely bound binary companions into tight orbits capable of supporting efficient material transport onto the compact object. We investigate the impact of CE phases on young (< 20 Myr) and bright (L-x < 1 x 10(36) erg s(-1)) X-ray binaries, finding CE evolution to produce a robust population of HMXBs with luminosities powered by Roche lobe overflow onto black hole accretors. We find that HMXBs formed through CE evolution match the observed luminosity and spatial distribution and metallicity dependence of the peculiar high luminosity extension of HMXBs known as the ultra-luminous X-ray sources (ULX). C1 [Linden, Tim] Univ Calif Santa Cruz, Dept Phys, 1156 High St, Santa Cruz, CA 95064 USA. [Linden, Tim] Fermilab Natl Accelerator Lab, Ctr Part Astrophys, Batavia, IL 60510 USA. [Kalogera, Vicky] Northwestern Univ, CIERA, Dept Phys & Astron, Evanston, IL 60208 USA. [Sepinsky, Jeremy] Univ Scranton, Dept Phys & Elect Engn, Scranton, PA 18510 USA. [Prestwich, Andrea; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gallagher, Jay] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Linden, T (reprint author), Univ Calif Santa Cruz, Dept Phys, 1156 High St, Santa Cruz, CA 95064 USA. FU NSF [AST-0449558]; NASA [GO0-11108B/NAS8-03060] FX We acknowledge suport from NSF grant AST-0449558 and NASA GO0-11108B/NAS8-03060 to VK. NR 26 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-774-2 J9 ASTR SOC P PY 2011 VL 447 BP 121 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAG94 UT WOS:000304125600015 ER PT B AU Valsecchi, F Glebbeek, E Farr, WM Fragos, T Willems, B Orosz, JA Liu, JF Kalogera, V AF Valsecchi, Francesca Glebbeek, Evert Farr, Will M. Fragos, Tassos Willems, Bart Orosz, Jerome A. Liu, Jifeng Kalogera, Vassiliki BE Schmidtobreick, L Schreiber, MR Tappert, C TI An Evolutionary Model for the Massive Black Hole X-Ray Binary M33 X-7 SO EVOLUTION OF COMPACT BINARIES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on the Evolution of Compact Binary Stars CY MAY 06-11, 2011 CL Vina del Mar, CHILE ID M-33; STARS AB Black hole (BH) X-ray binaries (XRBs) are X-ray bright binary systems comprising a BH accreting matter from a companion star. Unravelling the evolutionary history of observed XRBs can shed light on how BHs form, evolve and interact with their host environment, processes that yet lack a conclusive physical explanation. Our focus here lies on M33 X-7, which is among the heaviest BH XRBs known to date, hosting a 15.65 M-circle dot BH orbiting a 70 M-circle dot companion star in a 3.45 day orbit. The high masses of the binary components and the tight orbit present a challenge for typically invoked BH-XRBs formation channels. The picture is further complicated by the measured underluminosity of the stellar component. Here we propose the first evolutionary scenario for M33 X-7 that is consistent with the complete set of current observational constraints. According to our model, the progenitors of M33 X-7 are constrained to host primaries and secondaries between 85-99 M-circle dot and 28-32 M-circle dot, respectively, and initial orbital periods between 2.8-3.1 days. In order to form a BH of 15.65 M-circle dot, the BH progenitor transferred part of its envelope to the companion star and lost the rest in a strong stellar wind. During this dynamically stable mass transfer phase the companion accreted matter, to become the presently underluminous 70 M-circle dot star. C1 [Valsecchi, Francesca; Farr, Will M.; Fragos, Tassos; Willems, Bart; Kalogera, Vassiliki] Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA. [Glebbeek, Evert] McMaster Univ, Dept Phys & Astrophys, Hamilton, ON L8S 4MI, Canada. [Fragos, Tassos; Liu, Jifeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Liu, Jifeng] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Valsecchi, F (reprint author), Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA. FU NSF [AST-0908930, AST-0449558, PHY-0619274]; CAREER FX This work was partially supported by NSFgrants AST-0908930 and CAREER AST-0449558 to VK.TF is supported by a Northwestern University Presidential Fellowship.Simulations were performed on the computing cluster Fugu available to the Theoretical Astrophysics group at Northwestern University and partially funded by NSF grant PHY-0619274 to VK. NR 15 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-774-2 J9 ASTR SOC P PY 2011 VL 447 BP 271 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAG94 UT WOS:000304125600040 ER PT B AU Dai, Y Huang, JS Omont, A Hatziminaoglou, E Willmer, C Fazio, G Elvis, M Bergeron, J Rigopoulou, D Perez-Fournon, I AF Dai, Y. Huang, J-S. Omont, A. Hatziminaoglou, E. Willmer, C. Fazio, G. Elvis, M. Bergeron, J. Rigopoulou, D. Perez-Fournon, I. BE Wang, W Lu, JF Luo, Z Yang, ZQ Hua, H Chen, Z TI Spectral Energy Distribution of Far-infrared Bright Quasar Sample in the Lockman Hole SO GALAXY EVOLUTION: INFRARED TO MILLIMETER WAVELENGTH PERSPECTIVE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on the Galaxy Evolution: Infrared to Millimeter Wavelength Perspective CY OCT 25-29, 2010 CL Guilin, PEOPLES R CHINA SP Shanghai Normal Univ, Harvard Smithsonian Ctr Astrophys, Natl Nature Sci Fdn China, Purple Mt Observ, Shanghai Astronom Observ, Chinese Natl Key Project 973, Sci & Technol Commiss Shanghai Municipal, Chinese Astronom Soc ID PALOMAR-GREEN QUASARS; STAR-FORMATION; ULIRG EVOLUTION; SPITZER QUASAR; EXTRAGALACTIC SURVEY; GALAXIES; CONTINUUM; HECTOSPEC; HISTORY; QUEST AB The far-infrared (FIR) properties of Quasi-Stellar Objects (QSOs) is important in connecting the Starburst (SB) and Active Galactic Nucleus (AGN) activities. Therefore, we constructed a 24 mu m selected QSO sample to study their FIR behavior. All sources were spectroscopically identified from MMT or the Sloan Digital Sky Survey (SDSS) as broadline quasars. Of the total similar to 330 sources, 37 have secure FIR detections in the Herschel-HERMES field. We compared their SEDs to previous QS templates, and found that those FIR bright quasars differ from existing AGNs only by an additional dust component(s). Further studies on the origin for the FIR emission reveals the relative roles starburst and AGN play in powering the dust emission, based on the dust temperature, FIR luminosity, and the shapes of individual SEDs. The dust temperatures have a wide range from 20K to 80K with a median of similar to 30K, indicating homogeneous heating mechanisms that could later be related to the origin of these cold dust emissions. C1 [Dai, Y.; Huang, J-S.; Fazio, G.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dai, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jhuang@cfa.harvard.edu; gfazio@cfa.harvard.edu NR 29 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-772-8 J9 ASTR SOC P PY 2011 VL 446 BP 241 EP 248 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAF56 UT WOS:000304023000033 ER PT B AU Fazio, GG AF Fazio, G. G. CA SEDS Team BE Wang, W Lu, JF Luo, Z Yang, ZQ Hua, H Chen, Z TI SEDS: Spitzer Extended Deep Survey SO GALAXY EVOLUTION: INFRARED TO MILLIMETER WAVELENGTH PERSPECTIVE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on the Galaxy Evolution: Infrared to Millimeter Wavelength Perspective CY OCT 25-29, 2010 CL Guilin, PEOPLES R CHINA SP Shanghai Normal Univ, Harvard Smithsonian Ctr Astrophys, Natl Nature Sci Fdn China, Purple Mt Observ, Shanghai Astronom Observ, Chinese Natl Key Project 973, Sci & Technol Commiss Shanghai Municipal, Chinese Astronom Soc ID ALPHA-EMITTING GALAXIES; HALO OCCUPATION DISTRIBUTION; QUASAR LUMINOSITY FUNCTION; STAR-FORMATION RATES; DIGITAL SKY SURVEY; STELLAR MASSES; FAINT-END; PHYSICAL-PROPERTIES; SPACE-TELESCOPE; EVOLUTION AB The Spitzer Extended Deep Survey (SEDS) will provide a unique opportunity to obtain the first complete census of the assembly of stellar mass and black holes as a function of cosmic time back to the era of reionization, yielding unique information on galaxy formation in the early Universe. The survey will also measure galaxy clustering over a wide redshift range, which will provide the critical link between galaxies and their dark matter halos and critical tests of models of early star formation. SEDS will achieve these goals by tracing the stellar mass growth in mass-selected samples of galaxies via their broadband spectral energy distributions. SEDS is an unbiased survey using the Spitzer Space Telescope Infrared Array Camera (IRAC) at 3.6 and 4.5 microns, with 12 hours/pointing, over five well-studied fields of 0.90 square degree total, requiring 2108 hours of observation. It is a unique program that will leave an important legacy for years to come. C1 [Fazio, G. G.; SEDS Team] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fazio, GG (reprint author), Harvard Smithsonian Ctr Astrophys, MS 65,60 Garden St, Cambridge, MA 02138 USA. EM gfazio@cfa.harvard.edu NR 40 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-772-8 J9 ASTR SOC P PY 2011 VL 446 BP 347 EP 354 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAF56 UT WOS:000304023000047 ER PT J AU Buffington, ML Sandler, RJ AF Buffington, Matthew L. Sandler, Robert J. TI The occurrence and phylogenetic implications of wing interference patterns in Cynipoidea (Insecta : Hymenoptera) SO INVERTEBRATE SYSTEMATICS LA English DT Article ID FIGITIDAE EUCOILINAE; CIRCUMSCRIPTION; EVOLUTION; GENUS AB Wing interference patterns (WIPs) are a potentially rich source of taxonomic data. We surveyed a broad range of Cynipoidea (Hymenoptera) for the presence of these patterns. Further, we used phylogeny to investigate the evolutionary patterns of WIPs throughout the superfamily. We also documented that WIPs occur across nearly all species sampled, in both the hindwing and forewing; in many instances, the forewing WIP is carried over to the hindwing. Only Austrocynips mirabilis Riek lacked WIPs. Among species that possess WIPs, we were able to recognise four distinct categories: radiform (radiating), striatiform (longitudinally striate), campiform (continuous field) and galactiform (amorphous mixture of colours). Wing interference patterns are not found in infuscate wings or areas of infuscation on otherwise hyaline wings, and are reduced on large wings. Within Figitidae, WIPs are more phylogenetically conservative, especially at the tribal level: within Cynipidae the phylogenetic conservatism of WIPs is somewhat less clear, though all Synergini sampled had a very consistent WIPs. For certain genera, such as Ganaspidium and Andricus, WIPs may prove useful for species-level discrimination. C1 [Buffington, Matthew L.] USNM, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Sandler, Robert J.] Brown Univ, Dept Sci & Soc, Providence, RI 02912 USA. RP Buffington, ML (reprint author), USNM, Systemat Entomol Lab, USDA, Smithsonian Inst, 10th & Constitut Ave NW,POB 37012,MRC 168, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov NR 21 TC 4 Z9 5 U1 1 U2 7 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1445-5226 EI 1447-2600 J9 INVERTEBR SYST JI Invertebr. Syst. PY 2011 VL 25 IS 6 BP 586 EP 597 DI 10.1071/IS11038 PG 12 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 937JQ UT WOS:000303655200003 ER PT J AU Adey, WH Hayek, LAC AF Adey, Walter H. Hayek, Lee-Ann C. TI Elucidating Marine Biogeography with Macrophytes: Quantitative Analysis of the North Atlantic Supports the Thermogeographic Model and Demonstrates a Distinct Subarctic Region in the Northwestern Atlantic SO NORTHEASTERN NATURALIST LA English DT Article ID URCHINS STRONGYLOCENTROTUS-DROEBACHIENSIS; GREEN SEA-URCHINS; NOVA-SCOTIA; REPRODUCTIVE ECOLOGY; EASTERN NEWFOUNDLAND; CRUSTOSE CORALLINES; CHONDRUS-CRISPUS; AGARUM-CRIBROSUM; INTERTIDAL ZONE; KELP COMMUNITY AB Quantitative analysis of North Atlantic macrophyte (seaweed) abundance was used to test the thermogeographic model (TM) of marine biogeography. The TM uses coastal area and seawater temperature over Pleistocene time to reveal long-term climate/area clusters that predict biogeographic regions. An earlier study with the TM predicted 20 of 24 classical biogeographic regions; the 4 omitted regions were either weak, disputed, or structurally (sandy/silty regions) inapplicable to the TM. The TM predicted a new western North Atlantic Subarctic Region, centered on the Strait of Belle Isle and lying between Newfoundland and Labrador. In contrast, Nova Scotia and the Gulf of Maine were found to be a Boreal/Subarctic transition zone. The predictions of the TM were earlier supported with coralline algal abundances, and here are supported by a test with macrophyte assemblages. Seaweed assemblages were studied at 51 primary SCUBA stations with 4-7 standard depth zones at each station from southern Labrador to Cape Elizabeth, ME. Meter-square quadrats were taken at each station, followed by at-sea sorting, identification, and weighing of biomass by species. A permanent record of these studies is provided by archived underwater photography and voucher herbarium samples, including tissue in silica gel to support future DNA analyses. Comparisons of European seaweed assemblages were accomplished by re-analyzing semi-quantitative data available in the literature. We demonstrate with the biomass data that a 3000-km stretch of coast (i.e., northern Gulf of St. Lawrence, northeastern Newfoundland, and southern Labrador) that is centered on the Strait of Belle Isle has a unique assemblage of seaweeds. In its location and marine climate, this coast closely matches the Subarctic Region predicted by the TM. Based on graphic demonstration, this Subarctic Region is radically different from that of Nova Scotia and the Gulf of Maine, and its dominant species derive from the North Pacific Ocean. Several different statistical approaches applied to the macrophyte data demonstrate the strength of these findings, while also finding that a subset of Subarctic species persists in deeper water to the south in the transition zone (i.e., southwestern Nova Scotia, Gulf of Maine). Only a very small proportion of the seaweed flora of the Subarctic Region is Arctic in origin (<4%). Earlier geographic analyses of biodiversity did not discover the Subarctic Region because rare species hide the strength of assemblages based on abundance. Many of the dominant seaweeds in the transitional region of the Gulf of Maine and Nova Scotia occur widely in Europe, and are Boreal in origin. Such Boreal species form 47-80% of the macrophyte biomass at depths shallower than 5 m in the northwestern Atlantic transition zone southwest of the Subarctic Region. In deeper water (>5 m), however, European Boreal species are only 22-25% of the macrophyte biomass. Although many of the dominant, shallow sublittoral species of the European Boreal flora have made the North Atlantic passage, only about 10% (by biomass) of mid-depth species (2.5-5 m) have crossed and even fewer of the deeper European species are found in the northwestern Atlantic. A few European "Boreal" seaweeds reach further north into the Subarctic Region, but only at low levels of biomass and primarily at mid-depths (2.5-5 m). The Subarctic is inhospitable for establishment of such species in shallow water because of low winter temperatures and sea ice, and in deeper water by low summer temperatures (<5 degrees C). Few ecologists have had the opportunity to work in the Subarctic Region; instead, most of the recent descriptive and experimental studies of northwestern Atlantic ecosystems are based on studies in the smaller transition zone in the Gulf of Maine and southwestern Nova Scotia. Consequently, we provide detailed photographic, tabular, and graphic descriptions of the seaweed assemblages within the Subarctic and their interactions with the major grazer, the sea urchin Strongylocentrotus droebachiensis. Three of the four most abundant seaweeds in the North Atlantic Subarctic Region (Agarum clathratum, Desmarestia viridis, and Ptilota serrata) occur in mid-deep water and are protected from grazing by secondary chemicals. The kelp Alaria esculenta often forms a monocultural canopy in the shallow subtidal zone, and it is the second-most abundant seaweed in the Subarctic. Sea urchins form "fronts" that graze back the Alaria in spring and summer when wave action is moderate, but the wide Alaria zone is persistent on more exposed shores. Agarum clathratum, D. viridis, and P serrata) in deeper water tend to form a savanna: dense patches of fleshy seaweeds separated by areas of coralline/urchin "barrens". Unlike Arctic or estuarine barren zones, the coralline "barrens" of Subarctic rocky shores are calcitic, biostromal structures with a rich invertebrate infauna. These formations demonstrate great temporal stability, with longevities of decades to centuries, as shown through laser/ablation mass spectrograph analysis of Mg2+ content in the coralline Clathromorphum compactum. This research examines the relationship of the Subarctic to the eastern Atlantic Boreal and to the largely Boreal-dominated transition zone in the Gulf of Maine and Nova Scotia. By analyzing the TM and its relationship to the history of deglaciation after the Last Glacial Maximum (LGM), we hypothesize the western Atlantic rocky shore was occupied primarily by Subarctic glacial relict seaweeds in the early Holocene. During the mid-Holocene's pre-rebound hypsithermal, due to a warmer and more open Canadian Northwest Passage, these species were likely supplemented by an injection of North Pacific Subarctic seaweeds. In the latest Holocene, and perhaps only in historical times, a surge of eastern North Atlantic Boreal seaweeds entered and came to dominate the southern, climatically transitional half of this coast; invasion and change continue today, and likely represent a major anthropogenic bridging of an oceanographic barrier. C1 [Adey, Walter H.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hayek, Lee-Ann C.] Smithsonian Inst, Natl Museum Nat Hist Stat & Math, Washington, DC 20013 USA. RP Adey, WH (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, NHB 166,POB 37012, Washington, DC 20013 USA. EM adeyw@si.edu FU Ecological Systems Technology, Inc.; Botany Department of the National Museum of Natural History FX Funding for this project was provided by Ecological Systems Technology, Inc. and the Botany Department of the National Museum of Natural History. NR 118 TC 17 Z9 17 U1 5 U2 34 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 J9 NORTHEAST NAT JI Northeast. Nat PY 2011 VL 18 BP 1 EP 128 PG 128 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 929US UT WOS:000303091800001 ER PT S AU Laskar, T Berger, E Chary, RR AF Laskar, Tanmoy Berger, Edo Chary, Ranga-Ram BE McEnery, JE Racusin, JL Gehrels, N TI Exploring the Galaxy Mass-Metallicity Relation at z 3-5 SO GAMMA RAY BURSTS 2010 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference of the Gamma Ray Bursts CY NOV 01-04, 2010 CL Annapolis, MD DE gamma-ray sources (astronomical); high-redshift galaxies; cosmology ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; BURST HOST GALAXIES; STELLAR POPULATIONS; EVOLUTION; SPECTROSCOPY; PROGENITOR; FIELD; IRAC; GAS AB Long-duration gamma-ray bursts (GRBs) provide a premier tool for studying high-redshift star-forming galaxies thanks to their extreme brightness and association with massive stars. Here we use GRBs to study the galaxy mass-metallicity (M-*-Z) relation at z similar to 3-5, where conventional direct metallicity measurements are extremely challenging. We use the interstellar medium metallicities of long-duration GRB hosts derived from afterglow absorption spectroscopy (Z approximate to 0.01 - 1 Z(circle dot)), in conjunction with host galaxy stellar masses determined from deep Spitzer 3.6 mu m observations of 20 GRB hosts. We detect about 1/4 of the hosts with M-AB(I) approximate to -21.5 to -22.5 mag, and place a limit of M-AB(I) greater than or similar to -19 mag on the remaining hosts from a stacking analysis. Using a conservative range of mass-to-light ratios for simple stellar populations (with ages of 70 Myr to similar to 2 Gyr), we infer the host stellar masses and present the galaxy mass-metallicity measurements at z similar to 3 - 5 (< z > approximate to 3.5). We find that the detected GRB hosts, with M-* approximate to 2 x 10(10) M-circle dot, display a wide range of metallicities, but that the mean metallicity at this mass scale, Z approximate to 0.1 Z(circle dot), is lower than measurements at z less than or similar to 3. Combined with stacking of the non-detected hosts (with M-* less than or similar to 4 x 10(9) M-circle dot and Z less than or similar to 0.03 Z(circle dot)), we find evidence for the existence of an M-*-Z relation at z similar to 3.5 and continued evolution of this relation to systematically lower metallicities from z similar to 2. C1 [Laskar, Tanmoy; Berger, Edo; Chary, Ranga-Ram] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Laskar, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0916-3 J9 AIP CONF PROC PY 2011 VL 1358 DI 10.1063/1.3621801 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BZU09 UT WOS:000302963100076 ER PT S AU Pe'er, A Zhang, BB Ryde, F McGlynn, S Zhang, B Preece, RD Kouveliotou, C AF Pe'er, Asaf Zhang, Bin-Bin Ryde, Felix McGlynn, Sinead Zhang, Bing Preece, Robert D. Kouveliotou, Chryssa BE McEnery, JE Racusin, JL Gehrels, N TI The Connection Between Thermal and Non-Thermal Emission in Gamma-ray Bursts: General considerations and GRB090902B as a Case Study SO GAMMA RAY BURSTS 2010 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference of the Gamma Ray Bursts CY NOV 01-04, 2010 CL Annapolis, MD DE gamma rays:bursts; gamma rays:theory; plasmas; radiation mechanisms:thermal; radiative transfer; scattering ID SYNCHROTRON SHOCK MODEL; PAIR PRODUCTION; SPECTRA; BATSE; COMPONENT; PROMPT; GRB; EVOLUTION; OUTFLOW AB Photospheric (thermal) emission is inherent to the gamma-ray burst (GRB) "fireball" model. We show that inclusion of this component in the analysis of the GRB prompt emission phase naturally explains some of the prompt GRB spectra seen by the Fermi satellite over its entire energy band. The sub-MeV peak is explained as multi-color black body emission, and the high energy tail, extending up to the GeV band, results from roughly similar contributions of synchrotron emission, synchrotron self Compton (SSC) and Comptonization of the thermal photons by energetic electrons originating after dissipation of the kinetic energy above the photosphere. We briefly discuss the theory of multicolor black body emission from relativistically expanding plasma, before showing how the analysis method proposed results in a complete, self consistent picture of the physical conditions at both emission sites of the thermal and non-thermal radiation. Furthermore, it enables to extract the values of the free model parameters. We demonstrate the analysis method on GRB090902B, and present the values of the physical parameters deduced. We briefly discuss the uniqueness of GRB090902B-type spectra. C1 [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Pe'er, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apeer@cfa.harvard.edu OI Preece, Robert/0000-0003-1626-7335 FU Riccardo Giacconi Fellowship award of the Space Telescope Science Institute; Swedish National Space Board.; [31014] FX This research was supported by the Riccardo Giacconi Fellowship award of the Space Telescope Science Institute, and Fermi grant award #31014. FR acknowledges financial support by the Swedish National Space Board. AP wishes to thank Dale Frail, Jeremy Schnittman, Andy Fruchter, Kuntal Misra, Zeljka Bosnjak, Mario Livio and Kailash Sahu for useful discussions. NR 26 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0916-3 J9 AIP CONF PROC PY 2011 VL 1358 DI 10.1063/1.3621745 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BZU09 UT WOS:000302963100021 ER PT S AU Silver, E Gillaspy, JD Gokhale, P Kanter, EP Brickhouse, NS Dunford, RW Kirby, K Lin, T McDonald, J Schneider, D Seifert, S Young, L AF Silver, E. Gillaspy, J. D. Gokhale, P. Kanter, E. P. Brickhouse, N. S. Dunford, R. W. Kirby, K. Lin, T. McDonald, J. Schneider, D. Seifert, S. Young, L. BE McDaniel, FD Doyle, BL TI Work Towards Experimental Evidence Of Hard X-Ray Photoionization In Highly Charged Krypton SO APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY: TWENTY-FIRST INTERNATIONAL CONFERENCE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 21st International Conference on Application of Accelerators in Research and Industry (CAARI) CY AUG 08-13, 2010 CL Ft Worth, TX SP Univ N Texas, Sandia Natl Labs, Los Alamos Natl Lab, AccSys Technol Inc, High Voltage Engn Europa BV, Natl Electrostat Corp, TDK-Lambda Amer DE x-rays; photoionization; spectroscopy; EBIT; synchrotron AB Ions of almost any charge state can be produced through electron-impact ionization. Here we describe our first experiments designed to photoionize these highly charged ions with hard x-rays by pairing an electron and photon beam. A spectral line at 12.7(1) keV with an intensity corroborated by theory may be the first evidence of hard x-ray photoionization of a highly charged ion. C1 [Silver, E.; Brickhouse, N. S.; Kirby, K.; Lin, T.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gillaspy, J. D.; Gokhale, P.] NIST, Gaithersburg, MD 20899 USA. [Kanter, E. P.; Dunford, R. W.; Seifert, S.; Young, L.] Argonne Natl Lab, Argonne, IL 60439 USA. [McDonald, J.] George E Wahle, Dept Veterans Affairs Med Ctr, Salt Lake City, UT 84148 USA. [Schneider, D.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Silver, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA [NNX08AK33G]; Argonne National Laboratory LDRD FX This work was supported by NASA Grant NNX08AK33G and an Argonne National Laboratory LDRD grant. NR 9 TC 3 Z9 3 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0891-3 J9 AIP CONF PROC PY 2011 VL 1336 BP 146 EP 149 DI 10.1063/1.3586076 PG 4 WC Physics, Applied SC Physics GA BZT55 UT WOS:000302912900030 ER PT S AU Kiziltan, B AF Kiziltan, Buelent BE Gogus, E Belloni, T Ertan, U TI REASSESSING THE FUNDAMENTALS NEW CONSTRAINTS ON THE EVOLUTION, AGES AND MASSES OF NEUTRON STARS SO ASTROPHYSICS OF NEUTRON STARS 2010: A CONFERENCE IN HONOR OF M. ALI ALPAR SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Astrophysics of Neutron Stars in Honor of M Ali Alpar (ASTRONS) CY AUG 02-06, 2010 CL Cesme, TURKEY SP Sabanci Univ, European Commiss FP6 Marie Curie Act DE Stars: neutron; pulsars: general; X-rays: binaries; stars: statistics ID MILLISECOND PULSARS; BINARY EVOLUTION AB The ages and masses of neutron stars (NSs) are two fundamental threads that make pulsars accessible to other sub-disciplines of astronomy and physics. A realistic and accurate determination of these two derived parameters play an important role in understanding of advanced stages of stellar evolution and the physics that govern relevant processes. Here I summarize new constraints on the ages and masses of NSs with an evolutionary perspective. I show that the observed P-(P) over dot demographics is more diverse than what is theoretically predicted for the standard evolutionary channel. In particular, standard recycling followed by dipole spin-down fails to reproduce the population of millisecond pulsars with higher magnetic fields (B>4x10(8)G) at rates deduced from observations. A proper inclusion of constraints arising from binary evolution and mass accretion offers a more realistic insight into the age distribution. By analytically implementing these constraints, I propose a "modified" spin-down age ((tau) over tilde) for millisecond pulsars that gives estimates closer to the true age. Finally, I independently analyze the peak, skewness and cutoff values of the underlying mass distribution froma comprehensive list of radio pulsars for which secure mass measurements are available. The inferred mass distribution shows clear peaks at 1.35M(circle dot) and 1.50M(circle dot) for NSs in double neutron star (DNS) and neutron star-white dwarf (NS-WD) systems respectively. I find a mass cutoff at 2 M-circle dot for NSs with WD companions, which establishes a firm lower bound for the maximum mass of NSs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kiziltan, B (reprint author), Harvard Smithsonian Ctr Astrophys, MS-51, Cambridge, MA 02138 USA. EM bkiziltan@cfa.harvard.edu NR 10 TC 1 Z9 1 U1 1 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0939-2 J9 AIP CONF PROC PY 2011 VL 1379 DI 10.1063/1.3629483 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BZT86 UT WOS:000302936600008 ER PT J AU Braje, TJ Rick, TC Willis, LM Erlandson, JM AF Braje, Todd J. Rick, Torben C. Willis, Lauren M. Erlandson, Jon M. TI SHELLFISH AND THE CHUMASH: MARINE INVERTEBRATES AND COMPLEX HUNTER-GATHERERS ON LATE HOLOCENE SAN MIGUEL ISLAND, CALIFORNIA SO NORTH AMERICAN ARCHAEOLOGIST LA English DT Article ID MIDDLE STONE-AGE; COASTAL SOUTHERN CALIFORNIA; CHANNEL-ISLANDS; NORTH-AMERICA; HUMAN IMPACTS; ROSA ISLAND; EVOLUTION; AFRICA; PERSPECTIVE; ADAPTATIONS AB Marine resources played an important role in fostering high population densities and cultural complexity among North American hunter-gatherers. In California, several researchers have emphasized the relationship among increases in fishing, marine mammal hunting, the development of more efficient watercraft, and increased sociopolitical complexity. Largely absent from discussions of emergent complexity is the changing role of shellfish in human subsistence economies. Analyzing marine shell from 12 Late Holocene sites on San Miguel Island, we illustrate the importance of shellfish in island subsistence economies and the evolution of Chumash complexity. The dietary importance of shellfish protein declined through time, but the density of shellfish remains increased dramatically in Late Holocene archaeological sites, suggesting that shellfish provided an important supplement to the higher yields of finfish and helped fuel growing human populations and sociopolitical complexity. C1 [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. [Rick, Torben C.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. [Willis, Lauren M.; Erlandson, Jon M.] Univ Oregon, Eugene, OR 97403 USA. RP Braje, TJ (reprint author), San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. EM Todd.Braje@humboldt.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 86 TC 3 Z9 3 U1 0 U2 18 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0197-6931 EI 1541-3543 J9 N AM ARCHAEOL JI N. Am. Archaeol. PY 2011 VL 32 IS 3 BP 267 EP 290 DI 10.2190/NA.32.3.c PG 24 WC Archaeology SC Archaeology GA 921XS UT WOS:000302512000003 ER PT S AU Slavin, JD AF Slavin, Jonathan D. BE Florinski, V Heerikhuisen, J Zank, GP Gallagher, DL TI Partially Ionized Gas in the Local Interstellar Medium and Its Galactic Context SO PARTIALLY IONIZED PLASMAS THROUGHOUT THE COSMOS - PROCEEDINGS OF THE 2010 HUNTSVILLE WORKSHOP SE AIP Conference Proceedings LA English DT Proceedings Paper CT Huntsville Workshop on Partially Ionized Plasmas Throughout the Cosmos CY OCT 03-08, 2010 CL Nashville, TN SP Univ Alabama, Huntsvilles Ctr Space Plasma & Aeronom Res (CSPAR), NASAs Marshall Space Flight Ctr (MSFC) DE ISM:clouds; ISM:abundances; ultraviolet:ISM; X-rays:diffuse background; solar system:general ID TURBULENCE; DISSIPATION AB The most thoroughly observed region of the interstellar medium (ISM) is that which immediately surrounds the heliosphere. Evidence that this gas is partially ionized (about 20% for H, 40% for He) comes from a variety of sources including absorption lines toward nearby stars, and in situ detection of interstellar neutral atoms and pickup ions in the solar system. The ionization in the Local Interstellar Cloud (LIC) is dominated by photoionization and requires more ionizing flux than is available stellar sources. Diffuse radiation from nearby hot gas can provide the necessary hard yet low intensity interstellar radiation field. To put the local ISM in a Galactic context, one can compare it to the warm ionized medium (WIM), but the H ionization level of the LIC is apparently substantially lower than that in the WIM. We discuss the nature and source of ionization of the LIC and compare it with evidence on more distant regions of the warm, diffuse ISM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Slavin, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 83, Cambridge, MA 02138 USA. OI Slavin, Jonathan/0000-0002-7597-6935 NR 15 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0926-2 J9 AIP CONF PROC PY 2011 VL 1366 DI 10.1063/1.3625593 PG 8 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BZT56 UT WOS:000302913100011 ER PT J AU Smith, DR Shinohara, A AF Smith, David R. Shinohara, Akihiko TI Review of the Asian wood-boring genus Euxiphydria (Hymenoptera, Symphyta, Xiphydriidae) SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Woodborers; Palearctic; Oriental; Hyperxiphia AB Five species of Euxiphydria are recognized, E. leucopoda Takeuchi, 1938, from Japan, E. potanini (Jakovlev, 1891) from Japan, Russia, Korea, and China, E. pseudoruficeps Okutani, 1966, from Taiwan, E. vietna-mensis, Sp. n. from Vietnam, and E. shaanxiana, sp. n., from China. Euxiphydria subtrifida Maa, 1944, is considered a new synonym of E. potanini. A key and illustrations are given to distinguish the species. C1 [Smith, David R.] Agr Res Serv, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Shinohara, Akihiko] Natl Museum Nat & Sci, Dept Zool, Tsukuba, Ibaraki 3050005, Japan. RP Smith, DR (reprint author), Agr Res Serv, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov NR 33 TC 1 Z9 1 U1 0 U2 0 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1070-9428 EI 1314-2607 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2011 VL 23 BP 1 EP 22 DI 10.3897/JHR.23.1548 PG 22 WC Entomology SC Entomology GA 920FN UT WOS:000302388500001 ER PT J AU Smith, DR AF Smith, David R. TI Nematinae (Hymenoptera,Tenthredinidae) of Thailand, with notes on some other southeastern Asian nematines SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE sawflies; Symphyta; southeastern Asia ID HYMENOPTERA-TENTHREDINIDAE; SYMPHYTA HYMENOPTERA; WORLD CATALOG; PRISTIPHORA AB Nine species in five genera of Nematinae are recorded for the first time from Thailand: Trichiocampus pruni Takeuchi, Dineura sharkeyi, sp. n., Moricella rueaensis, sp. n., Nematus soidaoi, sp. n., Pristiphora chalybeata Benson, Pristiphora ettera, sp. n., Pristiphora inthanoni, sp. n., Pristiphora annetna, sp. n., and Pristiphora phahompoki, sp. n. A key is given for the genera and species of Thailand. New records and description of the male are given for Pristiphora borneensis Forsius from Sabah, Malaysia, and a new record is given for Pristiphora sinensis Wong from China. C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov FU National Science Foundation [DEB-0542864] FX The National Science Foundation Grant # DEB-0542864, Thailand Biodiversity Inventory (also known as TIGER, Thailand Inventory Group for Entomological Research) to M. J. Sharkey, University of Kentucky, Lexington, is acknowledged. I thank M. J. Sharkey and S. Clutts, University of Kentucky, for sorting and sending specimens. I thank the curator at the B.P. Bishop Museum, Honolulu, HI, for the loan of specimens. Michele Touchet, Systematic Entomology Laboratory, USDA, Washington, DC, assisted with the images. Reviews by the following are appreciated: N. M. Schiff, U. S. Forest Service, Stoneville, MS; D. A. Nickle and T. J. Henry, Systematic Entomology Laboratory, USDA, Beltsville, MD, and Washington, DC, respectively; M. Wei, Central South University of Forestry and Technology, Changsha, China; and an anonymous reviewer. USDA is an equal opportunity provider and employer. NR 38 TC 0 Z9 0 U1 0 U2 2 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1070-9428 EI 1314-2607 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2011 VL 22 BP 1 EP 27 DI 10.3897/JHR.22.1617 PG 27 WC Entomology SC Entomology GA 920FM UT WOS:000302388400001 ER PT J AU Gates, MW Buffington, ML AF Gates, Michael W. Buffington, Matthew. L. TI Description of two techniques to increase efficiency in processing and curating minute arthropods, with special reference to parasitic Hymenoptera SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Chalcidoidea; Cynipoidea; crystal polystyrene; vacuum pump; curation; dehydration ID MALAISE TRAPS; PRESERVATION; DNA; EXTRACTION; SPECIMENS; DIVERSITY; INSECTS; WASPS AB We describe and illustrate two techniques for enhancing curatorial and processing efficiency as it pertains to parasitic Hymenoptera (Chalcidoidea, Cynipoidea). These techniques were developed in response not only to the massive number of parasitoids that have been acquired through various biodiversity studies, but also the difficulty in mobilizing the human resources to curate this material. The first technique uses small, crystal polystyrene boxes with tight-fitting lids to store dehydrated specimens prior to mounting. Locality information is affixed to the box and specimens are spread in a layer for ease of examination by researchers. Solutions for managing static electricity within the specimen boxes are discussed. The second involves a vacuum pump connected to a funnel with a filtration membrane and flask apparatus to rapidly dehydrate hard-bodied parasitoids (Figitidae) that are not subject to collapse during air-drying. C1 [Gates, Michael W.; Buffington, Matthew. L.] ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, Washington, DC 20013 USA. RP Buffington, ML (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, MRC 168,POB 37012, Washington, DC 20013 USA. EM michael.gares@ars.usda.gov NR 18 TC 1 Z9 1 U1 2 U2 6 PU PENSOFT PUBLISHERS PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1070-9428 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2011 VL 22 BP 133 EP 140 DI 10.3897/JHR.22.2099 PG 8 WC Entomology SC Entomology GA 920FM UT WOS:000302388400005 ER PT J AU Wilson, S Collister, DM Wilson, AG AF Wilson, Scott Collister, Douglas M. Wilson, Amy G. TI COMMUNITY COMPOSITION AND ANNUAL SURVIVAL OF LOWLAND TROPICAL FOREST BIRDS ON THE OSA PENINSULA, COSTA RICA SO ORNITOLOGIA NEOTROPICAL LA English DT Article DE Annual survival; avian community composition; fragmentation; mark-recapture; Osa Peninsula; species richness ID OLD-GROWTH FORESTS; INSECTIVOROUS BIRDS; SWAINSONS THRUSH; HABITAT; DEFORESTATION; DYNAMICS; RATES; CONSERVATION; COUNTRYSIDE; 2ND-GROWTH AB Tropical deforestation has resulted in many landscapes where forests exist as patches of varying size and connectivity within a human-dominated landscape. Understanding the implications of these landscapes for biodiversity and population dynamics is now a major challenge for tropical conservation biology. We examined community composition and annual survival of birds in a partially deforested landscape on the Osa Peninsula of Costa Rica, which is a region of high biodiversity and increasing conservation concern. Our study was based on seven years of mist-netting surveys on a 3 ha plot and a single year of point counts. These counts were conducted in two habitat types: a fragmented landscape with a mix of forest patches and open agricultural areas, and an approximately 100 ha patch of mature forest. Estimated species richness tended to be higher in the fragmented landscape (116 vs 89), likely because this landscape still contains moderate forest cover thus supporting species that tolerate some deforestation as well as species that prefer more open habitats. Accordingly, 43 species were only detected in the fragmented habitats while 22 were only detected in forest. The latter result suggests that some forest specialists have been able to persist in this partially deforested region, likely because of the presence of larger forest patches and connectivity between them. Our surveys also included moderate numbers of the endangered Black-cheeked Ant-Tanager (Habia atrimaxillaris), which was primarily detected in areas of greater forest cover. For eight common passerines, apparent annual survival of adults ranged from a low of 0.35 +/- 0.07 (SD) for Ochre-bellied Flycatchers (Mionectes oleagineus) to a high of 0.81 +/- 0.11 for Black-hooded Antshrikes (Thamnophilus bridges,) with an average of 0.63 +/- 0.05 across all species. This average rate is similar to other studies that have estimated survival with mist-net mark-recapture techniques elsewhere in the tropics. Our study provides one of the first assessments of avian community composition and survival in countryside landscapes on the Osa Peninsula. Conservation goals will increasingly need to consider such landscapes and we discuss additional studies that could further our knowledge in the region. Accepted 4 August 2011. C1 [Wilson, Scott; Wilson, Amy G.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Wilson, Scott; Collister, Douglas M.; Wilson, Amy G.] Calgary Bird Banding Soc, Calgary, AB T3E 5X2, Canada. RP Wilson, S (reprint author), Environm Canada, Canadian Wildlife Serv, 115 Perimeter Rd, Saskatoon, SK S7N 0X4, Canada. EM scottd.wilson@ec.gc.ca FU Calgary Bird Banding Society; Alberta Gaming and Liquor Commission; Canadian Wildlife Service; Natural Sciences and Engineering Research Council; Killam doctoral award FX We thank Jolanda Hess, David Argello, and Jay Tress for allowing access to their property and the Costa Rican government (MINAE) for granting us permission to conduct this project. We also thank members of the Calgary Bird Banding Society (P. Achuff, C. Bennett, J. Cartwright, A. Cole, R. Ebel, M. Gahbauer, J. Lane, S. Lane, P. Mitchell, M. Mulligan, A. Nava Donatti, E. Peterson, C. Savignac, G. Smiley, C. Smith, B. Taylor, G. Tietz, B. Trakalo, C. Watson, and A. Weerstra) as well as A. and E. Quesada-Calvo for assistance in the field. Funding for this project was provided by members of the Calgary Bird Banding Society, Alberta Gaming and Liquor Commission, Canadian Wildlife Service, Natural Sciences and Engineering Research Council (doctoral fellowships to SW and AGW) and a Killam doctoral award to SW. NR 50 TC 2 Z9 2 U1 5 U2 27 PU NEOTROPICAL ORNITHOLOGICAL SOC, USGS PATUXENT WILDLIFE RESEARCH CTR PI ATHENS PA UNIV GEORGIA, WARNELL SCH FOREST RESOURCES, ATHENS, GA 30602-2152 USA SN 1075-4377 J9 ORNITOL NEOTROP JI ORNITOL. NEOTROP. PY 2011 VL 22 IS 3 BP 421 EP 436 PG 16 WC Ornithology SC Zoology GA 918UC UT WOS:000302275600010 ER PT J AU Duraes, R Blake, JG Loiselle, BA Ryder, TB Tori, WP Hidalgo, JR AF Duraes, Renata Blake, John G. Loiselle, Bette A. Ryder, Thomas B. Tori, Wendy P. Hidalgo, Jose R. TI VOCALIZATION ACTIVITY AT LEKS OF SIX MANAKIN (PIPRIDAE) SPECIES IN EASTERN ECUADOR SO ORNITOLOGIA NEOTROPICAL LA English DT Article DE Ecuador; lek; manakin; Pipridae; vocalization; vocalization rate ID BLUE-CROWNED MANAKINS; WIRE-TAILED MANAKIN; MALE MATING SUCCESS; LEKKING BIRD; PHYLOGENETIC ANALYSIS; SOCIAL-ORGANIZATION; DISPLAY BEHAVIOR; SELECTION; EVOLUTION; CHOICE AB Most manakins (Pipridae) are lek-breeding species in which males engage in courtship displays directed toward females. Yet, the structure of leks and the complexity of the displays vary widely across species. Differences in male clustering and display attributes are expected to influence inter-specific patterns of lek activity. Here, we investigate how lek structure and display complexity affect vocalization activity at leks of six manakin species that co-occur in eastern Ecuador (Chiroxiphia pareola, Lepidothrix coronata, Machaeropterus regulus, Pipra erythrocephala, P. filicauda, and P pipra). Our results showed that, first, daily patterns of lek activity within species were consistent spatially (among leks) and temporally (across the breeding season), allowing for meaningful inter-specific comparisons. Second, that both lek structure (male spacing) and display complexity were predictors of vocal activity at leks but specific components of the vocalization output (e.g., output per male or per lek, temporal fluctuations in output levels) varied among species. This study adds to our understanding of how social structure and male-male social facilitation influence activity at leks. Accepted 10 August 2011. C1 [Duraes, Renata] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Blake, John G.; Loiselle, Bette A.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Loiselle, Bette A.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. [Ryder, Thomas B.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Tori, Wendy P.] Earlham Coll, Richmond, IN 47374 USA. RP Duraes, R (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, 400 Lindy Boggs Ctr, New Orleans, LA 70118 USA. EM john.blake@ufl.edu RI Hidalgo, Jose/C-3290-2014; Ribeiro, Renata/J-3943-2014; Loiselle, Bette/O-7106-2016 OI Ribeiro, Renata/0000-0002-8177-4109; Loiselle, Bette/0000-0003-1434-4173 FU National Science Foundation [IBN-0235141]; National Geographic Society [7113-01]; University of Missouri-St. Louis; Fundacao Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, Brazil) FX We thank J. Guerra, C. Romo, D. Romo, K. Swing, and all the staff at TBS and Universidad San Francisco de Quito for facilitating our research in Ecuador. We thank R. Macedo and D. B. McDonald for constructive comments that helped improve the manuscript. We worked under permission no. 13-IC-FAU-DFN granted by the Ministry of the Environment of Ecuador and Institutional Animal Care protocol no. 5-12-20. This work was funded by National Science Foundation (IBN-0235141), National Geographic Society (7113-01), and University of Missouri-St. Louis. RD was supported by a doctoral scholarship from Fundacao Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, Brazil). NR 28 TC 2 Z9 2 U1 4 U2 15 PU NEOTROPICAL ORNITHOLOGICAL SOC, USGS PATUXENT WILDLIFE RESEARCH CTR PI ATHENS PA UNIV GEORGIA, WARNELL SCH FOREST RESOURCES, ATHENS, GA 30602-2152 USA SN 1075-4377 J9 ORNITOL NEOTROP JI ORNITOL. NEOTROP. PY 2011 VL 22 IS 3 BP 437 EP 445 PG 9 WC Ornithology SC Zoology GA 918UC UT WOS:000302275600011 ER PT J AU Rick, TC Fitzpatrick, SM AF Rick, Torben C. Fitzpatrick, Scott M. TI The Journal of Island and Coastal Archaeology Turns Six SO JOURNAL OF ISLAND & COASTAL ARCHAEOLOGY LA English DT Editorial Material C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Fitzpatrick, Scott M.] N Carolina State Univ, Dept Sociol & Anthropol, Raleigh, NC 27695 USA. RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, POB 37012, Washington, DC 20013 USA. EM rickt@si.edu; scott_fitzpatrick@ncsu.edu NR 0 TC 0 Z9 0 U1 1 U2 3 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1556-4894 J9 J ISL COAST ARCHAEOL JI J. Isl. Coast. Archaeol. PY 2011 VL 6 IS 1 BP 1 EP 2 DI 10.1080/15564894.2011.555277 PG 2 WC Archaeology SC Archaeology GA 914GN UT WOS:000301937600001 ER PT S AU Cass, CAP Hazari, Z Cribbs, J Sadler, PM Sonnert, G AF Cass, Cheryl A. P. Hazari, Zahra Cribbs, Jennifer Sadler, Philip M. Sonnert, Gerhard GP IEEE TI Examining the Impact of Mathematics Identity on the Choice of Engineering Careers for Male and Female Students SO 2011 FRONTIERS IN EDUCATION CONFERENCE (FIE) SE Frontiers in Education Conference LA English DT Proceedings Paper CT 41st Annual Frontiers in Education Conference (FIE) CY OCT 12-15, 2011 CL Rapid City, SD SP IEEE Educ Soc, IEEE Comp Soc, Amer Soc Engn Educ (ASEE), Educl Res Methods (ERM), Inst Elect & Elect Engineers (IEEE), S Dakota Sch Mines & Technol DE Engineering career choice; Gender; Mathematics identity; Quantitative assessment AB Previous research suggests strong connections between mathematics background and persistence in engineering career aspirations. This study expands on this research by examining how mathematics identity impacts the choice of engineering careers for male and female students. Our framework encompasses interest, recognition, performance, and competence as central factors that contribute to the development of mathematics identity. The data used in this study were drawn from the Factors Influencing College Success in Mathematics (FICS-Math) project; the survey included questions on students' demographics, mathematics background/experiences, interest in mathematics, and career aspirations. Results indicate that factors of mathematics interest, mathematics competence and performance, and mathematics recognition are significant predictors of the choice of an engineering career, even after controlling for SAT/ACT math scores and demographics such as parental education. Moreover, the interaction between mathematics recognition and gender is also significant with the estimate indicating that females who are recognized in mathematics are more likely to choose engineering careers. This work reaffirms the importance of mathematics to engineering career choices and furthers the discussion by looking beyond mathematics grades to ascertaining the importance of mathematics identity. C1 [Cass, Cheryl A. P.] North Carolina State Univ, Dept Mat Sci & Engn, Chapel Hill, NC 27515 USA. [Hazari, Zahra; Cribbs, Jennifer] Clemson Univ, Clemson, SC USA. [Sadler, Philip M.; Sonnert, Gerhard] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA USA. RP Cass, CAP (reprint author), North Carolina State Univ, Dept Mat Sci & Engn, Chapel Hill, NC 27515 USA. EM cheryl_cass@ncsu.edu; zahra@clemson.edu; jdshipl@clemson.edu; psadler@cfa.harvard.edu; gsonnert@cfa.harvard.edu FU National Science Foundation [0813702] FX This material is based upon work supported by the National Science Foundation under Grant No. 0813702. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. We would like to thank all the FICS-Math team members and all the professors and students who participated in the study. NR 16 TC 0 Z9 0 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0190-5848 BN 978-1-61284-469-5 J9 PROC FRONT EDUC CONF PY 2011 PG 5 WC Computer Science, Interdisciplinary Applications; Education, Scientific Disciplines; Engineering, Electrical & Electronic SC Computer Science; Education & Educational Research; Engineering GA BYZ96 UT WOS:000300879800186 ER PT J AU Wieland, LM Mesquita, RCG Bobrowiec, PED Bentos, TV Williamson, GB AF Wieland, Lindsay M. Mesquita, Rita C. G. Bobrowiec, Paulo Estefano D. Bentos, Tony V. Williamson, G. Bruce TI Seed rain and advance regeneration in secondary succession in the Brazilian Amazon SO TROPICAL CONSERVATION SCIENCE LA English DT Article DE Vismia; Cecropia; secondary succession; seed dispersal; advance regeneration; Brazil; Amazon ID KIBALE NATIONAL-PARK; FOREST FRAGMENTATION; COMMUNITY COMPOSITION; ARRESTED SUCCESSION; ABANDONED PASTURE; EASTERN AMAZONIA; TROPICAL FOREST; PERUVIAN AMAZON; COSTA-RICA; DISPERSAL AB Succession in the Brazilian Amazon depends on prior land-use history. Abandoned clearcuts become dominated by Cecropia trees and exhibit species replacements characteristic of natural succession in forest lightgaps. In contrast, abandoned pastures are dominated by Vismia trees that inhibit natural succession for a decade or more. Here we explore how advance regeneration and limited seed dispersal may contribute to the arrested succession in Vismia-dominated stands. Vegetation surveys showed that every Vismia stem in 3-8 year old Vismia stands originated as a re-sprout. In Cecropia stands, all tree species, including Vismia, originated mostly from seeds, after deforestation and abandonment. The 100% re-sprouts of Vismia in the abandoned pastures confirms that Vismia dominance results from re-sprouting following pasture fires. Seed rain in both Vismia and Cecropia dominated stands was limited almost exclusively to second growth species already reproducing in those stands, suggesting that the bats and birds foraging there were not bringing mature forest seeds into the second growth, but simply feeding and depositing local second growth species. As dispersal was similar in both stand types, dispersal differences cannot account for the ongoing dominance of Vismia relative to the ongoing successional transitions in Cecropia stands. Overall, advance regeneration in the form of Vismia re-sprouts is much more likely to be the driver of Vismia dominated succession than differential dispersal of mature forest seeds. In order to avoid extensive forest conversion into unproductive Vismia wastelands in the Amazon Basin, forestry permits for harvesting timber should include restrictions on subsequent anthropogenic degradation, such as conversion to pasture and prescribed burning. C1 [Wieland, Lindsay M.; Williamson, G. Bruce] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Mesquita, Rita C. G.; Bobrowiec, Paulo Estefano D.; Bentos, Tony V.; Williamson, G. Bruce] Natl Inst Res Amazon INPA, Biol Dynam Forest Fragments Project, BR-69083000 Manaus, Amazonas, Brazil. [Mesquita, Rita C. G.; Bobrowiec, Paulo Estefano D.; Bentos, Tony V.; Williamson, G. Bruce] Smithsonian Trop Res Inst, BR-69083000 Manaus, Amazonas, Brazil. RP Wieland, LM (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. EM lwiela1@tigers.lsu.edu; rita@inpa.gov.br; pauloedb@inpa.gov.br; vizcarra@inpa.gov.br; btwill@lsu.edu RI Bobrowiec, Paulo Estefano/A-2630-2013 FU Conservation, Food & Health Foundation; National Science Foundation [DEB-0639114]; Louisiana State University Biograds FX Funding for this research was provided by the Conservation, Food & Health Foundation, the National Science Foundation (DEB-0639114), and Louisiana State University Biograds. Special thanks to A. M. dos Reis and C. Jackovac for assistance in the field and to the staff at the Biological Dynamics of Forest Fragments Project for logistical and technical support. Finally, thanks to P. C. Stouffer and R. Stevens for their thoughtful comments on various stages of this manuscript. Two anonymous reviewers provided insightful comments. This is publication # 583 in the Technical Series of the Biological Dynamics of Forest Fragments Project BDFFP-INPA-SI. NR 65 TC 13 Z9 13 U1 4 U2 32 PU TROPICAL CONSERVATION SCIENCE PI MENIO PARK PA PO BOX 0291, MENIO PARK, CA 94026-0291 USA SN 1940-0829 J9 TROP CONSERV SCI JI Trop. Conserv. Sci. PY 2011 VL 4 IS 3 BP 300 EP 316 PG 17 WC Biodiversity Conservation SC Biodiversity & Conservation GA 900QQ UT WOS:000300903900008 ER PT J AU Cairns, SD Lindner, A AF Cairns, Stephen D. Lindner, Alberto TI A Revision of the Stylasteridae (Cnidaria, Hydrozoa, Filifera) from Alaska and Adjacent Waters SO ZOOKEYS LA English DT Review DE Stylasteridae; Hydrozoa; Cnidaria; Aleutian Islands; Alaska; British Columbia; Stylaster; Errinopora ID ALEUTIAN ISLANDS; GENERIC REVISION; COELENTERATA; CORALS AB The stylasterid fauna of Alaska is revised, consisting of the description or redescription and illustration of 21 species, one additional subspecies, and a geographically adjacent species: Stylaster venustus. Six new species and one new subspecies are described: Errinopora fisheri, E. undulata, E. disticha, E. dichotoma, Stylaster crassiseptum, S. repandus, and Stylaster parageus columbiensis. Four subspecies are raised to species rank: Stylaster leptostylus, S. trachystomus, S. parageus, and Distichopora japonica, and five species and one subspecies were synonymized. A dichotomous key to the Errinopora species and tabular keys to the Errinopora and Alaskan Stylaster species are provided. The focus of the study was on the stylasterids from Alaska, primarily those from the diverse Aleutian Islands, but also including records from British Columbia. This is the first revisionary work on this fauna since the seminal report by Fisher in 1938. C1 [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Lindner, Alberto] Univ Fed Santa Catarina, Dept Ecol & Zool, BR-88040970 Florianopolis, SC, Brazil. RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM cairnss@si.edu RI Lindner, Alberto/E-1946-2013 FU National Science Foundation [NSF PEET DEB-9978086]; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) [BEX0917-0] FX We are grateful to the following people who generously loaned or gave us specimens to study: Anita Brinckmann-Voss, Arthur Schultz, Garry Fletcher, Steve Blair, 'Skip' Zenger, Jay Orr, Dale Calder, Bob van Syoc, Bob Stone, Bruce Wing, Kirsten Lindstrom, Mary Sue Brancato, Adam Baldinger, and John Pearse. We are indebted to Tim Coffer for constructing most of the figures and to Walter Larrimore for taking the color photographs. This work was partially funded by a National Science Foundation grant (NSF PEET DEB-9978086) and by a scholarship from Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES BEX0917-0) to A. Lindner. We also thank the reviewers for comments that improved the manuscript. NR 55 TC 6 Z9 7 U1 0 U2 8 PU PENSOFT PUBLISHERS PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2011 IS 158 BP 1 EP 88 DI 10.3897/zookeys.158.1910 PG 88 WC Zoology SC Zoology GA 903YG UT WOS:000301158600001 PM 22303109 ER PT J AU Konstantinov, AS Konstantinova, AA AF Konstantinov, A. S. Konstantinova, A. A. TI New genus and species of flea beetles (Coleoptera, Chrysomelidae, Galerucinae, Alticini) from Puerto Rico, with comments on flea beetle diversity in the West Indies and a key to the West Indian Monoplatini genera SO ZOOKEYS LA English DT Article DE Leaf beetles; species diversity; moss; West Indies; Puerto Rico AB A new genus (Borinken) and five new species (Borinken elyunque, Distigmoptera chamorrae, Kiskeya elyunque, Ulrica eltoro, and U. iviei) from Puerto Rico are described and illustrated. A key to all West Indian Monoplatini genera is provided, as are keys to all species of Kiskeya and to the species of Ulrica from Puerto Rico. A list of the flea beetle genera, along with the number of species and some of the faunal features is presented and discussed for the West Indies. C1 [Konstantinov, A. S.] ARS, ASK Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. [Konstantinova, A. A.] AAK Franklin W Olin Coll Engn, Needham, MA 02492 USA. RP Konstantinov, AS (reprint author), ARS, ASK Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,Natl Museum Nat Hist, POB 37012,MRC 168, Washington, DC 20013 USA. EM alex.konstantinov@ars.usda.gov NR 25 TC 3 Z9 3 U1 0 U2 3 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2011 IS 155 BP 61 EP 87 DI 10.3897/zookeys.155.2124 PG 27 WC Zoology SC Zoology GA 903YF UT WOS:000301158500003 PM 22291512 ER PT B AU Adey, W Bannon, J AF Adey, Walter Bannon, Jeffrey BE Bhatnagar, SK Saxena, A Kraan, S TI ALGAL TURF SCRUBBERS: CLEANING WATER WHILE CAPTURING SOLAR ENERGY SO ALGAE BIOFUEL LA English DT Article; Book Chapter DE Algal turf scrubbers; Solar energy; Cyanobacteria; Red algae; Environmental use; ATS engineering AB Present paper deals with the algal turfs and Algal Turf Scrubbers (ATS) which clean water and remove Carbon dioxide more efficiently from water and the atmosphere and can be configured to remove CO2 from power plant stack gases. Algal turfs are communities of organisms dominated by aggregations of unicellular to branched filamentous algae and cyanobacteria (blue-green algae). Algal Turf Scrubber is applied biomimicry, an ecologically engineered, algal turf dominated mini-ecosystem. The applications of ATS in monitoring various environmental parameters have been discussed. C1 [Bannon, Jeffrey] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Bannon, J (reprint author), Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. EM adey.walter@nmnh.si.edu; jbenemann@aol.com NR 42 TC 0 Z9 0 U1 0 U2 3 PU STUDIUM PRESS LLC PI HOUSTON PA PO BOX 722200, HOUSTON, TX 77072 USA BN 978-93-80012-44-5 PY 2011 BP 215 EP 227 PG 13 WC Biotechnology & Applied Microbiology; Energy & Fuels SC Biotechnology & Applied Microbiology; Energy & Fuels GA BTI83 UT WOS:000287046700012 ER PT S AU Banda, JM Angryk, RA Martens, PC AF Banda, Juan M. Angryk, Rafal A. Martens, Petrus C. GP IEEE TI ON THE SURPRISINGLY ACCURATE TRANSFER OF IMAGE PARAMETERS BETWEEN MEDICAL AND SOLAR IMAGES SO 2011 18TH IEEE INTERNATIONAL CONFERENCE ON IMAGE PROCESSING (ICIP) SE IEEE International Conference on Image Processing ICIP LA English DT Proceedings Paper CT 18th IEEE International Conference on Image Processing (ICIP) CY SEP 11-14, 2011 CL Brussels, BELGIUM SP IEEE, IEEE Signal Proc Soc (SPS) DE image processing; classification; solar image analysis; medical image analysis ID TEXTURAL FEATURES; RETRIEVAL-SYSTEMS AB In this work we report on the transfer of image parameters that produce good results for medical images to the domain of solar image analysis. Using the first solar domain-specific benchmark dataset that contains multiple types of solar phenomena we discovered during our work for constructing a content-based image retrieval (CBIR) system for NASA's Solar Dynamics Observatory (SDO) mission that we could take advantage of the research on the analysis of images in the medical field. We demonstrate that, while image analysis is a very domain-specific task, there are lessons to be learned and methods to be shared between different fields. In this paper we present an extensive comparative analysis of several different domain-specific datasets in order to provide some guidance for the solar physics community on the well-researched field of medical image analysis allowing them to transfer knowledge from one applied field to their own. C1 [Banda, Juan M.; Angryk, Rafal A.] Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 USA. [Martens, Petrus C.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Martens, Petrus C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Banda, JM (reprint author), Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 USA. FU NASA [08-SDOSC08-0008]; Solar Dynamics Observatory Science Center solicitation [NNH08ZDA001N-SDOSC] FX This work was supported in part by the NASA Grant Award No. 08-SDOSC08-0008, funded from NNH08ZDA001N-SDOSC: Solar Dynamics Observatory Science Center solicitation. NR 29 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1522-4880 BN 978-1-4577-1303-3 J9 IEEE IMAGE PROC PY 2011 PG 4 WC Engineering, Electrical & Electronic; Imaging Science & Photographic Technology SC Engineering; Imaging Science & Photographic Technology GA BYI89 UT WOS:000298962503201 ER PT J AU Holland, RA Meyer, CFJ Kalko, EKV Kays, R Wikelski, M AF Holland, Richard A. Meyer, Christoph F. J. Kalko, Elisabeth K. V. Kays, Roland Wikelski, Martin TI Emergence time and foraging activity in Pallas' mastiff bat, Molossus molossus (Chiroptera: Molossidae) in relation to sunset/sunrise and phase of the moon SO ACTA CHIROPTEROLOGICA LA English DT Article DE Molossus molossus; emergence; foraging; nocturnal; predator pressure; activity ID CAROLLIA-CASTANEA PHYLLOSTOMIDAE; AERIAL INSECTIVOROUS BATS; PREDATION RISK; ACTIVITY PATTERNS; RADIO-TELEMETRY; LUNAR PHOBIA; FOREST; PERSPICILLATA; URBANIZATION; ENVIRONMENT AB The decision on when to emerge from the safety of a roost and forage for prey is thought to be a result of the trade off between peak insect abundance and predation pressure for bats. In this study we show that the velvety free-tailed bat Molossus molossus emerges just after sunset and just before sunrise for very short foraging bouts (average 82.2 min foraging per night). Contrary to previous studies, bats remain inactive in their roost between activity patterns. Activity was measured over two complete lunar cycles and there was no indication that phase of the moon had an influence on emergence time or the numbers of bats that emerged from the roost. This data suggests that M. molossus represents an example of an aerial hawking bat whose foraging behaviour is in fact adapted to the compromise between the need to exploit highest prey availability and the need to avoid predation. C1 [Holland, Richard A.] Univ Leeds, IICB, Leeds LS2 9JT, W Yorkshire, England. [Meyer, Christoph F. J.] Univ Lisbon, Fac Ciencia, Ctr Biol Ambiental, P-1749016 Lisbon, Portugal. [Kalko, Elisabeth K. V.; Kays, Roland] Smithsonian Trop Res Inst, Balboa, Panama. [Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kays, Roland] New York State Museum & Sci Serv, Albany, NY 12230 USA. [Wikelski, Martin] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. [Holland, Richard A.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. RP Holland, RA (reprint author), Queens Univ Belfast, Ctr Med Biol, Sch Biol Sci, 97 Lisburn Rd, Belfast BT9 7BL, Antrim, North Ireland. EM r.holland@qub.ac.uk RI Holland, Richard/A-6107-2010; OI Holland, Richard/0000-0003-4495-8061; Meyer, Christoph F. J./0000-0001-9958-8913 FU Marie Curie grant [MOIF-CT-2005-021508] FX We thank Dina Dechmann for helpful comments on the manuscript. Thanks to Christian Ziegler, Daniel Obando and Alejandro Ortega for help with the motion sensor. R.A.H. was supported by Marie Curie grant MOIF-CT-2005-021508. NR 35 TC 7 Z9 8 U1 2 U2 24 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 EI 1733-5329 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2011 VL 13 IS 2 BP 399 EP 404 DI 10.3161/150811011X624875 PG 6 WC Zoology SC Zoology GA 901ZJ UT WOS:000301008100015 ER PT J AU Jenks, KE Chanteap, P Damrongchainarong, K Cutter, P Cutter, P Redford, T Lynam, AJ Howard, J Leimgruber, P AF Jenks, Kate E. Chanteap, Prawatsart Damrongchainarong, Kanda Cutter, Peter Cutter, Passanan Redford, Tim Lynam, Antony J. Howard, JoGayle Leimgruber, Peter TI Using relative abundance indices from camera-trapping to test wildlife conservation hypotheses - an example from Khao Yai National Park, Thailand SO TROPICAL CONSERVATION SCIENCE LA English DT Article DE large mammals; protected area management; wildlife monitoring ID CAT PRIONAILURUS-BENGALENSIS; DOMESTIC DOGS; NEOFELIS-NEBULOSA; ETHIOPIAN WOLVES; CLOUDED LEOPARD; ECOLOGY; FOREST; COMMUNITY; MAMMALS; TIGERS AB Khao Yai National Park (KYNP) is well known for its biodiversity and has the potential to serve as a regional model for wildlife conservation. From October 2003 through October 2007, the managers of KYNP conducted a Carnivore Conservation Project to develop and implement long-term monitoring of their large mammal populations. We present these data as an example to demonstrate the usefulness of long-term camera-trapping despite data that cannot be fitted to mark/recapture or occupancy statistical frameworks. Overall, a relatively high number of camera trap photographs was obtained for viverrids (four species; 44 photos) and ursids (two species; 39 photos). However, a relatively low number (range, one to eight) of camera trap photographs was obtained for each of the four felid species and two canid species detected by cameras. Of a total survey effort of 6,260 trap nights, no tigers (Panthera tigris) were detected by camera traps, suggestive of at best a small, non-viable tiger population. Compared to previous camera-trapping efforts at KYNP, we expanded intensive sampling beyond the core area to include all zones and edges of the park. We found significantly lower relative abundance indices (RAIs) for certain mammal species, and collectively for all mammals compared to data obtained in 1999-2000 from 34 similar survey locations, suggesting population declines linked to increased human activity. Information from long-term camera-trapping can provide critical information on the occurrence of elusive species, hotspots, the role of invasive or domestic species, and an indication of the effectiveness of patrolling and other management and conservation interventions. C1 [Jenks, Kate E.] Univ Massachusetts, Grad Program Organism & Evolutionary Biol, Amherst, MA 01003 USA. [Jenks, Kate E.] Univ Massachusetts, Grad Program Wildlife & Fisheries Conservat, Amherst, MA 01003 USA. [Jenks, Kate E.; Damrongchainarong, Kanda; Howard, JoGayle; Leimgruber, Peter] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Damrongchainarong, Kanda; Redford, Tim] FREELAND Fdn, Bangkok 10110, Thailand. [Cutter, Peter] Thailand Country Off, WWF Greater Mekong Programme, Bangkok 10900, Thailand. [Cutter, Passanan] Fishing Cat Res & Conservat Project, Prachuap Kiri Khan 77150, Thailand. [Lynam, Antony J.] Wildlife Conservat Soc, Global Conservat Program, Bronx, NY 10460 USA. RP Jenks, KE (reprint author), Univ Massachusetts, Grad Program Organism & Evolutionary Biol, 611 N Pleasant St, Amherst, MA 01003 USA. EM kate@katejenks.info RI Leimgruber, Peter/O-1304-2015; OI Leimgruber, Peter/0000-0002-3682-0153; Lynam, Antony/0000-0002-8395-7902 FU Thailand Department of National Park, Wildlife, and Plant Conservation; North American zoos FX Many individuals contributed to the success of this project and research. Park Superintendent P. Wohandee provided vision and foresight about the importance of monitoring for biodiversity conservation. Park rangers and team leaders B. Boonpeng, W. Kongsiri, M. Penprathom, S. Narongsak, P. Saenkod, P. Sontienwat, and N. Sungsuwan, with additional rangers from the park's substations, spent many days and hours under difficult field conditions to collect the data. Their dedication was essential. S. Galster and B. Senior of FREELAND provided substantial material and intellectual support. Earlier versions of the manuscript were edited by T. K. Fuller, S. DeStefano, L. Godfrey, N. Songsasen, and B. Houseman. This project and research were supported by the Thailand Department of National Park, Wildlife, and Plant Conservation and funded by donations from North American zoos participating in the American Zoo and Aquarium Association (AZA) Felid Taxon Advisory Group, and the AZA Clouded Leopard Species Survival Plan, along with Friends of the National Zoo. We also credit J. Aynes (Oakhill Center of Rare and Endangered Species) and B. Antle ( T. I. G. E. R. S. and Rare Species Fund) for their substantial support for the training course and field surveys. We thank three anonymous reviewers for their extensive comments and useful suggestions. NR 38 TC 20 Z9 30 U1 6 U2 66 PU TROPICAL CONSERVATION SCIENCE PI MENIO PARK PA PO BOX 0291, MENIO PARK, CA 94026-0291 USA SN 1940-0829 J9 TROP CONSERV SCI JI Trop. Conserv. Sci. PY 2011 VL 4 IS 2 BP 113 EP 131 PG 19 WC Biodiversity Conservation SC Biodiversity & Conservation GA 900QD UT WOS:000300902300003 ER PT J AU Staines, CL AF Staines, Charles L. TI Hispines (Chrysomelidae, Cassidinae) of La Selva Biological Station, Costa Rica SO ZOOKEYS LA English DT Article DE Chrysomelidae; hispine; La Selva Biological Station ID LEAF BEETLES COLEOPTERA; DISTRIBUTIONAL RECORDS; PARASITOID COMMUNITY; HELICONIA; INSECT; ZINGIBERALES; HERBIVORES; CEPHALOLEIINI; COMPETITION; EVOLUTION AB Survey work from 1992-2001 identified 139 species of hispines at the lowland part of La Selva Biological Station, Costa Rica. The tribe Cephaloleiini was the most speciose with 58 species (41.7%) followed by the Chalepini with 55 (39.5%). The fauna is most closely related to that in South America but with some genera which are more speciose in the Nearctic Region. Plant associations are known for 88 (63.3%) of the species but many of these are merely collecting records, not host plant associations. The first plant associations are reported for Alurnus ornatus, A. salvini, and Acentroptera nevermanni. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Staines, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM stainesc@si.edu FU NSF [BSR-9025024, DEB 9401069, DEB 9706976] FX I thank Jack Longino, Evergreen State College, and Henry Hespenheide, University of California at Los Angeles, for inviting me to participate in the ALAS project, Danilo Brenes, Ronald Vargas, Maylin Paniagua, and Nelci Oconotrillo, the ALAS parataxonomists, for their work in specimen collecting and processing. Funding for field work as provided by NSF grants BSR-9025024, DEB 9401069, and DEB 9706976. NR 81 TC 6 Z9 6 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2011 IS 157 SI SI BP 45 EP 65 DI 10.3897/zookeys.157.1338 PG 21 WC Zoology SC Zoology GA 899FC UT WOS:000300800800004 PM 22303103 ER PT J AU Rappole, JH Glasscock, S Goldberg, K Song, D Faridani, S AF Rappole, J. H. Glasscock, S. Goldberg, K. Song, D. Faridani, S. TI RANGE CHANGE AMONG NEW WORLD TROPICAL AND SUBTROPICAL BIRDS SO BONNER ZOOLOGISCHE MONOGRAPHIEN LA English DT Article ID AVIAN COMMUNITY; CLIMATE-CHANGE; TEXAS AB Range change is occurring at a rapid rate for tropical, subtropical, and warns desert birds in Texas. Comparisons between former(1974) and current avian distributions for the region show significant breeding range extension of 40-220 km to the N, NE, or E for at least 68 species, many of which cross major biogeographic boundaries. Fieldwork at the northern end of the subtropics along the coastal plain of the Gulf of Mexico has provided extensive documentation of breeding populations in new areas (e.g., nests, eggs, nestlings, fledglings, pairs, singing males on territory, and response to playback) for nine subtropical species (e.g., Green Jay Cyanocorax yncas and White-tipped Dove Leptotila verreauxi), as well as photographic evidence of seasonal persistence derived from use of a novel, web-based collaborative online robotic wildlife camera. Poor previous documentation, population change, habitat loss in the former range, and habitat change in the new range are considered as possible explanations. We conclude that change in key parameters of habitat, e.g. seasonal food availability, as affected by factors related to climatic change, e.g., mean annual precipitation, temporal distribution of precipitation (monthly means), or monthly means for nighttime-low temperatures during the breeding season, provide the most likely explanations for observed range extensions. At present, movement of a large segment of the subtropical avian community into temperate habitats has not been met with a corresponding shift of temperate species as had been predicted by a number of models; rather the communities now overlap, creating, in effect, novel communities. Results of this overlap are likely to produce profound changes that may first be evident in the genetics of subtropical/temperate species pairs, e.g., Black-crested Titmouse Baeolophus atricapillus and Tufted Titmouse Baeolophus bicolor. RP Rappole, JH (reprint author), Conservat & Res Ctr, Smithsonian Natl Zool Pk,1500 Remount Rd, Front Royal, VA USA. EM rappolej@si.edu OI Goldberg, Ken/0000-0001-6747-9499 NR 64 TC 1 Z9 1 U1 1 U2 17 PU ZOOLOGISCHES FORSCHUNGSINSTITUT & MUSEUM ALEXANDER KOENIG PI BONN PA ADENAUERALLEE 160, BONN, 00000, GERMANY SN 0302-671X J9 BONN ZOOL MONOGR JI Bonn. Zool. Monogr. PY 2011 IS 57 BP 151 EP 167 PG 17 WC Zoology SC Zoology GA 895BY UT WOS:000300472400010 ER PT J AU Chew, DM Cardona, A Miskovic, A AF Chew, David M. Cardona, Agustin Miskovic, Aleksandar TI Tectonic evolution of western Amazonia from the assembly of Rodinia to its break-up SO INTERNATIONAL GEOLOGY REVIEW LA English DT Article DE Amazonia; Rodinia; supercontinent; geochronology; palaeomagnetism ID LAURENTIA-GONDWANA LINK; SOUTH-AMERICA; COLOMBIAN ANDES; GRENVILLE PROVINCE; EASTERN LAURENTIA; PERUVIAN ANDES; NORTHERN CHILE; IAPETUS OCEAN; PROTO-ANDES; ND ISOTOPES AB Plate tectonic reconstructions of the late Mesoproterozoic-Neoproterozoic supercontinent of Rodinia juxtapose the western margin of Amazonia against eastern Laurentia based on palaeomagnetic, isotopic, and geological evidence. Mesoproterozoic ('Grenvillian') orogenic belts are of crucial importance to these reconstructions as they act as key tectonic tracers for Amazonia-Laurentia interactions. They include orogenic belts sited on Amazonia (such as the Sunsas Orogen), para-autochthonous elements such as the Mesoproterozoic metamorphic basement inliers within the Andean Belt (e.g. in the Colombian Andes), exotic terranes accreted to Amazonia during Rodinia assembly (such as the Arequipa Massif), and orphaned fragments of Amazonian basement in Central and North America. A review of the timing of Sunsas orogenesis demonstrates that it occurred from about 1.2-1 Ga in eastern Bolivia and the western Amazon region of Brazil. This is significantly older than the timing of metamorphism in Mesoproterozoic basement inliers of the Colombian Andes, which record a late metamorphic event between 0.9 and 1.0 Ga. Orphaned fragments of Amazonian basement in Laurentia (such as the Blue Ridge/Mars Hill terrane) suggest collision between southeastern Laurentia and Amazonia at ca. 1.15 Ga. The Arequipa Massif (and Antofalla Basement) most likely represents an exotic basement terrane that was caught up in the collision of southeastern Laurentia with western Amazonia. Recent palaeomagnetic data suggest that Amazonia moved northeastwards along the eastern Laurentian margin during Grenvillian collision. Amazonia evidently collided with southern Laurentia at ca. 1200 Ma and, as a result of progressive dextral transcurrent movement, it encountered the Labrador-Greenland sector of eastern Laurentia (and possibly Baltica) by 980 Ma. The timing of the Rodinia break-up in western Amazonia is poorly constrained. Evidence exists supporting a Neoproterozoic western Amazonian active margin, which would imply its at least partial separation from the conjugate rift margin of eastern Laurentia (i.e. formation of a proto-Iapetus Ocean) prior to ca. 650 Ma. This rifting event may be linked to A-type magmatism at ca. 770-690 Ma which is documented in both southeast Laurentia and western Amazonia. Final separation must have been completed by Early Cambrian times based on the unequivocal evidence for drift-related sedimentation on the Laurentian margin of the Iapetus Ocean. C1 [Chew, David M.] Trinity Coll Dublin, Dept Geol, Dublin, Ireland. [Cardona, Agustin] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Miskovic, Aleksandar] MIT, Cambridge, MA 02139 USA. RP Chew, DM (reprint author), Trinity Coll Dublin, Dept Geol, Dublin, Ireland. EM chewd@tcd.ie RI Chew, David/B-7828-2008 OI Chew, David/0000-0002-6940-1035 FU Swiss National Science Foundation FX Professor Wilson Teixeira is thanked for constructive comments which greatly improved this manuscript. Support from the Swiss National Science Foundation under grants awarded to Urs Schaltegger of the University of Geneva is acknowledged. NR 83 TC 9 Z9 9 U1 2 U2 23 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0020-6814 J9 INT GEOL REV JI Int. Geol. Rev. PY 2011 VL 53 IS 11-12 SI SI BP 1280 EP 1296 DI 10.1080/00206814.2010.527630 PG 17 WC Geology SC Geology GA 837KE UT WOS:000296199500003 ER PT S AU Grant, JA Leuschen, CJ AF Grant, John A. Leuschen, Carlton J. GP IEEE TI The Strata Ground Penetrating Radar as a Means for Constraining the Near Surface Properties of the Moon and Mars SO 2011 IEEE RADAR CONFERENCE (RADAR) SE IEEE National Radar Conference Proceedings LA English DT Proceedings Paper CT IEEE Radar Conference (RADAR) CY MAY 23-27, 2011 CL Kansas City, MO SP IEEE, IEEE Aerosp & Elect Syst Soc (AESS), IEEE Kansas City Sect, IEEE Microwave Theory & Tech Soc, IEEE Geosci & Remote Sensing Soc, KURSL ID ART. NO. E09002; METEOR CRATER; ARIZONA AB Strata is a low-mass, low-power, and low-volume impulse ground penetrating radar operating at 400 MHz and capable of defining subsurface stratigraphy and structure at the spatial resolution of tens of centimeters to 10-15 m depth. Strata would be used along transects suitable for to characterizing regolith properties on the Moon or distinguishing habitable environments on Mars. C1 [Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 6 & Independence Ave SW, Washington, DC 20560 USA. [Leuschen, Carlton J.] Univ Kansas, Dept Elect Engn & Comp Sci, Lawrence, KS 66045 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 6 & Independence Ave SW, Washington, DC 20560 USA. EM grantj@si.edu NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5659 BN 978-1-4244-8902-2 J9 IEEE NATL RADAR CONF PY 2011 BP 1132 EP 1134 PG 3 WC Engineering, Electrical & Electronic; Remote Sensing; Telecommunications SC Engineering; Remote Sensing; Telecommunications GA BWZ74 UT WOS:000295457000224 ER PT J AU Faynel, C Busby, RC Moser, A Robbins, RK AF Faynel, Christophe Busby, Robert C. Moser, Alfred Robbins, Robert K. TI Species level taxonomy of the Neotropical hairstreak genus Porthecla (Lepidoptera: Lycaenidae: Theclinae: Eumaeini) SO ANNALES DE LA SOCIETE ENTOMOLOGIQUE DE FRANCE LA English DT Article DE Oenomaus; Thepytus; South-America; lectotypes; wing pattern ID OENOMAUS-HUBNER; FRENCH-GUIANA; BUTTERFLIES AB The species level taxonomy of Porthecla is revised. Six previously described species are recognized: P. ravus (Druce 1907); P. barba (Druce 1907); P. dinus (Hewitson 1867); P. porthura (Druce 1907); P. minyia (Hewitson 1867); P. gemma (Druce 1907), and another six new species are proposed: P. forasteira Faynel & Moser n. sp.; P. annette Faynel & Robbins n. sp.; P. johanna Faynel & Robbins n. sp.; P. peruensis Faynel & Moser n. sp.; P. prietoi Faynel & Busby n. sp. and P. willmotti Busby, Faynel & Moser n. sp. For each Porthecla species we present diagnostic characters, images of male and female adults, drawings of male and female genitalia, distribution maps, and notes on habitat and other biological traits. An identification key for males is provided. To stabilize names; lectotypes are designated for Thecla minyia Hewitson 1867, and Thecla gemma Druce 1907. Wing pattern resemblances between Porthecla and other genera are discussed. C1 [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Faynel, C (reprint author), 16 Rue Aspres, F-34160 Montaud, France. EM christophe.faynel@wanadoo.fr; rc.busby@comcast.net; a.moser@ensinger.com.br; RobbinsR@SI.edu NR 28 TC 2 Z9 2 U1 0 U2 3 PU SOC ENTOMOLOGIQUE FRANCE PI PARIS PA 45 RUE BUFFON, 75005 PARIS, FRANCE SN 0037-9271 J9 ANN SOC ENTOMOL FR JI Ann. Soc. Entomol. Fr. PD JAN-JUN PY 2011 VL 47 IS 1-2 BP 241 EP 259 PG 19 WC Entomology SC Entomology GA 830JN UT WOS:000295653400025 ER PT J AU Lucas, SG Allen, BD Krainer, K Barrick, J Vachard, D Schneider, JW DiMichele, WA Bashforth, AR AF Lucas, Spencer G. Allen, Bruce D. Krainer, Karl Barrick, James Vachard, Daniel Schneider, Joerg W. DiMichele, William A. Bashforth, Arden R. TI Precise age and biostratigraphic significance of the Kinney Brick Quarry Lagerstatte, Pennsylvanian of New Mexico, USA SO STRATIGRAPHY LA English DT Article ID GLOBAL GZHELIAN STAGE; NORTH-AMERICA; CARBONIFEROUS SYSTEM; MIDCONTINENT; FUSULINIDS; BOUNDARY; EUROPE; MARKER; SERIES; BASE AB The Kinney Brick Quarry is a world famous Late Pennsylvanian fossil Lagerstatte in central New Mexico, USA. The age assigned to the Kinney Brick Quarry (early-middle Virgilian) has long been based more on its inferred lithostratigraphic position than on biostratigraphic indicators at the quarry. We have developed three datasets-stratigraphic position, fusulinids and conodonts-that indicate the Kinney Brick Quarry is older, of middle Missourian (Kasimovian) age. Our detailed local lithostratigraphic studies coupled with regional stratigraphic investigations indicate the Kinney Brick Quarry is in the Tinajas Member of the Atrasado Formation, so it is stratigraphically lower than suggested by previously published maps. A laterally extensive fusulinid-bearing limestone a few meters below the level of the Kinney Brick Quarry yields an early-middle Missourian fusulinid assemblage consisting of Tumulotriticites cf. T tumidus and species of Triticites: T. cf. T. planus, T. cf. T. myersi and T. ex gr. T. ohioensis. The Kinney conodont fauna is characterized by Idiognathodus corrugatus and I. cherryvalensis, which suggest an assignment to the Idiognathodus confragus Zone of the North America Midcontinent region (Dennis cyclothem; middle Missourian). Nonmarine biostratigraphic indicators at the Kinney Brick Quarry indicate either an imprecise age (Late Pennsylvanian: megaflora) or a slightly younger age (late Kasimovian-early Gzhelian: blattids) than do stratigraphic position and marine microfossils. The well-established age of Kinney on the marine timescale thus can be used to better calibrate the nonmarine biostratigraphy. So, the insect biozonation of the Euramerican continental basins, which was calibrated to the so-called regional West European Carboniferous stages by macrofloras and to the global marine scale by sparse, ambiguous isotopic ages, can now be linked directly to the marine conodont zonation. C1 [Lucas, Spencer G.] New Mexico Museum Nat Hist, Albuquerque, NM 87104 USA. [Allen, Bruce D.] New Mexico Bur Geol & Mineral Resources, Socorro, NM 87801 USA. [Krainer, Karl] Univ Innsbruck, Inst Geol & Paleontol, A-6020 Innsbruck, Austria. [Barrick, James] Texas Tech Univ, Dept Geosci, Lubbock, TX 79409 USA. [Vachard, Daniel] Univ Sci & Technol Lille, UFR Sci Terre, UPRESA 8014, CNRS,Lab LP3, F-59655 Villeneuve Dascq, Crdex, France. [Schneider, Joerg W.] TU Bergakad Freiberg, D-09596 Freiberg, Germany. [DiMichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Bashforth, Arden R.] Univ Copenhagen, Nat Hist Museum Denmark, Geol Museum, DK-1350 Copenhagen K, Denmark. RP Lucas, SG (reprint author), New Mexico Museum Nat Hist, 1801 Mt Rd NW, Albuquerque, NM 87104 USA. EM Spencer.lucas@state.nm.us; allenb@gis.nmt.edu; Karl.Krainer@uibk.ac.at; Jim.Barrick@ttu.edu; daniel.vachard@univ-lille1.fr; Joerg.Schneider@geo.tu-freiberg.de; DIMICHEL@si.edu; bashforth@snm.ku.dk RI DiMichele, William/K-4301-2012; Bashforth, Arden/H-6057-2013 OI Bashforth, Arden/0000-0003-3050-7032 NR 117 TC 6 Z9 7 U1 0 U2 2 PU MICROPALEONTOLOGY PRESS PI NEW YORK PA 256 FIFTH AVE, NEW YORK, NY 10001 USA SN 1547-139X J9 STRATIGRAPHY JI Stratigraphy PY 2011 VL 8 IS 1 BP 7 EP 27 PG 21 WC Geology; Paleontology SC Geology; Paleontology GA 829GJ UT WOS:000295566300002 ER PT J AU West, CF AF West, Catherine F. TI A Revised Radiocarbon Sequence for Karluk-1 and the Implications for Kodiak Island Prehistory SO ARCTIC ANTHROPOLOGY LA English DT Article ID ALASKA; CALIBRATION; GULF AB The Karluk-1 site has played a central role in defining the late prehistory of the Kodiak archipelago, in particular the Koniag tradition and its genesis. As part of the Bryn Mawr College Karluk Archaeology Project, Richard Jordan and Richard Knecht excavated the site in the 1980s and obtained six radiocarbon dates. Here, I add 21 new dates for the Karluk-1 site, which suggest that the site was occupied approximately 250-300 years later than previously thought. These new dates help to refine our understanding of Karluk's place in prehistory and raise questions about the role of the Little Ice Age in driving cultural changes observed at Karluk-1. C1 Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Smithsonian Inst, Washington, DC 20013 USA. RP West, CF (reprint author), Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Smithsonian Inst, Washington, DC 20013 USA. NR 41 TC 3 Z9 3 U1 0 U2 0 PU UNIV WISCONSIN PRESS PI MADISON PA JOURNAL DIVISION, 1930 MONROE ST, 3RD FL, MADISON, WI 53711 USA SN 0066-6939 J9 ARCTIC ANTHROPOL JI Arct. Anthropol. PY 2011 VL 48 IS 1 BP 80 EP 92 PG 13 WC Anthropology SC Anthropology GA 822IE UT WOS:000295036800006 ER PT S AU Grimm, V Calabrese, JM AF Grimm, Volker Calabrese, Justin M. BA Deffuant, G Gilber, N BF Deffuant, G Gilber, N TI What Is Resilience? A Short Introduction SO VIABILITY AND RESILIENCE OF COMPLEX SYSTEMS: CONCEPTS, METHODS AND CASE STUDIES FROM ECOLOGY AND SOCIETY SE Understanding Complex Systems Springer Complexity LA English DT Editorial Material; Book Chapter ID GLOBAL ENVIRONMENTAL-CHANGE; SOCIAL-ECOLOGICAL SYSTEMS; SCHOLARLY NETWORKS; HUMAN DIMENSIONS; VULNERABILITY; ADAPTATION; STABILITY; LESSONS; PATTERN C1 [Grimm, Volker; Calabrese, Justin M.] UFZ Helmholtz Ctr Environm Res, D-04318 Leipzig, Germany. [Calabrese, Justin M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Grimm, V (reprint author), UFZ Helmholtz Ctr Environm Res, Permoserstr 15, D-04318 Leipzig, Germany. EM volker.grimm@ufz.de; CalabreseJ@si.edu NR 30 TC 8 Z9 8 U1 1 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1860-0832 BN 978-3-642-20422-7 J9 UNDERST COMPLEX SYST PY 2011 BP 3 EP 13 DI 10.1007/978-3-642-20423-4_1 D2 10.1007/978-3-642-20423-4 PG 11 WC Mathematics, Interdisciplinary Applications; Social Sciences, Interdisciplinary SC Mathematics; Social Sciences - Other Topics GA BWO44 UT WOS:000294391700001 ER PT S AU Martin, S Deffuant, G Calabrese, JM AF Martin, Sophie Deffuant, Guillaume Calabrese, Justin M. BA Deffuant, G Gilber, N BF Deffuant, G Gilber, N TI Defining Resilience Mathematically: From Attractors To Viability SO VIABILITY AND RESILIENCE OF COMPLEX SYSTEMS: CONCEPTS, METHODS AND CASE STUDIES FROM ECOLOGY AND SOCIETY SE Understanding Complex Systems Springer Complexity LA English DT Article; Book Chapter ID ECOLOGICAL-SYSTEMS; MODEL; COMMUNITIES; MANAGEMENT; DYNAMICS C1 [Martin, Sophie; Deffuant, Guillaume] Cemagref L1SC, F-63172 Aubiere, France. [Calabrese, Justin M.] UFZ Helmholtz Ctr Environm Res, D-04318 Leipzig, Germany. [Calabrese, Justin M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Deffuant, G (reprint author), Cemagref L1SC, 24 Av Landais, F-63172 Aubiere, France. EM sophie.martin@cemagref.fr; guillaume.deffuant@cemagref.fr; CalabreseJ@si.edu; guillaume.deffuant@cemagref.fr NR 18 TC 4 Z9 4 U1 1 U2 3 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1860-0832 BN 978-3-642-20422-7 J9 UNDERST COMPLEX SYST PY 2011 BP 15 EP 36 DI 10.1007/978-3-642-20423-4_2 D2 10.1007/978-3-642-20423-4 PG 22 WC Mathematics, Interdisciplinary Applications; Social Sciences, Interdisciplinary SC Mathematics; Social Sciences - Other Topics GA BWO44 UT WOS:000294391700002 ER PT S AU Calabrese, JM Deffuant, G Grimm, V AF Calabrese, Justin M. Deffuant, Guillaume Grimm, Volker BA Deffuant, G Gilber, N BF Deffuant, G Gilber, N TI Bridging the Gap Between Computational Models and Viability Based Resilience in Savanna Ecosystems SO VIABILITY AND RESILIENCE OF COMPLEX SYSTEMS: CONCEPTS, METHODS AND CASE STUDIES FROM ECOLOGY AND SOCIETY SE Understanding Complex Systems Springer Complexity LA English DT Article; Book Chapter ID SEMIARID SAVANNAS; SOUTHERN KALAHARI; AFRICAN SAVANNAS; SIMULATION-MODEL; FIRE; TREE; DYNAMICS; GRASS; COEXISTENCE; PATTERN C1 [Calabrese, Justin M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Calabrese, Justin M.; Grimm, Volker] UFZ Helmholtz Ctr Environm Res, D-04318 Leipzig, Germany. [Deffuant, Guillaume] Cemagref LISC, F-63172 Aubiere, France. RP Calabrese, JM (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM CalabreseJ@si.edu; guillaume.deffuant@cemagref.fr; volker.grimm@ufz.de NR 38 TC 2 Z9 2 U1 1 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1860-0832 BN 978-3-642-20422-7 J9 UNDERST COMPLEX SYST PY 2011 BP 107 EP 130 DI 10.1007/978-3-642-20423-4_5 D2 10.1007/978-3-642-20423-4 PG 24 WC Mathematics, Interdisciplinary Applications; Social Sciences, Interdisciplinary SC Mathematics; Social Sciences - Other Topics GA BWO44 UT WOS:000294391700005 ER PT B AU Ubelaker, DH Montaperto, KM AF Ubelaker, Douglas H. Montaperto, Kristin M. BE Ross, AH Abel, SM TI Biomechanical and Remodeling Factors in the Interpretation of Fractures in Juveniles SO JUVENILE SKELETON IN FORENSIC ABUSE INVESTIGATIONS LA English DT Article; Book Chapter ID MAMMALIAN LONG BONES; BLUNT FORCE TRAUMA; CHILD-ABUSE; SKELETAL SURVEY; HATCHET TRAUMA; RIB FRACTURE; INFANT ABUSE; HEAD-INJURY; PATTERNS; FEMUR AB Interpretation of juvenile trauma requires understanding of biomechanical and remodeling factors, as well as the dynamics of the growth process. Although terminology relating especially to biomechanical factors can be complex, use of proper terms is essential to avoid misunderstanding. Analysis can include direct observation, individual history documentation, radiography, microscopy, and bone scintigram study. In addition to the appearance of the trauma, relevant observations include the type and area of bone involved, age of the individual, and possible evidence of repair. Such analysis can elucidate the nature of juvenile trauma and facilitate interpretation of the timing of fracture events. C1 [Ubelaker, Douglas H.; Montaperto, Kristin M.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM ubelaked@si.edu; montapek@si.edu NR 87 TC 5 Z9 5 U1 2 U2 9 PU HUMANA PRESS INC PI TOTOWA PA 999 RIVERVIEW DR, STE 208, TOTOWA, NJ 07512-1165 USA BN 978-1-61779-254-0 PY 2011 BP 33 EP 48 DI 10.1007/978-1-61779-255-7_4 D2 10.1007/978-1-61779-255-7 PG 16 WC Anthropology; Archaeology; Criminology & Penology; Medicine, Legal; Pediatrics; Social Work; Sociology SC Anthropology; Archaeology; Criminology & Penology; Legal Medicine; Pediatrics; Social Work; Sociology GA BWI29 UT WOS:000293929200004 ER PT S AU Kress, WJ AF Kress, W. John BE Stuessy, TF Lack, HW TI DNA barcoding and systematic monographs SO MONOGRAPHIC PLANT SYSTEMATICS: FUNDAMENTAL ASSESSMENT OF PLANT BIODIVERSITY SE Regnum Vegetabile LA English DT Article; Book Chapter ID LAND PLANTS; FOREST TREE; SEED PLANTS; IDENTIFICATION; COMMUNITY; IDENTIFY; DISCRIMINATE; DIVERSITY; TAXONOMY; SUCCESS C1 Smithsonian Inst, Dept Bot, MRC US Natl Herbarium 166, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Kress, WJ (reprint author), Smithsonian Inst, Dept Bot, MRC US Natl Herbarium 166, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM kressj@si.edu NR 72 TC 0 Z9 0 U1 0 U2 1 PU A R G GANTNER VERLAG K G PI KOENIGSTEIN PA C/O KOELTZ SCIENTIFIC BOOKS, PO BOX 1360, KOENIGSTEIN, D-61453, GERMANY SN 0080-0694 BN 978-3-906166-98-8 J9 REGNUM VEG JI Regnum Veg. PY 2011 VL 153 BP 49 EP 71 PG 23 WC Plant Sciences SC Plant Sciences GA BWR47 UT WOS:000294660500005 ER PT S AU Garry, WB Bleacher, JE AF Garry, W. Brent Bleacher, Jacob E. BE Ambrose, WA Williams, DA TI Emplacement scenarios for Vallis Schroteri, Aristarchus Plateau, the Moon SO RECENT ADVANCES AND CURRENT RESEARCH ISSUES IN LUNAR STRATIGRAPHY SE Geological Society of America Special Papers LA English DT Article; Book Chapter ID LAVA FLOW MORPHOLOGY; LUNAR SINUOUS RILLS; EROSION; REGION; DEPOSITS; CHANNEL; EARTH; STRATIGRAPHY; TOPOGRAPHY; VISCOSITY AB The volcanic processes that formed Vallis Schroteri are not well understood. Vallis Schroteri, located on the Aristarchus Plateau, is the largest rille on the Moon, and it displays three key morphologic components: the Cobra Head, the 155-km-long primary rille, and the 240-km-long inner rille. Observations of terrestrial eruptions are applied here to help explain the morphologic relationships observed for Vallis Schroteri. The Cobra Head, a 10-km-wide source vent surrounded by a 35-km-diameter and 900-m-high low shield, might have been constructed from flows, spatter, and pyroclastic deposits erupted during lava fountain events, similar to the early stages of the vent at Pu'u 'O''o in Hawaii and the final morphology of Bandera crater, a cinder cone in New Mexico. The vent fed an initial sheet flow controlled by preeruption topography. A channel formed within this sheet flow was the foundation for the primary rille, which deepened through construction and thermomechanical erosion by lava. The inner rille is confined to the flat floor of the primary rille and is characterized by tight gooseneck meanders. This rille crosscuts the distal scarp of the primary rille and extends toward Oceanus Procellarum. This enigmatic relationship can be explained through backup, overflow, and diversion of the lava into a new rille that eroded into the margin of the primary rille. Similar backup, overflow, and redirection of the lava flow were observed during the 1984 Mauna Loa eruption in Hawaii. Analysis of the final morphology of lunar rilles provides key information about lunar volcanic processes and insight into the local stratigraphy. C1 [Garry, W. Brent] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Bleacher, Jacob E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Garry, WB (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. RI Bleacher, Jacob/D-1051-2012 OI Bleacher, Jacob/0000-0002-8499-4828 NR 76 TC 5 Z9 5 U1 2 U2 2 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2477-5 J9 GEOL SOC AM SPEC PAP PY 2011 VL 477 BP 77 EP 93 DI 10.1130/2011.2477(03) D2 10.1130/9780813724775 PG 17 WC Astronomy & Astrophysics; Geology SC Astronomy & Astrophysics; Geology GA BWN51 UT WOS:000294291300004 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI The Transits of Extrasolar Planets with Moons Introduction SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Editorial Material; Book Chapter ID SUN-LIKE STAR; BARNARDS STAR; SUPER-EARTH; BROWN DWARF; VB 10; COMPANION; FIELD; CANDIDATE; REFRACTOR; VIRGINIS C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu; dkipping@cfa.harvard.edu NR 50 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 1 EP 23 DI 10.1007/978-3-642-22269-6_1 D2 10.1007/978-3-642-22269-6 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000001 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI Extrasolar Moons SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Article; Book Chapter ID GIANT PLANETS; SOLAR-SYSTEM; SATELLITES; PULSAR; EXOPLANETS; ACCRETION; CAPTURE; ORIGIN C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu; dkipping@cfa.harvard.edu NR 32 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 25 EP 35 DI 10.1007/978-3-642-22269-6_2 D2 10.1007/978-3-642-22269-6 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000002 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI The Transiting Planet SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Article; Book Chapter ID EXTRASOLAR PLANETS; LIGHT CURVES; HD 189733B; STELLAR VARIABILITY; INFRARED-EMISSION; ORBITAL PERIOD; ATMOSPHERE; STARS; WATER; TIME C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu NR 47 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 37 EP 56 DI 10.1007/978-3-642-22269-6_3 D2 10.1007/978-3-642-22269-6 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000003 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI Timing the Transit SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Article; Book Chapter ID LIGHT-CURVE; EXTRASOLAR PLANETS; PERTURBATIONS; ECCENTRICITY; ORBIT; STAR C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu; dkipping@cfa.harvard.edu NR 28 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 57 EP 91 DI 10.1007/978-3-642-22269-6_4 D2 10.1007/978-3-642-22269-6 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000004 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI Transit Distortions SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Article; Book Chapter ID TIME-SERIES PHOTOMETRY; EXOPLANET HD 189733B; EXTRASOLAR PLANET; LIGHT-CURVE; TRANSMISSION SPECTRA; MODEL ATMOSPHERES; MU-M; WATER; PARAMETERS; 209458B C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu NR 48 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 93 EP 126 DI 10.1007/978-3-642-22269-6_5 D2 10.1007/978-3-642-22269-6 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000005 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI Transit Timing Effects Due to an Exomoon SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Article; Book Chapter ID COROT SPACE MISSION; LIGHT-CURVE PROJECT; EXTRASOLAR PLANETS; HOT-JUPITER; PERIOD VARIATIONS; ORBITAL PERIOD; EXOPLANETS; SATELLITES; SYSTEM C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu; dkipping@cfa.harvard.edu NR 32 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 127 EP 164 DI 10.1007/978-3-642-22269-6_6 D2 10.1007/978-3-642-22269-6 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000006 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI Detectability of Habitable Exomoons with Kepler-Class Photometry SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Article; Book Chapter ID EXTRASOLAR GIANT PLANETS; SATELLITES; MOONS C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu; dkipping@cfa.harvard.edu NR 24 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 165 EP 182 DI 10.1007/978-3-642-22269-6_7 D2 10.1007/978-3-642-22269-6 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000007 ER PT S AU Kipping, DM AF Kipping, David M. BA Kipping, DM BF Kipping, DM TI Conclusions and Future Work SO TRANSITS OF EXTRASOLAR PLANETS WITH MOONS SE Springer Theses-Recognizing Outstanding PhD Research LA English DT Editorial Material; Book Chapter ID PLANETS C1 Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Ctr Astrophys, Rm P-348,60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu; dkipping@cfa.harvard.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 2190-5053 BN 978-3-642-22268-9 J9 SPRINGER THESES-RECO PY 2011 BP 183 EP 189 DI 10.1007/978-3-642-22269-6_8 D2 10.1007/978-3-642-22269-6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWR91 UT WOS:000294694000008 ER PT B AU Piperno, DR AF Piperno, D. R. BE Bush, MB Flenley, JR Gosling, WD TI Prehistoric human occupation and impacts on Neotropical forest landscapes during the Late Pleistocene and Early/Middle Holocene SO TROPICAL RAINFOREST RESPONSES TO CLIMATE CHANGE, SECOND EDITION SE Springer-Praxis Books in Environmental Sciences LA English DT Article; Book Chapter ID MODERN POLLEN SPECTRA; BALSAS RIVER VALLEY; LOW ATMOSPHERIC CO2; RAIN-FOREST; AMAZON BASIN; NEW-GUINEA; PHYTOLITH EVIDENCE; BOLIVIAN AMAZON; TROPICAL FOREST; LATE QUATERNARY C1 [Piperno, D. R.] Smithsonian Trop Res Inst, Balboa, Panama. [Piperno, D. R.] Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM Pipernod@si.edu NR 116 TC 7 Z9 7 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-642-05382-5 J9 S-P B ENVIRON SCI PY 2011 BP 185 EP 212 D2 10.1007/978-3-642-05383-2 PG 28 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA BWN03 UT WOS:000294270600006 ER PT S AU Evans, NR AF Evans, Nancy Remage BE Neiner, C Wade, G Meynet, G Peters, G TI Multiplicity in 5 M-circle dot stars SO ACTIVE OB STARS: STRUCTURE, EVOLUTION, MASS-LOSS, AND CRITICAL LIMITS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 272nd Symposium of the International-Astronomical-Union on Active OB Stars: Structure, Evolution, Mass-Loss, and Critical Limits CY JUL 19-23, 2010 CL Paris, FRANCE SP Int Astronom Union, Region Ile France, CNRS, Inst Natl Sci Univ, Minist Enseignement Superieur & Rech, Programme Natl Phys Stellaire, GEPI Lab, Sci Council Paris Observ, A & A, EDP Sci DE binaries: general; stars: variables: Cepheids ID CARINAE AB Binary/multiple status can affect stars at all stages of their lifetimes: evolution onto the main sequence, properties on the main sequence, and subsequent evolution. 5 M-circle dot stars have provided a wealth of information about the binary properties fairly massive stars. The combination of cool evolved primaries and hot secondaries in Cepheids (geriatric B stars) have yielded detailed information about the distribution of mass ratios. and have also provided a surprisingly high fraction of triple systems. Ground-based radial velocity orbits combined with satellite data from Hubble, FUSE, IUE, and Chandra are needed to provide full information about the systems, including the masses. As a recent example, X-ray observations can identify low mass companions which are young enough to be physical companions. Typically binary status and properties (separation, eccentricity, mass ratio) determine whether any stage of evolution takes an exotic form. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 4, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu NR 7 TC 4 Z9 4 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-52119-840-0 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2011 VL 272 BP 537 EP 538 DI 10.1017/S1743921311011355 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWP46 UT WOS:000294438200145 ER PT S AU Fitzhugh, WW Herzog, A Perdikaris, S McLeod, B AF Fitzhugh, William W. Herzog, Anja Perdikaris, Sophia McLeod, Brenna BE Ford, B TI Ship to Shore: Inuit, Early Europeans, and Maritime Landscapes in the Northern Gulf of St. Lawrence SO ARCHAEOLOGY OF MARITIME LANDSCAPES SE When the Land Meets the Sea LA English DT Article; Book Chapter ID BOWHEAD WHALES; ATLANTIC C1 [Fitzhugh, William W.] Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA. [Herzog, Anja] Univ Laval, CELAT Dept Hist, Quebec City, PQ G1V 0A6, Canada. [McLeod, Brenna] Trent Univ, Nat Resource DNA Profiling & Forens Ctr NRDPFC, Peterborough, ON K9J 7B8, Canada. [Perdikaris, Sophia] CUNY, Dept Anthropol, New York, NY 10021 USA. RP Fitzhugh, WW (reprint author), Smithsonian Inst, Dept Anthropol, POB 37012, Washington, DC 20013 USA. EM Fitzhugh@si.edu OI McLeod, Brenna A./0000-0002-8535-1410 NR 78 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1869-6783 BN 978-1-4419-8209-4 J9 WHEN LAND MEETS SEA PY 2011 BP 99 EP 128 DI 10.1007/978-1-4419-8210-0_6 D2 10.1007/978-1-4419-8210-0 PG 30 WC Anthropology; Archaeology SC Anthropology; Archaeology GA BVI77 UT WOS:000291622200007 ER PT S AU Korzennik, SG Eff-Darwich, A AF Korzennik, S. G. Eff-Darwich, A. BE Appourchaux, T TI The rotation rate and its evolution derived from improved mode fitting and inversion methodology SO GONG-SOHO 24: A NEW ERA OF SEISMOLOGY OF THE SUN AND SOLAR-LIKE STARS SE Journal of Physics Conference Series LA English DT Proceedings Paper CT GONG2010-SoHO24 Conference on A New Era of Seismology of the Sun and Solar-Like Stars CY JUN 27-JUL 02, 2010 CL Aix-en-Province, FRANCE SP Univ Paris Sud, Ctr Natl Etudes Spatiales (CNES), Programme Natl Relations Soleil-Terre, Programme Natl Phys Stellaire, INSU Ctr Natl Rech Sci, SoHo Project European Space Agcy, Sci Programme ESA, Global Oscillat Network Grp, European Aeronaut Def Space Co, Inst Natl Sci Univers AB We present inferences of the internal solar rotation rate and its evolution during solar cycle 23. A full solar cycle of MDI observations have been analyzed using an improved fitting methodology and using time series of various lengths, up to a single 4,608 day long epoch (64 times 72 days or 12.6 yr). We used time series of spherical harmonic coefficients computed by the MDI group, including those resulting from using their improved spatial decomposition. This decomposition includes our best estimate of the image plate scale and of the MDI instrumental image distortion. The leakage matrix used in the fitting includes the effect of the distortion of the eigenfunctions by the solar differential rotation, while the undistorted leakage matrix was itself carefully reviewed and independently recomputed. Rotation inversions were carried out for all available mode sets, fitted for that epoch, including the MDI and GONG "pipe-line" values. The improved inversion method uses an iterative methodology based on a least-squares regularization, but with an optimal model grid determined by the actual information in the input set. This method also allows us to use an optimized irregular grid, with a variable number of latitudes at different depths. C1 [Korzennik, S. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM skorzennik@cfa.harvard.edu; adarwich@iac.es NR 8 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2011 VL 271 AR 012067 DI 10.1088/1742-6596/271/1/012067 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BWS76 UT WOS:000294742700067 ER PT B AU Ubelaker, DH AF Ubelaker, Douglas H. BE MarquezGrant, N Fibiger, L TI United States of America SO ROUTLEDGE HANDBOOK OF ARCHAEOLOGICAL HUMAN REMAINS LEGISLATION: AN INTERNATIONAL GUIDE TO LAWS AND PRACTICE IN THE EXCAVATION AND TREATMENT OF ARCHAEOLOGICAL HUMAN REMAINS LA English DT Article; Book Chapter ID HUMAN SKELETAL REMAINS; AGE ESTIMATION; DEATH; SAMPLE; CRANIA; RATIOS C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 45 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE PI LONDON PA 11 NEW FETTER LANE, LONDON EC4P 4EE, ENGLAND BN 978-0-203-83871-6; 978-0-415-58857-7 PY 2011 BP 533 EP 540 PG 8 WC Archaeology; Medicine, Legal SC Archaeology; Legal Medicine GA BUX50 UT WOS:000290612800049 ER PT S AU Ashton, MS Hall, JS AF Ashton, Mark S. Hall, Jefferson S. BE Gunter, S Weber, M Stimm, B Mosandl, R TI Review The Ecology, Silviculture, and Use of Tropical Wet Forests with Special Emphasis on Timber Rich Types SO SILVICULTURE IN THE TROPICS SE Tropical Forestry LA English DT Review; Book Chapter DE Amazon; Central Africa; Dipterocarps; Entandrophragma; Southeast Asia; Swietenia ID SIMULATED LIGHT ENVIRONMENTS; NEOTROPICAL RAIN-FOREST; SOUTHERN NEW-ENGLAND; REDUCED-IMPACT; TREE SEEDLINGS; LOGGING DAMAGE; DIPTEROCARP FORESTS; HARDWOOD STANDS; EAST KALIMANTAN; MORABALLI CREEK AB Tropical wet forests were once extensive throughout the high rainfall (>2,000 mm per year) areas of the equatorial latitudes between 23 N and 23 S. Most of the of the forest in Asia, West Africa, Central America, and northern Latin America is either degraded from logging or has been cleared for agriculture. However, extensive forest remains in Central Africa, Amazonia, and parts of Asia. This chapter is a review of the autecology and forest dynamics of the timber-rich forest types of these regions, with special attention to work done on the silviculture and sustainable management of such forests. New insights are provided into management particularly in integrating nontimber forest products with timber for higher economic values that are competitive compared to other land uses, and in providing a strong case for episodic regeneration methods and their variants based on recent studies of the ecology of the tree species and their forest dynamics. More sophisticated silvicultural methods need to be implemented if the remaining forests are to be sustainably managed for timber and nontimber products. It is clear that silvicultural research both on timber and on nontimber species is lacking, and what information there is, is concentrated on only a few species and in particular regions. What is now being realized is that these forests provide much more than wood and nonwood products. Such realized provisions now include: (1) water for downstream urban drinking supply, hydroelectricity, and for irrigated agriculture; (2) climate mitigation through action as a store house and sequestration site for carbon; and (3) as moderator of surface temperatures and variability in rainfall functions that have global consequences if these forests are destroyed. It is therefore in our own best interests to protect and sustainably manage them. C1 [Ashton, Mark S.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Hall, Jefferson S.] Smithsonian Trop Res Inst, Balboa, Panama. RP Ashton, MS (reprint author), Yale Univ, Sch Forestry & Environm Studies, 360 Prospect St, New Haven, CT 06511 USA. EM mark.ashton@yale.edu; hallje@si.edu NR 181 TC 1 Z9 1 U1 1 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1614-9785 BN 978-3-642-19985-1 J9 TROP FOREST JI Trop. For. PY 2011 BP 145 EP 192 DI 10.1007/978-3-642-19986-8_12 PG 48 WC Forestry SC Forestry GA BWE51 UT WOS:000293760700012 ER PT S AU Hall, JS AF Hall, Jefferson S. BE Gunter, S Weber, M Stimm, B Mosandl, R TI Natural Forest Silviculture for Central African Meliaceae SO SILVICULTURE IN THE TROPICS SE Tropical Forestry LA English DT Article; Book Chapter DE African mahoganies; Central Africa; Entandrophragma; Khaya; Logging; Management; Meliaceae; Timber harvest ID ENTANDROPHRAGMA SPECIES MELIACEAE; SEEDLING PERFORMANCE; MANAGEMENT; MAHOGANY; DISPERSAL; SPP. AB African Meliaceae have long been appreciated for their timber, with exports from coastal West Africa beginning over 100 years ago. Exploitation of African mahoganies of the genera Khaya and Entandrophragma has sustained much of the timber industry in Central Africa for several decades. Low levels of high-grade logging have led to the situation where Meliaceae still remain an important component of the timber harvest in the Central African subregion, particularly in more remote areas. Thus, the potential for natural forest silviculture where Meliaceae are targeted still exists. African Meliaceae are found in low densities within the subregion, with densities of between 0.5 and 2 individuals per hectare of exploitable individuals (more than 80-cm diameter at breast height, DBH) in unlogged forest being common. Typically there is an abundance of individuals within the 10-cm-DBH size class, with relatively few individuals in intermediate (20-70-cm-DBH) size classes. African mahoganies are classed as nonpioneer light demanders or species that can regenerate in the shade but need light to recruit to larger size classes. Seedlings can suffer high rates of mortality and many species distributions within the forest have been found to be related to microsite soil fertility. Because of these challenges, management of these species should be undertaken in association with management of nonpioneer light demander species from other genera and families where the exploitation intensity of mahoganies is reduced and volumes are replaced by a suite of timber species. Management for regeneration and recruitment of these species requires increasing understory light and liberating individuals belonging to the small and intermediate size classes. Highly selective logging will likely lead to long-term impoverishment of African mahogany populations where these species no longer play an important role in the timber industry. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Hall, JS (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM hallje@si.edu NR 25 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1614-9785 BN 978-3-642-19985-1 J9 TROP FOREST JI Trop. For. PY 2011 BP 215 EP 225 DI 10.1007/978-3-642-19986-8_14 PG 11 WC Forestry SC Forestry GA BWE51 UT WOS:000293760700014 ER PT S AU Boos, K Ashton, GV Cook, EJ AF Boos, Karin Ashton, Gail V. Cook, Elizabeth J. BE Galil, BS Clark, PF Carlton, JT TI The Japanese Skeleton Shrimp Caprella mutica (Crustacea, Amphipoda): A Global Invader of Coastal Waters SO IN THE WRONG PLACE - ALIEN MARINE CRUSTACEANS: DISTRIBUTION, BIOLOGY AND IMPACTS SE Invading Nature-Springer Series in Invasion Ecology LA English DT Article; Book Chapter DE Life history; Population dynamics; Interspecific interactions; Competition; Dispersal; Distribution; Vectors; Anthropogenic transport ID BIOLOGICAL INVASIONS; SEXUAL-DIMORPHISM; REPRODUCTIVE-BEHAVIOR; INTRAGUILD PREDATION; MARINE-ENVIRONMENT; SCAURA-TYPICA; WEST-COAST; COMMUNITIES; COMPETITION; MECHANISMS AB Successful invasion must be viewed as the result of a unique sequence of events, with the established species overcoming a number of previously prohibitive obstacles, for example lack of dispersal vectors, habitat characteristics and environmental conditions of the new area, and the ability to persist in interspecific interactions in the new community. The Japanese skeleton shrimp, Caprella mutica, is proving to be a highly successful non-native crustacean in coastal waters outside its native range having overcome these obstacles. In the past 40 years, C. mutica has spread from its native sub-boreal waters of north-east Asia to numerous locations in both the northern and southern hemisphere, where it has successfully established self-sustaining and thriving populations. After its first European record from the Netherlands in 1995, C. mutica spread rapidly within the North Sea and later to the west coast of Scotland and to Ireland in less than 15 years. Caprella mutica is generally associated with man-made structures and can be found in abundance on boat hulls, floating pontoons and aquaculture infrastructure clinging to fouling organisms. Species-specific traits which enable C. mutica to perform superiorly in its introduced ranges include: rapid growth, short maturation time, high reproductive activity, broad tolerance towards prevailing environmental conditions, omnivorous feeding behaviour and efficient dispersal and distribution. These traits provide excellent prerequisites for any species to colonise a variety of different microhabitats. The availability of suitable structures, however, is of paramount importance to the invasion success of C. mutica in European coastal waters and most likely elsewhere. On artificial structures directed away from the seabed, C. mutica is able to avoid benthic predation pressure and thus, to develop massive population densities. These high abundances in disturbed habitats may also reflect the species' ability to inhabit fluctuating systems better than other species. Caprella mutica was found to be competitively superior over native congeners and to show aggressive behaviour towards conspecifics. The characteristics described here are surely not unique to C. mutica and, therefore, cannot explain its success relative to other potential non-native species. They do, however, provide insight into why C. mutica has been so successful and consequently in determining whether another species may also be successful. When making these assessments, it is of particular importance to consider potential risks of the species and how important prevention or eradication may be. Although C. mutica can be assigned a potentially harmful invader, detailed knowledge on community or ecosystem level impacts are still lacking. Recommendations on management and control actions, therefore, remain insufficient. C1 [Boos, Karin] Alfred Wegener Inst Polar & Marine Res, Biol Anstalt Helgoland, Marine Stn, D-27483 Helgoland, Germany. [Ashton, Gail V.] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Cook, Elizabeth J.] Scottish Assoc Marine Sci, Scottish Marine Inst, Oban PA37 1QA, Argyll, Scotland. RP Boos, K (reprint author), Alfred Wegener Inst Polar & Marine Res, Biol Anstalt Helgoland, Marine Stn, POB 180, D-27483 Helgoland, Germany. EM Karin.Boos@awi.de NR 139 TC 5 Z9 5 U1 1 U2 17 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1874-7809 BN 978-94-007-0590-6 J9 INVAD NAT SPRING SER JI Invading Nat.-Springer Ser. Invasion Ecol. PY 2011 VL 6 BP 129 EP 156 DI 10.1007/978-94-007-0591-3_4 D2 10.1007/978-94-007-0591-3 PG 28 WC Ecology SC Environmental Sciences & Ecology GA BWJ05 UT WOS:000293984800004 ER PT S AU Ruiz, G Fofonoff, P Steves, B Dahlstrom, A AF Ruiz, Gregory Fofonoff, Paul Steves, Brian Dahlstrom, Alisha BE Galil, BS Clark, PF Carlton, JT TI Marine Crustacean Invasions in North America: A Synthesis of Historical Records and Documented Impacts SO IN THE WRONG PLACE - ALIEN MARINE CRUSTACEANS: DISTRIBUTION, BIOLOGY AND IMPACTS SE Invading Nature-Springer Series in Invasion Ecology LA English DT Article; Book Chapter ID SAN-FRANCISCO-BAY; RHIZOCEPHALAN LOXOTHYLACUS-PANOPAEI; CHINESE MITTEN CRAB; FOULING COMMUNITY; TROPHIC CASCADES; JOAQUIN ESTUARY; CARCINUS-MAENAS; STRIPED BASS; DELTA SMELT; GREEN CRAB AB We examine the history and relative importance of marine crustacean invasions for North America. Nearly 400 non-native species of invertebrates and algae have established populations in marine and estuarine waters of North America. Of these documented invasions, 28% are crustaceans, contributing the largest number of species of any taxonomic group. Crustaceans also dominate non-native species richness on each coast of North America, but there are strong differences in the total number of non-native species and in their taxonomic distribution among coasts. Crustaceans contribute prominently to the current knowledge base about marine invasions, due both to the large number (proportion) of documented introductions and also the extent of research on the group; they are thus a potentially important model for understanding marine biological invasions in general. Using an analysis of available literature, we evaluate what is known about the impacts of 108 non-native crustaceans in North America. Ecological and economic impacts are reported for many (28%) of these species, but they are rarely well documented, resulting in low certainty about the magnitude, spatial scale, and temporal scale of effects. C1 [Ruiz, Gregory; Fofonoff, Paul; Steves, Brian] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Dahlstrom, Alisha] Univ Tasmania, Launceston, Tas 7248, Australia. RP Ruiz, G (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM ruizg@si.edu NR 132 TC 8 Z9 8 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1874-7809 BN 978-94-007-0590-6 J9 INVAD NAT SPRING SER JI Invading Nat.-Springer Ser. Invasion Ecol. PY 2011 VL 6 BP 215 EP 250 DI 10.1007/978-94-007-0591-3_6 D2 10.1007/978-94-007-0591-3 PG 36 WC Ecology SC Environmental Sciences & Ecology GA BWJ05 UT WOS:000293984800006 ER PT B AU Fitzhugh, WW Bayarsaikhan, J AF Fitzhugh, William W. Bayarsaikhan, Jamsranjav BE Sabloff, PLW TI Mapping Ritual Landscapes in Bronze Age Mongolia and Beyond: Interpreting the Ideoscape of the Deer Stone-Khirigsuur Complex SO MAPPING MONGOLIA: SITUATING MONGOLIA IN THE WORLD FROM GEOLOGIC TIME TO THE PRESENT SE Penn Museum International Research Conferences LA English DT Proceedings Paper CT 3rd Conference on Mapping Mongolia - Situating Mongolia in the World from Geologic Time to the Present CY MAY 06-11, 2007 CL Univ Penn, Penn Museum, Philadelphia, PA SP Univ Penn HO Univ Penn, Penn Museum C1 [Fitzhugh, William W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Arctic Studies Ctr, Washington, DC 20560 USA. NR 49 TC 3 Z9 3 U1 0 U2 0 PU UNIV PENNSYLVANIA MUSEUM ARCHAEOLOGY & ANTHROPOLOGY PI PHILADELPHIA PA 3260 SOUTH STREET, PHILADELPHIA, PA 19104-6324 USA BN 978-1-934536-18-6 J9 PENN MUSEUM INT RES PY 2011 VL 2 BP 166 EP 192 PG 27 WC Anthropology; Archaeology SC Anthropology; Archaeology GA BWD24 UT WOS:000293607000009 ER PT J AU FitzHugh, EW Leona, M Shibayama, N AF FitzHugh, Elisabeth West Leona, Marco Shibayama, Nobuko TI Pigments in a Paint Box Belonging to Whistler in the Library of Congress SO STUDIES IN CONSERVATION LA English DT Article ID SURFACE-ENHANCED RAMAN; SCATTERING; DYES; ART AB A paint box and palette that belonged to the American painter James McNeill Whistler (1834-1903) are in the Library of Congress, Washington, DC. There are 37 tubes of paint in the box, including 6 in a separate cardboard box labeled Spectrum Colors. There are also painting and etching tools. The tubes were supplied by five British colormen, except for the Spectrum Colors, which came from the American firm if Devoe & Raynolds Inc. Sonic of the tube labels are missing or illegible. The pigments were identified using polarized light microscopy, X-ray powder diffraction, high performance liquid chromatography, and Raman spectroscopy. Information from Devoe & Raynold's catalogs suggests that the Spectrum Colors were not available before 1909; toluidine red found in one Spectrum Color; was first synthesized in 1904. Thus, the Spectrum Colors must have been put in the paint box after Whistler's death. Of the other pigments in the box, three graphite, emerald,green and synthetic malachite are not known to have been used by Inn,, but it may be that they are yet to be identified. The paint box was given to the Library if Congress by Joseph and Elizabeth Pennell in 1917, 14 years after the artist's death, and it is not known whether the paint box was used during that time. C1 [FitzHugh, Elisabeth West] Smithsonian Inst, Dept Conservat & Sci Res, Washington, DC 20560 USA. [Leona, Marco; Shibayama, Nobuko] Metropolitan Museum Art, Dept Sci Res, New York, NY 10028 USA. [Shibayama, Nobuko] Metropolitan Museum Art, HPLC Lab, New York, NY 10028 USA. RP FitzHugh, EW (reprint author), Smithsonian Inst, Dept Conservat & Sci Res, Washington, DC 20560 USA. EM r.fitzhugh@wap.org; marco.leona@metmuseum.org; nobuko.shibayama@metmuseum.org NR 31 TC 1 Z9 1 U1 0 U2 6 PU INT INST CONSERVATION HISTORIC ARTISTIC WORKS PI LONDON PA 6 BUCKINGHAM ST, LONDON WC2N 6BA, ENGLAND SN 0039-3630 J9 STUD CONSERV JI Stud. Conserv. PY 2011 VL 56 IS 2 BP 115 EP 124 PG 10 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA 806NM UT WOS:000293814900004 ER PT J AU Gedan, KB Altieri, AH Bertness, MD AF Gedan, Keryn B. Altieri, Andrew H. Bertness, Mark D. TI Uncertain future of New England salt marshes SO MARINE ECOLOGY PROGRESS SERIES LA English DT Review DE Climate change; Sea level rise; Salt marsh die-off; Eutrophication; Invasive species; Phragmites australis; Management ID SEA-LEVEL RISE; SOUTHERN NEW-ENGLAND; PHRAGMITES-AUSTRALIS; CONSUMER CONTROL; COMMON REED; ECOSYSTEM SERVICES; COASTAL WETLANDS; PLANT DIVERSITY; CHESAPEAKE BAY; TIDAL WETLAND AB Salt marsh plant communities have long been envisioned as dynamic, resilient systems that quickly recover from human impacts and natural disturbances. But are salt marshes sufficiently resilient to withstand the escalating intensity and scale of human impacts in coastal environments? In this study we examined the independent and interactive effects of emerging threats to New England salt marshes (temperature increase, accelerating eutrophication, consumer-driven salt marsh die-off, and sea level rise) to understand the future trajectory of these ecologically valuable ecosystems. While marsh plant communities remain resilient to many disturbances, loss of critical foundation species and changing tidal inundation regimes may short circuit marsh resilience in the future. Accelerating sea level rise and salt marsh die-off in particular may interact to overwhelm the compensatory mechanisms of marshes and increase their vulnerability to drowning. Management of marshes will require difficult decisions to balance ecosystem service tradeoffs and conservation goals, which, in light of the immediate threat of salt marsh loss, should focus on maintaining ecosystem resilience. C1 [Gedan, Keryn B.; Altieri, Andrew H.; Bertness, Mark D.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. RP Gedan, KB (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gedank@si.edu RI Gedan, Keryn/A-3575-2010 OI Gedan, Keryn/0000-0003-4020-5441 FU Marine Alliance for Science and Technology for Scotland (MASTS) Coastal Zone Joint Research Theme FX Open Access for the Theme Section on Coastal Zone Management is sponsored by the Marine Alliance for Science and Technology for Scotland (MASTS) Coastal Zone Joint Research Theme. NR 74 TC 27 Z9 27 U1 16 U2 104 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2011 VL 434 BP 229 EP 237 DI 10.3354/meps09084 PG 9 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 802TC UT WOS:000293532900019 ER PT B AU Steiger, M Charola, AE Sterflinger, K AF Steiger, Michael Charola, A. Elena Sterflinger, Katja BE Siegesmund, S Snethlage, R TI Weathering and Deterioration SO STONE IN ARCHITECTURE: PROPERTIES, DURABILITY, FOURTH EDITION LA English DT Article; Book Chapter ID POROUS MATERIALS; SODIUM-SULFATE; CRYSTALLIZATION PRESSURE; EXPERIMENTAL FROST; THERMAL-EXPANSION; CRYSTAL-GROWTH; AIR-POLLUTION; MARBLE DETERIORATION; CARBONATE STONE; CLAY-MINERALS AB It is generally assumed that stone is one of the most durable materials because it is compared to weaker building materials, such as wood or mud. But stone can deteriorate and many factors will affect it. The nature of the stone is critical in determining its resistance to the various deterioration factors. The most important one, salt, was already identified by Herodotus, nearly two and a half millennia ago. However, salt by itself is not damaging, it requires the presence of water for its aggressiveness to become evident. And water is needed for biocolonization to occur, for freeze-thaw phenomena and for wet-dry expansion. Control of this single factor can decrease significantly the deterioration potential of a stone and any structure built from it. The chapter aims to present a review of the most important deterioration processes and their effect on the various types of stones and rocks used by man. Among them are thermal effects, the influence of moisture, both as water vapor or in liquid state, the presence of salts and the damages that can be expected from biocolonization. The chapter also aims at identifying the areas where more research is needed to understand the actual deterioration mechanism of the various factors. C1 [Steiger, Michael] Univ Hamburg, Dept Chem Inorgan & Appl Chem, D-20146 Hamburg, Germany. [Charola, A. Elena] Smithsonian Inst, Museum Conservat Inst, Washington, DC 20560 USA. [Sterflinger, Katja] Univ Nat Resources & Appl Life Sci Vienna, Inst Appl Microbiol, A-1190 Vienna, Austria. RP Steiger, M (reprint author), Univ Hamburg, Dept Chem Inorgan & Appl Chem, Martin Luther King Pl 6, D-20146 Hamburg, Germany. EM michael.steiger@chemie.uni-hamburg.de; charola_ae@yahoo.com; katja.sterflinger@boku.ac.at RI Steiger, Michael/D-1241-2015 OI Steiger, Michael/0000-0002-7527-1097 NR 269 TC 28 Z9 28 U1 0 U2 7 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-642-14474-5 PY 2011 BP 227 EP 316 DI 10.1007/978-3-642-14475-2_4 D2 10.1007/978-3-642-14475-2 PG 90 WC Construction & Building Technology; Geosciences, Multidisciplinary SC Construction & Building Technology; Geology GA BTM64 UT WOS:000287334700004 ER PT B AU Miralles, MP Almeida, JS AF Miralles, Mari Paz Sanchez Almeida, Jorge BE Miralles, MP Almeida, JS TI The Sun, the Solar Wind, and the Heliosphere SO SUN, THE SOLAR WIND, AND THE HELIOSPHERE SE IAGA Special Sopron Book Series LA English DT Editorial Material; Book Chapter ID CORONAL HOLES; 0.3-AU; 1-AU AB We describe the aims and contents of the book entitled "The Sun, the Solar Wind, and the Heliosphere". This is a volume in the IAGA Special Book Series dedicated to the science covered by IAGA Division IV, Solar Wind and Interplanetary Field. The book features review articles on topics from the interior of the Sun to the outermost regions of the heliosphere. In addition, we highlight some of the results presented during the Division IV symposia at the 11th Scientific Assembly of IAGA in Sopron, Hungary, which was planned simultaneously with this book. C1 [Miralles, Mari Paz] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanchez Almeida, Jorge] Inst Astrofis Canarias, E-38205 Tenerife, Spain. RP Miralles, MP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmiralles@cfa.harvard.edu; jos@iac.es; mmiralles@cfa.harvard.edu; jos@iac.es NR 34 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-90-481-9786-6 J9 IAGA SPEC SOPRON PY 2011 VL 4 BP 3 EP 8 DI 10.1007/978-90-481-9787-3_1 D2 10.1007/978-90-481-9787-3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUN20 UT WOS:000289819000001 ER PT J AU Briceno, RD Eberhard, WG AF Briceno, R. D. Eberhard, W. G. TI The hub as a launching platform: rapid movements of the spider Leucauge mariana (Araneae: Tetragnathidae) as it turns to attack prey SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Leg movements; rapid orientation behavior; orb web design ID ORB-WEAVING SPIDERS; NEPHILA-CLAVIPES; ARANEIDAE; CAPTURE; WEB; DISCRIMINATION; VIBRATIONS AB Spiders are effectively blind with respect to the lines in their webs, and they commonly use exploratory leg movements to find lines, just as a blind man finds objects using a cane. Nevertheless, a mature female Leucauge mariana (Keyserling 1881), which spins a relatively open, sparsely-meshed hub and whose legs I and II hold widely-spaced radii rather than dense hub lines, turns precisely and rapidly when prey strike her orb. She can turn > 90 degrees, finding and grasping new lines with all her legs, in as little as 0.1 s and can reach a prey several body lengths away in as little as 0.23 s after impact. The hub design and resting postures of the spider's legs allow her to sense where the prey strikes the web, generate the force necessary to turn her body rapidly, and find lines to grasp. The spider may move most (if not all) of her legs, without obtaining further guidance information once the leg has begun to move until it nears the site where it will grasp a line. The order in which legs are moved is relatively consistent, and each tarsus moves to a site where lines are relatively abundant; some then make small, quick searching movements to find and grasp lines there. When radial lines were experimentally cut near the hub in a sector in which a prey was subsequently introduced, legs I and II first made small searching movements, and then executed much larger searching movements. The rapid leg movements directed toward specific areas where lines are abundant, and the small searching movements employed at these sites suggest that the spider modifies her behavior when she is at the hub of an orb. C1 [Briceno, R. D.; Eberhard, W. G.] Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Pedro, Costa Rica. RP Briceno, RD (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, Ciudad Univ, San Pedro, Costa Rica. EM rbriceno@biologia.ucr.ac.cr FU Smithsonian Tropical Research; Vicerrectoria of the Universidad de Costa Rica FX We thank Bernal Burgos for technical help, and the Smithsonian Tropical Research and the Vicerrectoria of the Universidad de Costa Rica for financial support. NR 20 TC 3 Z9 3 U1 0 U2 8 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2011 VL 39 IS 1 BP 102 EP 112 PG 11 WC Entomology SC Entomology GA 797FP UT WOS:000293110200010 ER PT J AU Galvez, D AF Galvez, Dumas TI Web decoration of Micrathena sexpinosa (Araneae: Araneidae): a frame-web-choice experiment with stingless bees SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Decorated; foraging; stabilimenta; undecorated ID PREY-ATTRACTION HYPOTHESIS; ORB-WEAVING SPIDER; SILK DECORATIONS; GASTERACANTHA-CANCRIFORMIS; OCTONOBA-SYBOTIDES; FORAGING BEHAVIOR; WAIT PREDATOR; STABILIMENTA; CAMOUFLAGE; SUCCESS AB The function of silk web decorations in orb weaving spiders has been debated for decades. The most accepted hypothesized functions are that web decorations I) provide camouflage against predators, 2) are an advertisement for vertebrates to avoid web damage, or 3) increase the attraction of prey to the web. Most studies have focused on only a few genera, Argiope being the most common. In this study, I evaluated the prey attraction hypothesis of silk decorations for a species of a poorly studied genus in this topic, Micrathena sexpinosa Hahn 1822. I used a web-choice experiment in which I presented empty or web-bearing frames at the end of a tunnel to stingless bees (Tetragonisca angustula). This frame-choice experiment consisted of the following comparisons: decorated web vs. empty frame, decorated web vs. undecorated web, and undecorated web vs. empty frame. Webs with decoration intercepted significantly more bees than empty frames and undecorated webs. Therefore, the decorations of Micrathena sexpinosa might play a role in increasing foraging success. C1 [Galvez, Dumas] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Galvez, D (reprint author), Univ Lausanne, Dept Ecol & Evolut, UNIL Sorge, CH-1005 Lausanne, Switzerland. EM dumas.galvez@unil.ch FU Organization for Tropical Studies FX I thank Carlos Garcia-Robledo, Orlando Vargas, Johel Chaves, Arietta Fleming-Davies, Claudia Lizana, and Mirjam Knornschild for help during the experiments; Aidan Vey for improving the English of the manuscript; David W. Roubik for his help with the identification of the bees; Erin Kurten, Sean J. Blamires, Andrew T. Sensenig, and Linden Higgins for their comments on the manuscript; and finally, I also thank the Organization for Tropical Studies that funded this study. NR 47 TC 2 Z9 2 U1 0 U2 19 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2011 VL 39 IS 1 BP 128 EP 132 PG 5 WC Entomology SC Entomology GA 797FP UT WOS:000293110200013 ER PT J AU Zotz, G Bader, MY AF Zotz, Gerhard Bader, Maaike Y. TI SAMPLING VASCULAR EPIPHYTE DIVERSITY - SPECIES RICHNESS AND COMMUNITY STRUCTURE SO ECOTROPICA LA English DT Article DE community structure; evenness; San Lorenzo crane site; patchiness; species coexistence; species-accumulation curves; species richness estimators; substrate preference ID BARRO COLORADO ISLAND; RAIN-FOREST; SPATIAL STRUCTURE; LOWLAND FOREST; TREE SIZE; PANAMA; HEMIEPIPHYTES; VEGETATION; VENEZUELA; PATTERNS AB The minimum requirement for the documentation of the structure of vascular epiphyte communities comprises information on the number of co-occurring species and their abundance and distribution. Using subsampling from a comprehensive census of the epiphytes on more than 1000 trees with a diameter at breast height > 1 cm in 0.4 ha of lowland rainforest in Panama as a reference, this study investigates the minimum sampling effort necessary to obtain reliable information on essential community attributes (species numbers, a-diversity, and evenness). Large trees host the majority of all vascular epiphytes and therefore only the largest trees were sampled. Comparing the resulting community attributes deduced from a sample of epiphytes on 1-12 of the largest trees with those of the entire 0.4-ha study plot indicates that a sample size of about 6-8 trees is already sufficient to obtain a representative description of this epiphyte community. Accepted 6 March 2011. C1 [Zotz, Gerhard; Bader, Maaike Y.] Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, POB 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de RI Bader, Maaike/M-7998-2013 OI Bader, Maaike/0000-0003-4300-7598 NR 47 TC 8 Z9 8 U1 3 U2 17 PU SOC TROPICAL ECOLOGY, GTOE, ZOOLOGICAL RESEARCH INST & MUSE PI BONN PA ADENAUERALLE 160, BONN, 00000, GERMANY SN 0949-3026 J9 ECOTROPICA JI Ecotropica PY 2011 VL 17 IS 1 BP 103 EP 112 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 795RJ UT WOS:000292993200009 ER PT J AU da Costa, RCL Lobato, AKD da Silveira, JAG Laughinghouse, HD AF Lobo da Costa, Roberto Cezar da Silva Lobato, Allan Klynger Gomes da Silveira, Joaquim Albenisio Laughinghouse, Haywood Dail TI ABA-mediated proline synthesis in cowpea leaves exposed to water deficiency and rehydration SO TURKISH JOURNAL OF AGRICULTURE AND FORESTRY LA English DT Article DE Abscisic acid; nitrogen metabolism; osmotic adjustment; rehydration; Vigna unguiculata L. (Walp.); water deficit ID BIOCHEMICAL RESPONSES; RICE LEAVES; GLUTAMINE-SYNTHETASE; USE EFFICIENCY; ABSCISIC-ACID; GAS-EXCHANGE; STRESS; ACCUMULATION; DROUGHT; PLANTS AB The aim of this study was (i) to evaluate the impact of water deficit and rehydration on nitrogen compounds and abscisic acid of Vigna unguiculata leaves, and (ii) to investigate the hypothesis that abscisic acid influences proline. The experimental design was entirely randomized in a factorial design, with 2 water conditions (control and stress) and 7 evaluation periods (0, 1, 2, 3, and 4 days under water deficit, followed by the 5th and 6th day under rehydration). The leaf relative water content presented significant reduction, presenting a lower value on the 4th day of treatment under water deficit. After rehydration, the plants reestablished the leaf relative water content. The correlation analysis suggested a significant relationship between the leaf relative water content and abscisic acid. The abscisic acid concentration of the plants under water deficiency were of 2.4, 45.9, 42.6, 47.9, 66.9, 9.2, and 5.5 mg kg(-1) DM on days 0, 1, 2, 3, 4, 5, and 6, respectively. Rehydration quickly decreased abscisic acid. In addition, the correlation analysis indicated a significant relationship between abscisic acid and proline. The proline levels of the plants under stress showed significant increases by 67%, 354%, 423%, and 532% on the 1st, 2nd, 3rd, and 4th day, respectively, when compared with control plants. This study with Vigna unguiculata plants reveals negative consequence of water deficiency over nitrogen metabolism, and fast recovery after rehydration. The nitrogen compounds and enzymes presented direct and indirect responses in the osmotic adjustment of the plant, as well as increasing abscisic acid concentration with the intent to decrease water loss in Vigna unguiculata induced by the water deficiency. Furthermore, a positive relationship between abscisic acid and proline synthesis was confirmed. C1 [da Silva Lobato, Allan Klynger] Univ Fed Rural Amazonia, Paragominas, Brazil. [Lobo da Costa, Roberto Cezar] Univ Fed Rural Amazonia, Lab Adv Plant Physiol, Belem, Para, Brazil. [Gomes da Silveira, Joaquim Albenisio] Univ Fed Ceara, Lab Metab & Stress Plant, Fortaleza, Ceara, Brazil. [Laughinghouse, Haywood Dail] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Lobato, AKD (reprint author), Univ Fed Rural Amazonia, Paragominas, Brazil. EM allanllobato@yahoo.com.br RI Laughinghouse, Haywood/M-5836-2016 OI Laughinghouse, Haywood/0000-0003-1018-6948 FU Conselho Nacional de Pesquisa (CNPq/Brazil); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES/Brazil) FX This research had financial support from Conselho Nacional de Pesquisa (CNPq/Brazil) for R.C.L. Costa and J.A.G. Silveira and from Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES/Brazil) for A.K.S. Lobato. The manuscript was reviewed by H.D. Laughinghouse IV. NR 45 TC 3 Z9 4 U1 1 U2 13 PU TUBITAK SCIENTIFIC & TECHNICAL RESEARCH COUNCIL TURKEY PI ANKARA PA ATATURK BULVARI NO 221, KAVAKLIDERE, ANKARA, 00000, TURKEY SN 1300-011X J9 TURK J AGRIC FOR JI Turk. J. Agric. For. PY 2011 VL 35 IS 3 BP 309 EP 317 DI 10.3906/tar-0911-409 PG 9 WC Agriculture, Multidisciplinary; Agronomy; Forestry SC Agriculture; Forestry GA 794MC UT WOS:000292900300010 ER PT J AU Labandeir, CC AF Labandeir, Conrad C. TI EVIDENCE FOR AN EARLIEST LATE CARBONIFEROUS DIVERGENCE TIME AND THE EARLY LARVAL ECOLOGY AND DIVERSIFICATION OF MAJOR HOLOMETABOLA LINEAGES SO ENTOMOLOGICA AMERICANA LA English DT Article ID HYMENOPTERA INSECTA; SENSITIVITY-ANALYSIS; PHYLOGENY; ORIGIN; ENDOPTERYGOTA; DIVERSITY; HISTORY; ORDERS; BASE; USA AB Four fossil taxa of earliest Holometabola recently were identified based on a variety of determinative evidence and assigned to a stem-group or a basal lineage within a modern order. One consequence of these new discoveries is that the divergence date between the Holometabola and its sister clade has been set earlier than previously thought on the basis of fossils or molecular phylogenetic evidence. This new date provides a minimal calibration date pegged to the Early Carboniferous-Late Carboniferous boundary, and approximates an absolute date of 318 million years. The four taxa provide new insights into the life habits, particularly feeding habits, of early holometabolan larvae. Additionally, they require an explanation of why there is an 80 million year lag between the origin and the taxonomic dominance of this profound developmental innovation in early terrestrial ecosystems. An earlier lead time is likely present for these earliest holometabolan fossils, which can be extrapolated conservatively to the Late Mississippian, 328 to 318 million years ago. Consequently, a focused investigation on earlier, Late Mississippian strata to search for ancestral holometabolan insects is imperative. C1 [Labandeir, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeir, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeir, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. RP Labandeir, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM labandce@si.edu NR 74 TC 14 Z9 14 U1 0 U2 5 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 1947-5136 EI 1947-5144 J9 ENTOMOL AM-NY JI Entomol. Am. PY 2011 VL 117 IS 1-2 BP 9 EP 21 PG 13 WC Entomology SC Entomology GA 790IC UT WOS:000292580700002 ER PT S AU Winter, FH AF Winter, Frank H. BE Liepack, OG TI On the "Spaghetti" Trail: The Story of a Revolution in Modern Rocket Technology SO HISTORY OF ROCKETRY AND ASTRONAUTICS SE AAS History Series LA English DT Proceedings Paper CT 37th International-Academy-of-Astronautics History Symposium CY SEP 29-OCT 03, 2003 CL Bremen, GERMANY C1 [Winter, Frank H.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 58 TC 1 Z9 1 U1 0 U2 0 PU AMER ASTRONAUTICAL SOC PI SAN DIEGO PA PUBLICATIONS OFFICE PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0730-3564 BN 978-0-87703-564-0 J9 AAS HIST SER PY 2011 VL 34 BP 293 EP 340 PG 48 WC Engineering, Aerospace; Astronomy & Astrophysics; History; History & Philosophy Of Science SC Engineering; Astronomy & Astrophysics; History; History & Philosophy of Science GA BVS00 UT WOS:000292619100016 ER PT J AU Larjavaara, M Muller-Landau, HC AF Larjavaara, Markku Muller-Landau, Helene C. TI Cross-Section Mass: An Improved Basis for Woody Debris Necromass Inventory SO SILVA FENNICA LA English DT Editorial Material DE biomass; coarse woody debris (CWD); deadwood; log; void space; nominal volume and wood density; carbon in woody detritus ID LINE-INTERSECT; FORESTS; BIOMASS; CARBON C1 [Larjavaara, Markku; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA. [Larjavaara, Markku] Univ Helsinki, Dept Forest Sci, FIN-00014 Helsinki, Finland. RP Larjavaara, M (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, Dpo, AA 34002 USA. EM larjavaaram@si.edu OI Larjavaara, Markku/0000-0002-3484-889X NR 19 TC 2 Z9 2 U1 0 U2 8 PU FINNISH SOC FOREST SCIENCE-NATURAL RESOURCES INST FINLAND PI VANTAA PA PO BOX 18, FI-01301 VANTAA, FINLAND SN 0037-5330 EI 2242-4075 J9 SILVA FENN JI Silva. Fenn. PY 2011 VL 45 IS 2 BP 291 EP 298 AR 119 DI 10.14214/sf.119 PG 8 WC Forestry SC Forestry GA 790JX UT WOS:000292585400010 ER PT B AU Christy, JH Rittschof, D AF Christy, John H. Rittschof, Dan BE Breithaupt, T Thiel, M TI Deception in Visual and Chemical Communication in Crustaceans SO CHEMICAL COMMUNICATION IN CRUSTACEANS LA English DT Article; Book Chapter ID RHYNCHOCINETES-TYPUS DECAPODA; CRAB CALLINECTES-SAPIDUS; FIDDLER-CRAB; CARCINUS-MAENAS; INDIVIDUAL RECOGNITION; SIGNAL RESIDUALS; SEX-PHEROMONE; MACROBRACHIUM-ROSENBERGII; REPRODUCTIVE-BEHAVIOR; AGONISTIC ENCOUNTERS AB Deception in animal communication occurs when one animal causes another to respond to a condition that does not exist or to fail to respond to one that does Signals that bluff produce the first kind of error behavior that hides causes the second and both are common in visual communication by crustaceans In contrast crustacean chemical communication may usually be honest because the communicative chemicals typically are byproducts of the biochemical mechanisms by which crustaceans are built and operate These cues which often are released in urine reliably reveal an individual s identity sex reproductive state and condition There are however opportunities for deception by bluffing and by hiding in the chemical channel Bluffing may occur when dominance relationships are learned and individuals recognize each other Subordinates may avoid known dominants even after the condition of the dominant has declined and it is no longer able to win a fight with the subordinate Frequent probing by subordinates should check such bluffing Hiding in the chemical channel may occur in escalated fights in which one animal fails to chemically announce Its Intent to strike and wins by delivering a blind side punch to an unprepared opponent Receptive female crabs and lobsters may also withhold cues of their receptivity to avoid courtship by some males yet direct the same cues to preferred potential mates In species with multiple male morphs we speculate that subordinate males may hide from dominants by with holding male odors or mimicking female odors In species with Internal fertilization we also suggest that male seminal fluids may contain chemicals that affect female reproductive processes and bias the rate the male s sperm fertilize the female s eggs Detecting deception in chemical communication will be very challenging but we encourage crustacean researchers to keep this possibility in mind when examining signaling behavior via chemicals C1 [Christy, John H.] Smithsonian Trop Res Inst, Balboa, Panama. [Rittschof, Dan] Duke Univ, Marine Lab, Beaufort, NC 28516 USA. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 68 TC 11 Z9 11 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-0-387-77100-7 PY 2011 BP 313 EP 333 DI 10.1007/978-0-387-77101-4_16 D2 10.1007/978-0-387-77101-4 PG 21 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA BSQ57 UT WOS:000285482400016 ER PT B AU Fong, P Paul, VJ AF Fong, Peggy Paul, Valerie J. BE Dubinsky, Z Stambler, N TI Coral Reef Algae SO CORAL REEFS: AN ECOSYSTEM IN TRANSITION LA English DT Article; Book Chapter DE Macroalgae; cyanobacteria; chemical defenses; nutrients; herbivory; climate change; invasive species; diversity; coral/algal competition ID GREAT-BARRIER-REEF; MACROALGA DICTYOSPHAERIA-CAVERNOSA; CYANOBACTERIUM-LYNGBYA-MAJUSCULA; MACROCYSTIS-PYRIFERA PHAEOPHYTA; PLANT-HERBIVORE INTERACTIONS; ALTERNATIVE STABLE STATES; TRANSIENT AMMONIUM UPTAKE; FUNCTIONAL-GROUP APPROACH; NUTRIENT-LIMITED GROWTH; INTESTINALIS L. LINK AB Benthic macroalgae, or "seaweeds," are key members of coral reef communities that provide vital ecological functions such as stabilization of reef structure, production of tropical sands, nutrient retention and recycling, primary production, and trophic support. Macroalgae of an astonishing range of diversity, abundance, and morphological form provide these equally diverse ecological functions. Marine macroalgae are a functional rather than phylogenetic group comprised of members from two Kingdoms and at least four major Phyla. Structurally, coral reef macroalgae range from simple chains of prokaryotic cells to upright vine-like rockweeds with complex internal structures analogous to vascular plants. There is abundant evidence that the historical state of coral reef algal communities was dominance by encrusting and turf-forming macroalgae, yet over the last few decades upright and more fleshy macroalgae have proliferated across all areas and zones of reefs with increasing frequency and abundance. Ecological processes that sustain these shifts from coral- to algal-dominated tropical reefs include increases in open suitable substrate due to coral mortality, anthropogenic increases in nutrient supply, reductions in herbivory due to disease and overfishing, and the proliferation of algae with chemical defenses against herbivory. These shifts are likely to be accelerated and the algal state stabilized by the impacts of invasive species and climate change. Thus, algal-dominated tropical reefs may represent alternative stable states that are resistant to shifts back to coral domination due to the strength and persistence of ecological processes that stabilize the algal state. C1 [Fong, Peggy] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Fong, P (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Young Dr S, Los Angeles, CA 90095 USA. EM pfong@biology.ucla.edu; Paul@si.edu NR 328 TC 41 Z9 45 U1 2 U2 26 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-94-007-0113-7 PY 2011 BP 241 EP 272 DI 10.1007/978-94-007-0114-4_17 D2 10.1007/978-94-007-0114-4 PG 32 WC Biodiversity Conservation; Marine & Freshwater Biology SC Biodiversity & Conservation; Marine & Freshwater Biology GA BSW81 UT WOS:000285982500017 ER PT B AU Warrit, N Lekprayoon, C AF Warrit, Natapot Lekprayoon, Chariya BE Hepburn, HR Radloff, SE TI Asian Honeybee Mites SO HONEYBEES OF ASIA LA English DT Article; Book Chapter ID VARROA-JACOBSONI OUD; APIS-MELLIFERA COLONIES; LINKED-IMMUNOSORBENT-ASSAY; EUVARROA-SINHAI DELFINADO; ACARAPIS-WOODI RENNIE; DNA SEQUENCE DATA; TROPILAELAPS-CLAREAE; BEES HYMENOPTERA; TRACHEAL MITES; PARASITIC MITE C1 [Warrit, Natapot] Chulalongkorn Univ, Fac Sci, Dept Biol, Ctr Excellence Entomol, Bangkok 10330, Thailand. [Warrit, Natapot] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Lekprayoon, Chariya] Chulalongkorn Univ, Fac Sci, Dept Biol, Ctr Excellence Biodivers, Bangkok 10330, Thailand. RP Warrit, N (reprint author), Chulalongkorn Univ, Fac Sci, Dept Biol, Ctr Excellence Entomol, Bangkok 10330, Thailand. EM Natapot.w@chula.ac.th; Chariya.l@chula.ac.th NR 141 TC 6 Z9 6 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-642-16421-7 PY 2011 BP 347 EP 368 DI 10.1007/978-3-642-16422-4_16 D2 10.1007/978-3-642-16422-4 PG 22 WC Entomology SC Entomology GA BTF70 UT WOS:000286842400016 ER PT S AU Hendy, AJW AF Hendy, Austin J. W. BE Allison, PA Bottjer, DJ TI Taphonomic Overprints on Phanerozoic Trends in Biodiversity: Lithification and Other Secular Megabiases SO TAPHONOMY: PROCESS AND BIAS THROUGH TIME, SECOND EDITION SE Topics in Geobiology LA English DT Article; Book Chapter ID CRETACEOUS-TERTIARY BOUNDARY; FOSSIL RECORD; ORGANIC PRESERVATION; GLOBAL DIVERSITY; LARGE-SCALE; SAMPLING-STANDARDIZATION; ARAGONITE DISSOLUTION; MARINE BIODIVERSITY; ALPHA-DIVERSITY; LATE MIOCENE AB Taphonomic biases introduce heterogeneity into the quality of the fossil record and can skew paleontologists' perception of biodiversity. This paper reviews the temporal extent and consequences of major taphonomic biases, including lithification of sediments, skeletal replacement through silicification and phosphatization, concentration of skeletal hard-parts, and the exceptional preservation of soft-bodied faunas. The frequency of occurrence of particular biases, and their effects of fossil faunas is identified using occurrence-based datasets, such as the Paleobiology Database. Lithification of most Paleozoic and Mesozoic fossiliferous sediments has likely had a significant influence on perceptions of within-community diversity and paleoecological composition. The increased availability of unlithified sediments in rocks of late Mesozoic through Cenozoic age coincides with a two- to threefold increase in local diversity, a discrepancy that remains even after employing sampling-standardization techniques. Taxa that possess small body size and aragonitic skeletal mineralogy are preferentially lost or obscured following the cementation of host sediments. Additionally, morphological details are often obscured or not preserved in specimens obtained from lithified sediments, suggesting that taphonomic damage could hinder taxonomic practice and estimates of diversity at the global-scale. Silica replacement, which generally enhances diversity among groups composed of less stable skeletal composition, appears most frequently among Permian fossil assemblages. Phosphatic replacement, which plays a key role in the preservation of soft-bodied and small-shelly faunas, appears commonly in assemblages of Cambrian age. Konservat-lagerstatten, while providing a rich source of information on the rarely preserved soft-bodied biota, are infrequent in the fossil record, but perhaps are most notable in rocks of Cambrian age. Shell beds are well known as sources of tremendous diversity and although they are not easily defined these beds appear to increase in frequency in middle Paleozoic and Cenozoic age successions. Fossil molds, unlike previously mentioned biases, suggest lost diversity, and are most frequent in rocks of early Cambrian and early Mesozoic age. The non-random nature of the above biases raises concerns regarding the comparison of diversity or ecological complexity over the course of the Phanerozoic or between contemporaneous faunal groups. Furthermore, a number of the biases have tremendous potential to affect community-scale patterns, either degrading (e.g., lithification, aragonite dissolution) or enhancing (e.g., silicification, phosphatization) the relative quality of fossil data. A number of approaches can be undertaken to minimize these biases, including the selective filtering of datasets to remove taphonomically vulnerable groups or the use of taphonomic control taxa that indicate the appropriate preservation state of fossil assemblages. C1 [Hendy, Austin J. W.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Panama City, Panama. [Hendy, Austin J. W.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06510 USA. RP Hendy, AJW (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Panama City, Panama. EM hendyaj@si.edu RI Hendy, Austin/C-1279-2013 OI Hendy, Austin/0000-0002-9818-1158 NR 148 TC 12 Z9 12 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0275-0120 BN 978-90-481-8642-6 J9 TOP GEOBIOL JI Top. Geobiol. PY 2011 VL 32 BP 19 EP 77 DI 10.1007/978-90-481-8643-3_2 D2 10.1007/978-90-481-8643-3 PG 59 WC Biology; Paleontology SC Life Sciences & Biomedicine - Other Topics; Paleontology GA BSI03 UT WOS:000284505600002 ER PT S AU Brett, CE Allison, PA Hendy, AJW AF Brett, Carlton E. Allison, Peter A. Hendy, Austin J. W. BE Allison, PA Bottjer, DJ TI Comparative Taphonomy and Sedimentology of Small-Scale Mixed Carbonate/Siliciclastic Cycles: Synopsis of Phanerozoic Examples SO TAPHONOMY: PROCESS AND BIAS THROUGH TIME, SECOND EDITION SE Topics in Geobiology LA English DT Article; Book Chapter ID SEQUENCE STRATIGRAPHIC SIGNIFICANCE; SILURIAN MARINE COMMUNITIES; FAUNAL GRADIENT ANALYSIS; MIDDLE CAMBRIAN WHEELER; WESTERN UNITED-STATES; NEW-YORK-STATE; UPPER ORDOVICIAN; NEW-ZEALAND; SHELL CONCENTRATIONS; BOOK-CLIFFS AB Small scale cycles deposited over 10-100 kyr are a common component of Phanerozoic shelfal deposits. A combination of detailed outcrop analysis and data-mining from published literature of cycles largely deposited in greenhouse regimes reveals a series of recurring sedimentological, paleoecological, and taphonomic motifs. In general, each cycle is composed of three to four components: (a) a basal skeleton-rich bed with evidence of condensation and, in some cases mineralization; (b) a medium-dark gray siliciclastic mudstone/shale interval; (c) a calcareous and/or silty mudstone interval with common concretionary, diagenetic overprint. A series of exemplars are highlighted from proximal and distal shelf settings and described using a depositional sequence approach. The cycles studied include examples deposited under greenhouse (Cambrian, Ordovician, Devonian, Jurassic and Cretaceous) and, for comparison purposes, icehouse (Neogene) conditions. The fact that repetitive patterns can characterize deposits that formed over a 500 million year interval is striking. The primary taphonomic moderator in these cycles is rate of sedimentation, which varies exponentially from sediment-starved concentrations to obrutionary deposits. The occurrence of a persistent motif over this time scale suggests that biological innovations, which might be expected to impact upon fossil preservation, have in fact been overprinted by the extremes of sedimentation preserved in these small-scale cycles. Having a skeleton, which is twice as resistant to abrasion, is of little import when sedimentation is dominated by the extremes: instant obrution or condensation. C1 [Brett, Carlton E.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Allison, Peter A.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. [Hendy, Austin J. W.] Smithsonian Trop Res Inst, Ctr Trop Palaeoecol & Archaeol, Panama City, FL USA. RP Brett, CE (reprint author), Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. EM C.Brett@uc.edu; P.A.Allison@imperial.ac.uk; hendyaj@si.edu RI Hendy, Austin/C-1279-2013 OI Hendy, Austin/0000-0002-9818-1158 NR 228 TC 5 Z9 6 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0275-0120 BN 978-90-481-8642-6 J9 TOP GEOBIOL JI Top. Geobiol. PY 2011 VL 32 BP 107 EP 198 DI 10.1007/978-90-481-8643-3_4 D2 10.1007/978-90-481-8643-3 PG 92 WC Biology; Paleontology SC Life Sciences & Biomedicine - Other Topics; Paleontology GA BSI03 UT WOS:000284505600004 ER PT J AU Medeiros, MJ Gillespie, RG AF Medeiros, Matthew J. Gillespie, Rosemary G. TI Biogeography and the evolution of flightlessness in a radiation of Hawaiian moths (Xyloryctidae: Thyrocopa) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Dispersal; flightless insects; Gelechioidea; island evolution; Kahoolawe; Necker; Nihoa; Northwestern Hawaiian Islands; phylogeny ID ADAPTIVE RADIATION; PHYLOGENETIC-RELATIONSHIPS; GENUS THYROCOPA; MIXED MODELS; LEPIDOPTERA; DIVERSIFICATION; MITOCHONDRIAL; ISLANDS; COLEOPTERA; INFERENCE AB Aim Although the ability to fly confers benefits to most insects, some taxa have become secondarily flightless. Insect flightlessness may be more likely to evolve in environments such as islands and other windswept and alpine areas, but this prediction has rarely been tested while controlling for phylogenetic effects. Here we present a phylogeny for the endemic Hawaiian Lepidoptera genus Thyrocopa, which has two flightless species that occur in alpine areas on Maui and Hawaii islands, in order to determine whether the flightless species are sister to each other or represent separate losses of flight. We also explore divergence times and biogeographic patterns of inter-island colonization in Thyrocopa, and present the first Hawaiian study to sample a genus from nine islands. Location The Hawaiian Islands. Methods The phylogeny is composed of 70 individuals (including 23 Thyrocopa species and 7 outgroup species) sequenced for portions of cytochrome c oxidase subunit I, elongation factor 1 alpha and wingless genes, for a total of 1964 base pairs, and was estimated using both parsimony (paup*) and Bayesian inference (MrBayes). Divergence times were estimated using the beast software package. Results Our results indicate that two independent invasions of alpine habitats with concomitant loss of flight have occurred in Thyrocopa. Based on current taxon sampling, Thyrocopa colonized the Hawaiian Islands slightly before the formation of Kauai. In terms of overall patterns of diversification, subclades generally follow a progression from older to younger islands. The genus has the greatest number of species on Kauai, with species numbers generally decreasing with decreasing island age. Main conclusions Loss of flight ability has evolved twice in a short period of geological time in Thyrocopa, perhaps as a result of low temperatures, high winds and/or a lack of predation pressure. However, several other Thyrocopa species that live on small islands with consistently high winds, such as Necker and Nihoa islands, retain the ability to fly. C1 [Medeiros, Matthew J.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Gillespie, Rosemary G.] Univ Calif Berkeley, Dept Environm Biol, Berkeley, CA 94720 USA. RP Medeiros, MJ (reprint author), Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. EM matt.j.medeiros@gmail.com FU University of California, Berkeley; Department of Integrative Biology; UC Museum of Paleontology; NSF; Schlinger Foundation; Margaret C. Walker Fund FX We thank three anonymous referees for comments that greatly improved the manuscript, and Jordana Anderson, Sam Aruch, Sara Backowski, Randy Bartlett, Gordon Bennett, Jeremy Dresel, Robert Dudley, Betsy Gagne, Jon Giffin, the Evolab at UC Berkeley, Will Haines, Ryan Hill, Frank Howarth, Kevin Jenkins, Raina Kaholoa'a, Adam Leache, David Medeiros, Andrew Mitchell, Shepherd Myers, Steve Montgomery, Marko Mutanen, Pete Oboyski, Patrick O'Grady, Kevin Padian, Bonnie Ploger, Jerry Powell, Kari Roesch Goodman, Klaus Sattler, Sean Schoville, Wayne Souza, Kevin Tuck, Liz Wang, the Molokai TNC, the staff at Kokee State Park, and the Kahoolawe Island Reserve Commission for help with collecting, logistics and advice. This research was supported in part by the University of California, Berkeley, Department of Integrative Biology, UC Museum of Paleontology, the NSF GK-12 Exploring California Biodiversity grant, the Schlinger Foundation, and the Margaret C. Walker Fund for teaching and research in systematic entomology. The work presented here represents a portion of M.J.M.'s PhD dissertation research at the University of California, Berkeley. NR 67 TC 10 Z9 10 U1 4 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD JAN PY 2011 VL 38 IS 1 BP 101 EP 111 DI 10.1111/j.1365-2699.2010.02402.x PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 694LU UT WOS:000285300500010 ER PT J AU Brown, ME Crosier, A Lynch, W Converse, SJ Chandler, J Olsen, G French, J Wildt, DE Songsasen, N AF Brown, M. E. Crosier, A. Lynch, W. Converse, S. J. Chandler, J. Olsen, G. French, J. Wildt, D. E. Songsasen, N. TI SEMINAL QUALITY IN WHOOPING CRANE (GRUS AMERICANA) IS AFFECTED BY STAGE OF BREEDING SEASON BUT NOT BY AGE OF INDIVIDUAL SO REPRODUCTION FERTILITY AND DEVELOPMENT LA English DT Meeting Abstract C1 [Brown, M. E.; Crosier, A.; Lynch, W.; Wildt, D. E.; Songsasen, N.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Converse, S. J.; Chandler, J.; Olsen, G.; French, J.] US Fish & Wildlife Serv, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. NR 0 TC 0 Z9 0 U1 0 U2 6 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1031-3613 J9 REPROD FERT DEVELOP JI Reprod. Fertil. Dev. PY 2011 VL 23 IS 1 MA 231 BP 214 EP 214 PG 1 WC Developmental Biology; Reproductive Biology; Zoology SC Developmental Biology; Reproductive Biology; Zoology GA 690MF UT WOS:000285008200241 ER PT J AU Tennakoon, KU Chak, WH Bolin, JF AF Tennakoon, Kushan U. Chak, Wang H. Bolin, Jay F. TI Nutritional and isotopic relationships of selected Bornean tropical mistletoe-host associations in Brunei Darussalam SO FUNCTIONAL PLANT BIOLOGY LA English DT Article DE Dendrophthoe; Macrosolen; mineral nutrition; mistletoe-host interactions; Scurrula; delta(13)C; delta(15)N ID XYLEM-TAPPING MISTLETOES; TAPINANTHUS-OLEIFOLIUS; ANGIOSPERM PARASITES; MINERAL NUTRIENTS; WATER RELATIONS; GAS-EXCHANGE; CARBON; NITROGEN; HETEROTROPHY; RATIOS AB Our understanding of mineral nutrition and carbon heterotrophy in mistletoes is derived largely from arid and temperate plant communities. Sharp differences between the tropical, temperate and arid communities, such as seasonality, water availability and mean temperature may influence basic assumptions regarding mistletoe physiology. Thus, we present mineral nutrition profiles and natural abundance carbon and nitrogen stable isotope data for tropical mistletoes and their hosts. Parasite-host mineral nutrition profiles were estimated for three Loranthaceous mistletoes: Scurrula ferruginea Danser, Macrosolen cochinchinensis Blume, and Dendrophthoe curvata Blume and 12 unique mistletoe-host associations. delta(13)C and delta(15)N values were estimated for 12 parasite-host associations. Differences between host and parasite delta(13)C values were small but showed significant depletion in mistletoe leaves compared with the distal branch and proximal branch host leaves. Host and mistletoe delta(13)C values were uncorrelated whereas delta(15)N values were significantly correlated, demonstrating mistletoe N dependence. Concentrations of K were higher in mistletoes relative to hosts and significantly higher for Dendrophthoe host associations. For Scurrula and Macrosolen, mean mistletoe-host concentrations of major and minor elements did not differ significantly. C1 [Tennakoon, Kushan U.; Chak, Wang H.] Univ Brunei Darussalam, Fac Sci, Biol Program, BE-1410 Gadong, Brunei. [Bolin, Jay F.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Tennakoon, KU (reprint author), Univ Brunei Darussalam, Fac Sci, Biol Program, BE-1410 Gadong, Brunei. EM kushan.tennakoon@ubd.edu.bn FU Funding for this study was provided by the National Development Plan, Brunei Darussalam [8a] FX Funding for this study was provided by the National Development Plan, Brunei Darussalam (UBO Science and Technology Research Grant No. 8). Logistic and laboratory facilities provided by the Faculty of Science, University of Brunei Darussalam and the Soil and Plant Nutrition Division of Brunei Agriculture Department (Hjh. Suria binti Zanuddin and Dr. H. M. Thippeswamy) are gratefully acknowledged. Thanks are extended to Christine France at the Smithsonian Institution OUSS/MCI Stable Isotope Mass Spectrometry Laboratory for stable isotope analyses and the Smithsonian Institution, NMNH Botany Department for logistical support. We thank the Forest Department of Brunei Darussalam for granting permission to conduct plant sample collections. NR 48 TC 9 Z9 9 U1 2 U2 10 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-4408 J9 FUNCT PLANT BIOL JI Funct. Plant Biol. PY 2011 VL 38 IS 6 BP 505 EP 513 DI 10.1071/FP10211 PG 9 WC Plant Sciences SC Plant Sciences GA 772DL UT WOS:000291212100006 ER PT J AU Lovelock, CE Feller, IC Adame, MF Reef, R Penrose, HM Wei, LL Ball, MC AF Lovelock, Catherine E. Feller, Ilka C. Adame, Maria Fernanda Reef, Ruth Penrose, Helen M. Wei, Lili Ball, Marilyn C. TI Intense storms and the delivery of materials that relieve nutrient limitations in mangroves of an arid zone estuary SO FUNCTIONAL PLANT BIOLOGY LA English DT Article DE Avicennia marina; Cyclone Pancho; Exmouth Gulf; Giralia Bay; nitrogen; phosphate; resorption efficiency; Western Australia; delta N-15 ID VS. PHOSPHORUS LIMITATION; WATER-USE EFFICIENCY; RHIZOPHORA-MANGLE L; WESTERN-AUSTRALIA; EXMOUTH GULF; NITROGEN; HURRICANE; GROWTH; ECOSYSTEMS; PATTERNS AB Tropical cyclones can be devastating to ecosystems, but they can also result in pulses of fresh water and sediments delivered in floodwaters to the coastal zone. In the arid zone the pulses provided by cyclones may be particularly important for the maintenance of productivity. We examined the impacts of Cyclone Pancho on growth and nutrient limitations to growth in mangroves on the arid coast of Western Australia. We found that growth of trees was enhanced after the cyclone, more than doubling their rates of stem extension. Fertilisation studies showed that before the cyclone tree growth was nutrient limited. After the cyclone fertilisation treatments had no significant effect on growth, indicating nutrients had been delivered during the storm. Additionally, before the cyclone the efficiency of resorption of phosphorus and nitrogen from senescent leaves was higher than after the cyclone, suggesting that nutrient availability was enhanced. Analysis of stable isotopes of leaf tissue indicated that the cyclone was associated with small changes in water use efficiency, consistent with decreased soil salinity associated with the cyclone. There was, however, significant reductions in delta N-15 indicating enhanced N supply potentially from a new source. We conclude that in the arid zone, floodwater associated with cyclones is important for the delivery of nutrient subsidies that stimulate mangrove growth and that predicted future reductions in the frequency of cyclones will have negative impacts on the productivity of these ecosystems. C1 [Lovelock, Catherine E.; Adame, Maria Fernanda; Reef, Ruth; Penrose, Helen M.; Wei, Lili] Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. [Feller, Ilka C.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ball, Marilyn C.] Australian Natl Univ, Res Sch Biol, Div Plant Sci, Canberra, ACT 0200, Australia. RP Lovelock, CE (reprint author), Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. EM c.lovelock@uq.edu.au RI Ball, Marilyn/D-1180-2009; Adame, Maria Fernanda/N-8463-2014; Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU ARC [LP0561498, DP0774491]; National Centre of Excellence for Groundwater Research and Training FX This work was supported by ARC awards LP0561498 and DP0774491 and by the National Centre of Excellence for Groundwater Research and Training. We thank Jennifer and Denver Blake at Giralia Station, Jack Egerton, Nadia Santini and Nele Schmitz for their support and generosity. NR 46 TC 16 Z9 16 U1 1 U2 26 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-4408 EI 1445-4416 J9 FUNCT PLANT BIOL JI Funct. Plant Biol. PY 2011 VL 38 IS 6 BP 514 EP 522 DI 10.1071/FP11027 PG 9 WC Plant Sciences SC Plant Sciences GA 772DL UT WOS:000291212100007 ER PT J AU Shackleford, B AF Shackleford, Ben TI NASCAR Stock Car Racing: Establishment and Southern Retrenchment SO INTERNATIONAL JOURNAL OF THE HISTORY OF SPORT LA English DT Article DE NASCAR; Stock car; Southern Culture; American Automobile Association (AAA); USAC; Daytona; violence; Professional sport; Piedmont; textile mill AB Stock Car racing within the United States emerged as a national phenomenon fostered by two main competing organizations, the National Association for Stock Car Automobile Racing (NASCAR) and the Competition Board of the American Automobile Association (AAA). As initial success waned, the stock car format found revitalization where the violence and danger of the sport resonated with growing idealization of the traditional Southern culture. C1 [Shackleford, Ben] Georgia Tech, Ctr Ind Modern S, Atlanta, GA USA. [Shackleford, Ben] Smithsonian Inst, Lemelson Ctr Study Innovat, Washington, DC 20560 USA. EM Ben.A.Shackleford@irs.gov NR 18 TC 2 Z9 2 U1 1 U2 2 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0952-3367 J9 INT J HIST SPORT JI Int. J. Hist. Sport PY 2011 VL 28 IS 2 SI SI BP 300 EP 318 DI 10.1080/09523367.2011.537922 PG 19 WC History; Hospitality, Leisure, Sport & Tourism SC History; Social Sciences - Other Topics GA 761QK UT WOS:000290412500008 ER PT J AU de Rivera, CE Grosholz, ED Ruiz, GM AF de Rivera, Catherine E. Grosholz, Edwin D. Ruiz, Gregory M. TI Multiple and long-term effects of an introduced predatory crab SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Invasion effect; Nonindigenous species; Carcinus maenas; Demographic response; Long-term effects; Body size; Intertidal distribution; Hemigrapsus oregonensis ID SAN-FRANCISCO BAY; CARCINUS-MAENAS; BIOLOGICAL INVASIONS; DUNGENESS CRAB; CANCER-MAGISTER; SHORE CRABS; ESTUARINE INVERTEBRATES; CALLINECTES-SAPIDUS; INTERTIDAL HABITAT; SPECIES INVASIONS AB Despite the importance of invasions, few studies have explored their long-term consequences in marine systems or examined multiple types of population-level effects. Initial effects, however, may not persist over longer time frames; effects have been shown to wane in freshwater systems. We combined 14 yr of field surveys (1993 to 2006) with manipulative experiments to examine the potential for multiple effects of a nonindigenous crab Carcinus maenas on the native shore crab Hemigrapsus oregonensis over time in central California. H. oregonensis abundance was negatively correlated with C. maenas abundance. However, H. oregonensis abundance rebounded to pre-invasion levels once C. maenas numbers declined. Other measured changes include a marked decrease in H. oregonensis body size and an increase in the proportion of H. oregonensis in the high intertidal zone since the arrival of C. maenas. These changes in body size and tidal distribution persisted nearly a decade beyond the peak abundance of C. maenas and after H. oregonensis numbers rebounded. Observed changes in the distribution of the H. oregonensis population correspond to shifts in C. maenas abundance, and experiments support a causal relationship. Stepwise regression suggests a complex and possibly nonlinear relationship between predictor variables and H. oregonensis size and distribution. Overall, our data indicate strong persistent effects on multiple attributes, with a lag in recovery with declining invader abundance, underscoring the potential for long-term effects that are decoupled from year-to-year invasion dynamics. C1 [de Rivera, Catherine E.] Portland State Univ, Portland, OR 97207 USA. [de Rivera, Catherine E.; Grosholz, Edwin D.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [de Rivera, Catherine E.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP de Rivera, CE (reprint author), Portland State Univ, POB 751, Portland, OR 97207 USA. EM derivera@pdx.edu OI Ruiz, Gregory/0000-0003-2499-441X FU National Science Foundation; Sea Grant/NOAA Partnership Program; California Sea Grant; Pacific States Marine Fisheries Commission FX We thank B. Agius, C. Dean, R. Estelle, C. Juhasz, N. Rayl, L. Rodriguez, K. Shirley, C. Sorte, R. Tinsman, and B. Williams for their hours of help in the field and laboratory. The field work was conducted at the Bodega Marine Reserve. We also acknowledge grants from the National Science Foundation (E.D.G., G.M.R.), Sea Grant/NOAA Partnership Program (E.D.G.), California Sea Grant (E.D.G.), and the Pacific States Marine Fisheries Commission (C.E.D., E.D.G., and G.M.R.). NR 69 TC 3 Z9 3 U1 0 U2 45 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2011 VL 429 BP 145 EP U757 DI 10.3354/meps09101 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 765CX UT WOS:000290682100013 ER PT S AU Desert, JM Charbonneau, D Madhusudhan, N Fortney, J Fressin, F Knutson, H Deming, D AF Desert, J. M. Charbonneau, D. Madhusudhan, N. Fortney, J. Fressin, F. Knutson, H. Deming, D. CA Kepler Team BE Bouchy, F Diaz, R Moutou, C TI Observations of Hot-Jupiter occultations combining Spitzer and Kepler photometry SO DETECTION AND DYNAMICS OF TRANSITING EXOPLANETS SE EPJ Web of Conferences LA English DT Proceedings Paper CT International Conference on Transiting Planets - Detection and Dynamics CY AUG 23-27, 2010 CL FRANCE ID TRANSITING PLANET AB We present the status of an ongoing program which aim at measuring occultations by their parent stars of transiting hot giant exoplanets discovered recently by Kepler. The observations are obtained in the near infrared with Warm S pitzer Space Telescope and at optical wavelengths by combining more than a year of Kepler photometry. The investigation consists of measuring the mid-occultation times and the relative occultation depths in each band-passes. Our measurements of occultations depths in the Kepler bandpass is turned into the determination of the optical geometric albedo A(g) in this wavelength domain. The brightness temperatures of these planets are deduced from the infrared observations. We combine the optical and near infrared planetary emergent fluxes to obtain broad band emergent spectra of individual planet. We finally compare these spectra to hot Jupiter atmospheric models in order broadly distinguishing these atmospheres between different classes of models. C1 [Desert, J. M.; Charbonneau, D.; Fressin, F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Madhusudhan, N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 05844 USA. [Fortney, J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Knutson, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Deming, D.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdesert@cfa.harvard.edu NR 10 TC 0 Z9 0 U1 0 U2 1 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X J9 EPJ WEB CONF PY 2011 VL 11 AR UNSP 03007 DI 10.1051/epjconf/20111103007 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUU70 UT WOS:000290390000023 ER PT J AU Mawdsley, JR Harrison, JD Sithole, H Mawdsley, JL AF Mawdsley, Jonathan R. Harrison, James du G. Sithole, Hendrik Mawdsley, James L. TI Landscape-scale surveys reveal patterns of floral visitation by species of Scarabaeidae (Coleoptera) in the Kruger National Park, South Africa SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Cetoniinae; Scarabaeidae; pollination; insect-plant relationships; African savannah ID ACACIA-NIGRESCENS AB Insect visitors were sampled from flowers of nine sympatric tree and shrub species in the Kruger National Park, South Africa, using a landscape-scale survey approach. Two species of Terminalia L., Terminalia prunioides Lawson and Terminalia sericea Burchell (Combretaceae) together comprised 53% of the flowering trees and shrubs sampled. Scarab beetles (Coleoptera: Scarabaeidae) comprised a majority of visitors to flowers of the two Terminalia species (90% and 88%, respectively). Statistical comparisons indicate that both the composition and abundance of scarab floral visitors differ between T. prunioides and T. sericea, and between these species and sympatric flowering tree and shrub species. Individual species of Scarabaeidae show markedly different patterns of abundance: 42% were found on flowers of one tree species, 45% were found on flowers of two or three tree species, and the remaining four scarab species were common and occurred on four or more of the tree species sampled. C1 [Mawdsley, Jonathan R.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. [Harrison, James du G.] Transvaal Museum, Dept Invertebrates Coleoptera Collect, Ditsong Natl Museum Nat Hist, ZA-0001 Pretoria, South Africa. [Sithole, Hendrik] Kruger Natl Pk, ZA-1350 Skukuza, South Africa. [Mawdsley, James L.] Stark State Coll, N Canton, OH 44720 USA. RP Mawdsley, JR (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, MRC 187,POB 37012, Washington, DC 20013 USA. EM mawdsley@heinzctr.org NR 23 TC 5 Z9 5 U1 0 U2 5 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2011 VL 45 IS 21-22 BP 1257 EP 1273 DI 10.1080/00222933.2011.552806 PG 17 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 758ZK UT WOS:000290207700001 ER PT J AU Flint, OS Kjer, KM AF Flint, Oliver S., Jr. Kjer, Karl M. TI A NEW SPECIES OF NEOPHYLAX FROM NORTHERN VIRGINIA, USA (TRICHOPTERA: UENOIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE caddisfly; COI; barcodes; description; distribution ID DNA; CADDISFLIES AB A new species of Neophylax, Neophylax virginica Flint, is described from several sites along the Potomac, Shenandoah and Rappahannock Rivers in Northern Virginia. It is closely related to Neophylax stolus Ross, Neophylax acutus Vinyard and Wiggins, Neophylax ayanus Ross, and Neophylax ottawa Vineyard and Wiggins, differing in characteristics of the male and female genitalia, which are illustrated. A phylogram of the Neophylax ayanus species group based on COI data is included. C1 [Flint, Oliver S., Jr.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Kjer, Karl M.] Rutgers State Univ, Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08901 USA. RP Flint, OS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. EM flinto@si.edu; kjer@aesop.rutgers.edu FU NSF [DEB 0816865] FX We acknowledge the wholehearted cooperation of Brent W. Steury, E. Oberg, J. Olson, and various other George Washington parkway personnel for supporting and funding the survey of various insect groups in the West Section, including Great Falls Park, of the George Washington Parkway National Park. Thanks to Xin Zhou and the staff at the Biodiversity Institute of Ontario for producing the molecular data, and to Paul Hebert and Genome Canada for funding the barcoding efforts. Karl M. Kjer acknowledges NSF DEB 0816865 for financial support. John K. Moulton of the University of Tennessee very graciously donated examples of the new species from the Rappahannock River. Thanks to Christy Jo Geraci, Jason Robinson, and Ralph Holzenthal for providing specimens for barcoding. Thanks also to three reviewers for their helpful comments on the manuscript. NR 12 TC 3 Z9 3 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2011 VL 113 IS 1 BP 7 EP 13 DI 10.4289/0013-8797.113.1.7 PG 7 WC Entomology SC Entomology GA 755JF UT WOS:000289925100002 ER PT J AU Smith, DR Altenhofer, E AF Smith, David R. Altenhofer, Ewald TI A NEW ELM LEAFMINING SAWFLY (HYMENOPTERA: TENTHREDINIDAE) FROM RUSSIA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Heterarthrinae; Fenusini; introduced species ID TRIBE FENUSINI AB Fenusa absens, n. sp., is described from Novosibirsk, Russia. It was reared from leaf mines in Siberian elm, Ulmus pumila L. Placement of this species in Fenusa Leach is discussed, and comparison is made to other species of elm leaf-mining sawflies. Because Ulmus pumila is not native to the Novosibirsk region, it is possible that Fenusa absens is an introduced species in the area. C1 [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov; ewald.altenhofer@aon.at NR 17 TC 3 Z9 3 U1 0 U2 7 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2011 VL 113 IS 1 BP 50 EP 56 DI 10.4289/0013-8797.113.1.50 PG 7 WC Entomology SC Entomology GA 755JF UT WOS:000289925100006 ER PT J AU Smith, DR Altenhofer, E AF Smith, David R. Altenhofer, Ewald TI THE SECOND RECORD OF A SAWFLY LEAFMINER ON ROSA, A NEW SPECIES OF FENUSA (HYMENOPTERA: TENTHREDINIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Russia; Fenusini AB Fenusa ewaldi Smith, n. sp., is described from Novosibirsk, Russia. The larvae are leafminers of Rosa sp. (Rosaceae) and represent only the second sawfly leafminer of this plant genus. C1 [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov; ewald.altenhofer@aon.at NR 10 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2011 VL 113 IS 1 BP 57 EP 60 DI 10.4289/0013-8797.113.1.57 PG 4 WC Entomology SC Entomology GA 755JF UT WOS:000289925100007 ER PT S AU Juric, M Ivezic, Z AF Juric, M. Ivezic, Z. BE Turon, C Meynadier, F Arenou, F TI SDSS, LSST AND GAIA: LESSONS AND SYNERGIES SO GAIA: AT THE FRONTIERS OF ASTROMETRY SE EAS Publications Series LA English DT Proceedings Paper CT Symposium on Gaia at the Frontiers of Astrometry CY JUN 07-11, 2010 CL Sevres, FRANCE SP Observatoire Paris, ESA, CNES ID MILKY-WAY TOMOGRAPHY; DIGITAL SKY SURVEY; DATA RELEASE; SAGITTARIUS; GALAXY; HALO AB The advent of deep, wide, accurate, digital photometric surveys exemplified by the Sloan Digital Sky Survey (SDSS) has had a profound impact on studies of the Milky Way. In the past decade, we have transitioned from a scarcity to an (over)abundance of precise, well calibrated, observations of stars over a large fraction of the Galaxy. The avalanche of data will continue throughout this decade, culminating with Gaia and LSST. This new reality will necessitate changes in methodology, habits, and expectations both on the side of the large survey projects as well as the astrophysics community at large. We argue, based on the experience with SDSS, that surveys should release data as early and often as possible incorporating incremental improvements in each subsequent release, as opposed to holding off for a single, big, final release. The scientific community will need to reciprocate by performing analyses and (re-analyses) appropriate to the current fidelity of the released data, understanding that these are continually evolving and improving products. C1 [Juric, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivezic, Z.] Univ Washington, Seattle, WA 98105 USA. [Ivezic, Z.] Univ Zagreb, Zagreb CRO-10000, Croatia. RP Juric, M (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 18 TC 4 Z9 4 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 978-2-7598-0608-9 J9 EAS PUBLICATIONS PY 2011 VL 45 BP 281 EP + DI 10.1051/eas/1045047 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUG58 UT WOS:000289226200047 ER PT J AU Galvez, D AF Galvez, Dumas TI Digestibility of palm seeds and bruchids larvae by Neotropical rodents SO ANIMAL BIOLOGY LA English DT Article DE Energy assimilation; larva; rodents; palm seeds ID ATTALEA-BUTYRACEA; FRUITS; DISPERSAL; PREDATION; FOREST; BEETLE; ACORNS; COLEOPTERA; SQUIRRELS; DECISIONS AB Vertebrates show different tendencies in regard to their preference for seeds or fruits infested by insects compared to non-infested ones. Behaviour may include rejection of one type, preferential consumption of one type or no differentiation among them. When comparing infested versus non-infested fruits, most studies have focused on energy content and nutritional components of the food items; but the energy input provided to the consumer is a better measure for the comparison of the value of each type of food. In this study, I calculated the energy assimilated by rodents for the seeds of the palm Attalea butyracea contained in non-infested endocarps and from bruchid beetle larvae contained in infested endocarps. Using the energy assimilation and time of handling by rodents for both types of endocarps, I quantitatively demonstrated that both infested and non-infested endocarps produce a similar energy input. This finding is consistent with the previous hypothesis that there is a trade-off between the energy content and the time required to extract the insect larvae compared with the seeds in endocarps of Attalea butyracea. (C) Koninklijke Brill NV, Leiden, 2011. C1 [Galvez, Dumas] Smithsonian Trop Res Inst, Panama City, Panama. [Galvez, Dumas] Univ Lausanne, Dept Ecol & Evolut, UNIL Sorge, CH-1005 Lausanne, Switzerland. RP Galvez, D (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM dumas.galvez@unil.ch FU Smithsonian Tropical Research Institute FX I thank Yhamir Galvez, Patrick A. Jansen, Mirna Samaniego, Segundo Vasquez and Joe Wright. The Smithsonian Tropical Research Institute (STRI), the Summit Botanical Garden, the Autoridad Nacional del Ambiente (ANAM), and the University of Panama for permissions and facilities. I thank Jessica Purcell and Kathryn Hine for comments and improving the English of the manuscript. This study was funded by the Smithsonian Tropical Research Institute (Alan Smith Fellowship). NR 32 TC 1 Z9 1 U1 0 U2 8 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 1570-7555 EI 1570-7563 J9 ANIM BIOL JI Anim. Biol. PY 2011 VL 61 IS 1 BP 21 EP 27 DI 10.1163/157075511X554392 PG 7 WC Zoology SC Zoology GA 747OM UT WOS:000289329300002 ER PT J AU Taylor, RC Klein, BA Ryan, MJ AF Taylor, Ryan C. Klein, Barrett A. Ryan, Michael J. TI Inter-signal interaction and uncertain information in anuran multimodal signals SO CURRENT ZOOLOGY LA English DT Article DE Inter-signal interaction; Multimodal signaling; Signal detection; Signal weighting; Squirrel treefrog; Hyla squirella; Tungara frog; Physalaemus pustulosus; Vocal sac ID FROG PHYSALAEMUS-PUSTULOSUS; COURTSHIP DISPLAY; TUNGARA FROGS; ACOUSTIC INTERFERENCE; ANIMAL COMMUNICATION; CONVERGENT EVOLUTION; LEG ORNAMENTATION; HYLA-SQUIRELLA; MATE CHOICE; VOCAL SAC AB Disentangling the influence of multiple signal components on receivers and elucidating general processes influencing complex signal evolution are difficult tasks. In this study we test mate preferences of female squirrel treefrogs Hyla squirella and female tungara frogs Physalaemus pustulosus for similar combinations of acoustic and visual components of their multimodal courtship signals. In a two-choice playback experiment with squirrel treefrogs, the visual stimulus of a male model significantly increased the attractivness of a relatively unattractive slow call rate. A previous study demonstrated that faster call rates are more attractive to female squirrel treefrogs, and all else being equal, models of male frogs with large body stripes are more attractive. In a similar experiment with female tungara frogs, the visual stimulus of a robotic frog failed to increase the attractiveness of a relatively unattractive call. Females also showed no preference for the distinct stripe on the robot that males commonly bear on their throat. Thus, features of conspicuous signal components such as body stripes are not universally important and signal function is likely to differ even among species with similar ecologies and communication systems. Finally, we discuss the putative information content of anuran signals and suggest that the categorization of redundant versus multiple messages may not be sufficient as a general explanation for the evolution of multimodal signaling. Instead of relying on untested assumptions concerning the information content of signals, we discuss the value of initially collecting comparative empirical data sets related to receiver responses [Current Zoology 57 (2): 153-161, 2011]. C1 [Taylor, Ryan C.] Salisbury Univ, Dept Biol Sci, Salisbury, MD 21801 USA. [Klein, Barrett A.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Taylor, RC (reprint author), Salisbury Univ, Dept Biol Sci, Salisbury, MD 21801 USA. EM rctaylor@salisbury.edu FU NSF [IBN-981654]; IBN [0517328]; University of Louisiana [2003-8717-90]; University of Texas [4031701] FX We thank Eileen Hebets for the invitation to participate in this volume on complex signaling. We are grateful to Bryant Buchanan and Carl Gerhardt for recording, analyzing and synthesizing squirrel treefrog vocalizations. Bryant Buchanan sculpted and painted squirrel treefrog models. Joey Stein and Moey Inc. fabricated the electro-mechanical controller units that powered the tungara robofrog inflation/deflation cycles. Christina Martin, Lisa Guy, and Jessie Doherty provided help with data collection. John Christy, Eileen Hebets, Christina Martin, and one anonymous reviewer provided valuable comments on later versions of this manuscript. Funding for squirrel treefrog experiments was provided by Sigma Xi GIAR to RCT. Funding for tungara frog experiments was provided by NSF Grants IBN-981654 to D. Cannatella, MJR, and W. Wilczynski, and IBN 0517328 to MJR and RCT. This research complied with all requirements of the animal care and use protocols of the University of Louisiana (protocol # 2003-8717-90, squirrel treefrogs) and the University of Texas (protocol # 4031701, tungara frogs). RCT was formerly affiliated with the University of Louisiana, Lafayette. All necessary permits and permissions were obtained from the Smithsonian Tropical Research Institute and government of Panama. NR 58 TC 13 Z9 13 U1 1 U2 27 PU CURRENT ZOOLOGY PI BEIJING PA CHINESE ACAD SCIENCES, INST ZOOLOGY, BEICHEN XILU, CHAOYANG DISTRICT, BEIJING, 100101, PEOPLES R CHINA SN 1674-5507 J9 CURR ZOOL JI Curr. Zool. PY 2011 VL 57 IS 2 BP 153 EP 161 PG 9 WC Zoology SC Zoology GA 741FG UT WOS:000288848200004 ER PT J AU Nelson, JM AF Nelson, Joan M. TI SOCIAL POLICY REFORMS IN LATIN AMERICA Urgent but Frustrating SO LATIN AMERICAN RESEARCH REVIEW LA English DT Review C1 Smithsonian Inst, Woodrow Wilson Int Ctr Scholars, Washington, DC 20560 USA. RP Nelson, JM (reprint author), Smithsonian Inst, Woodrow Wilson Int Ctr Scholars, Washington, DC 20560 USA. NR 11 TC 1 Z9 1 U1 1 U2 2 PU LATIN AMER STUDIES ASSOC PI PITTSBURGH PA 416 BELLEFIELD HALL, UNIV PITTSBURGH, PITTSBURGH, PA 15260 USA SN 0023-8791 J9 LAT AM RES REV JI Lat. Am. Res. Rev. PY 2011 VL 46 IS 1 BP 226 EP 239 PG 14 WC Area Studies SC Area Studies GA 729VM UT WOS:000287979600012 ER PT J AU Gomez, MI Strong, EE Glaubrecht, M AF Gomez, Maria I. Strong, Ellen E. Glaubrecht, Matthias TI REDESCRIPTION AND ANATOMY OF THE VIVIPAROUS FRESHWATER GASTROPOD HEMISINUS LINEOLATUS (W. WOOD, 1828) FROM JAMAICA (CERITHIOIDEA, THIARIDAE) SO MALACOLOGIA LA English DT Article DE morphology; systematics; Paludomidae; brood pouch; Greater Antilles; Neotropics ID LAKE TANGANYIKA; EAST-AFRICA; CAENOGASTROPODA; PALUDOMIDAE; MOLLUSCA; BIOGEOGRAPHY; PULMONATA; OVOVIVIPARITY; POPULATIONS; MORPHOLOGY AB The West Indies, well known for its distinctive geological history, is well suited for studies in biogeography and biodiversity. However, the lack of comprehensive studies for much of its unique fauna has hampered insights into their systematics, evolution and phylogeography. The scarcity of data is particularly pronounced for freshwater gastropods in the viviparous family Thiaridae-represented in the archipelago by Hemisinus Swainson, 1840 and Cubaedomus Morrison, 1951. Hitherto described only on the basis of shell morphology, we here redescribe Hemisinus lineolatus (W. Wood, 1828), the type species of Hemisinus, based on type material and museum collections. The anatomy of this species is also described, representing the first such comprehensive study of any Neotropical thiarid. The synonymy of Hemisinus buccinoides Reeve, 1860, with H. lineolatus is confirmed. The species is found to possess a mixture of distinctly thiarid features (e.g., operculum, rachidian, midgut, brood pouch) and features previously undocumented in the family (e.g., gonochorism with equal sex ratios, glandular pallial oviduct with spermatophore bursa in lateral lamina, spermatophore organ, statoconia). Some of these features (e.g., statoconia, spermatophore organ) are also found in members of the apparent sister group to the Thiaridae - the African-Asian freshwater Paludomidae. Consequently, the combination of features in Hemisinus is consistent with a basal position in the family. C1 [Gomez, Maria I.; Glaubrecht, Matthias] Humboldt Univ, Museum Nat Kunde, Leibniz Inst Res Evolut & Biodivers, D-10115 Berlin, Germany. [Strong, Ellen E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Gomez, MI (reprint author), Humboldt Univ, Museum Nat Kunde, Leibniz Inst Res Evolut & Biodivers, Invalidenstr 43, D-10115 Berlin, Germany. EM gomez.berning@googlemail.com OI Strong, Ellen/0000-0001-7181-4114 FU DAAD (Deutscher Akademischer Austausch Dienst) FX We would like to thank J. Ablett (BMNH), A. J. Baldinger (MCZ), P. Greenhall (USNM), and G. Rosenberg (ANSP) for the loan of material and their help with some literature. We are grateful to C. Schubart, who supplied us with samples from Jamaica and to A. Fender for providing ecological information. MIG thanks the Smith-sonian Institution for a Graduate Student Fellowship allowing her visit 2007 to the National Museum of Natural History. MIG also thanks V. Anaya and B. Berning for their comments on previous versions of this manuscript. MIG work was supported by a DAAD (Deutscher Akademischer Austausch Dienst) fellowship for doctoral studies, conducted from 2005 to 2009 at the Humboldt University of Berlin, which is gratefully acknowledged. NR 89 TC 6 Z9 7 U1 0 U2 3 PU INST MALACOL PI ANN ARBOR PA 2415 SOUTH CIRCLE DR, ANN ARBOR, MI 48103 USA SN 0076-2997 EI 2168-9075 J9 MALACOLOGIA JI Malacologia PY 2011 VL 53 IS 2 BP 229 EP 250 PG 22 WC Zoology SC Zoology GA 736BZ UT WOS:000288465900003 ER PT J AU Ubelaker, DH Rife, JL AF Ubelaker, D. H. Rife, J. L. TI Skeletal Analysis and Mortuary Practice in an Early Roman Chamber Tomb at Kenchreai, Greece SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE Kenchreai; Greece; Early Roman; chamber tomb; formation processes; looting; mortuary practice; cremation ID CEMETERY AB Recent exploration of the site of Kenchreai, the eastern port of Corinth in southern Greece, has focussed on a cemetery of subterranean chamber tombs dating chiefly to the Early Roman period (middle-late 1st to 3rd centuries AD). The copious but fragmentary human bones and teeth found in Tomb 10 have been disturbed since burial by natural processes, including bedrock erosion and the infiltration of moisture, roots and basic sediment, and by destructive looters. Nonetheless, the remains furnish considerable information about the mortuary practices of wealthy residents. Analysis of the remains in their archaeological and taphonomic contexts reveals that Tomb 10 contained at least 23 individuals, 15 inhumed in loculi and 8 cremated and placed in niches, sometimes in urns. The identification of males, females and subadults among the burned and unburned bones and teeth suggests that spouses, parents and children probably from several generations of the same lineage or household were buried here. The nature of the cremated fragments reflects a laborious process during which mourners burned bodies on substantial pyres at extremely high temperatures for a long time. Then they carefully extracted a representative sample of small fragments from throughout the reduced skeleton for burial at the tomb. This study contributes to a better understanding of mortuary practices in the Roman East, particularly the Greek world, where the chamber tomb was a common sepulchral type. Copyright (C) 2009 John Wiley & Sons, Ltd. C1 [Ubelaker, D. H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Rife, J. L.] Vanderbilt Univ, Dept Class Studies, Nashville, TN USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, MRC 112, Washington, DC 20560 USA. EM ubelaked@si.edu NR 24 TC 2 Z9 2 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD JAN-FEB PY 2011 VL 21 IS 1 BP 1 EP 18 DI 10.1002/oa.1102 PG 18 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 718YR UT WOS:000287163100006 ER PT J AU Behrensmeyer, AK Bobe, R AF Behrensmeyer, Anna K. Bobe, Rene TI Questions, answers, and more questions: using databases to explore the taphonomy and paleoecology of the African hominin record SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Behrensmeyer, Anna K.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Bobe, Rene] Univ Georgia, Dept Anthropol, Athens, GA 30602 USA. NR 0 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 86 EP 86 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000058 ER PT J AU Bobe, R Behrensmeyer, AK Campisano, C Levin, N Hakala, S Patterson, D Villasenor, A AF Bobe, Rene Behrensmeyer, Anna K. Campisano, Christopher Levin, Naomi Hakala, Sarah Patterson, David Villasenor, Amelia TI The Turkana Basin 3.4 million years ago SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Bobe, Rene; Hakala, Sarah; Patterson, David; Villasenor, Amelia] Univ Georgia, Dept Anthropol, Athens, GA 30602 USA. [Behrensmeyer, Anna K.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Campisano, Christopher] Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. [Campisano, Christopher] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Levin, Naomi] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 92 EP 93 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000080 ER PT J AU Chalk, J Wright, BW Lucas, PW Richmond, BG Fragaszy, D Visalberghi, E Izar, P Ottoni, EB AF Chalk, Janine Wright, Barth W. Lucas, Peter W. Richmond, Brian G. Fragaszy, Dorothy Visalberghi, Elisabetta Izar, Patricia Ottoni, Eduardo B. TI Feeding behaviors and food mechanics during Cebus libidinosus ontogeny SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Chalk, Janine] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Wright, Barth W.] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, KS USA. [Chalk, Janine; Lucas, Peter W.; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Fragaszy, Dorothy] Univ Georgia, Dept Psychol, Athens, GA 30602 USA. [Visalberghi, Elisabetta] CNR, Ist Sci & Tecnol Cogniz, I-00185 Rome, Italy. [Izar, Patricia; Ottoni, Eduardo B.] Univ Sao Paulo, Inst Psychol, Dept Expt Psychol, BR-05508 Sao Paulo, Brazil. RI Ottoni, Eduardo/E-4941-2012 OI Ottoni, Eduardo/0000-0003-1288-8345 NR 0 TC 0 Z9 0 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 107 EP 107 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000135 ER PT J AU Crofoot, M Gilby, I AF Crofoot, Margaret Gilby, Ian TI Variability in the realized resource holding potential of capuchin social groups levels the balance-of-power between unevenly matched neighbors SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Crofoot, Margaret] Smithsonian Trop Res Inst, Balboa, Panama. [Crofoot, Margaret] Max Planck Inst Ornithol, Div Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Crofoot, Margaret] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Gilby, Ian] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA. NR 0 TC 0 Z9 0 U1 1 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 117 EP 117 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000172 ER PT J AU Deane, A Cornett, K Parell, P Tocheri, M AF Deane, Andrew Cornett, Kari Parell, Paul Tocheri, Matthew TI The functional morphology of the metacarpophalangeal joint surface of hominoid manual phalanges. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Deane, Andrew] Univ Kentucky, Dept Anat & Neurobiol, Lexington, KY 40506 USA. [Cornett, Kari; Parell, Paul; Tocheri, Matthew] Univ Kentucky, Coll Hlth Sci, Lexington, KY 40506 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 122 EP 123 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000195 ER PT J AU Dudar, JC AF Dudar, J. Christopher TI Searching and extracting reports from the Osteoware database SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Dudar, J. Christopher] Smithsonian Inst, Natl Museum Nat Hist, Repatriat Osteol Lab, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 128 EP 128 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000219 ER PT J AU Gordon, AD Wood, B AF Gordon, Adam D. Wood, Bernard TI The role of comparative databases in paleoanthropology research. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Gordon, Adam D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Wood, Bernard] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Wood, Bernard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 146 EP 146 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000286 ER PT J AU Green, DJ Richmond, BG Harris, JWK Mbua, E Braun, DR Griffin, NL Chirchir, H AF Green, David J. Richmond, Brian G. Harris, John W. K. Mbua, Emma Braun, David R. Griffin, Nicole L. Chirchir, Habiba TI A new similar to 1.5 Ma hominin scapula from Koobi Fora, Kenya. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Green, David J.; Richmond, Brian G.; Chirchir, Habiba] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Chirchir, Habiba] George Washington Univ, Dept Anthropol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA. [Mbua, Emma] Natl Museums Kenya, Dept Palaeontol, Nairobi, Kenya. [Braun, David R.] Univ Cape Town, Dept Archaeol, ZA-7700 Rondebosch, South Africa. [Griffin, Nicole L.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA. NR 0 TC 1 Z9 1 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 149 EP 149 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000298 ER PT J AU Gunter, S Potts, KB Brown, JL AF Gunter, Sholly Potts, Kevin B. Brown, Janine L. TI The mediation of increased energetic demands by lactating wild chimpanzees: behavioral and hormonal considerations SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Gunter, Sholly] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. [Gunter, Sholly] Baylor Univ, Dept Anthropol Forens Sci & Archaeol, Waco, TX 76798 USA. [Potts, Kevin B.] Augsburg Coll, Dept Biol, Minneapolis, MN USA. [Brown, Janine L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 151 EP 151 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000308 ER PT J AU Harris, TR Monfort, SL Vigilant, L AF Harris, Tara R. Monfort, Steven L. Vigilant, Linda TI Variation in sexual strategies and paternity skew in wild black and white colobus monkeys (Colobus guereza). SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Harris, Tara R.; Vigilant, Linda] Max Planck Inst Evolutionary Anthropol, Dept Primatol, Leipzig, Germany. [Harris, Tara R.; Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Harris, Tara R.] Minnesota Zoo, Apple Valley, MN USA. NR 0 TC 0 Z9 0 U1 3 U2 14 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 157 EP 157 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000330 ER PT J AU Hatala, KG Richmond, BG Harcourt-Smith, WEH Rossi, V Metallo, A Liutkus, CM Pobiner, BL Dingwall, H Moita, GO Brett, J AF Hatala, Kevin G. Richmond, Brian G. Harcourt-Smith, William E. H. Rossi, Vincent Metallo, Adam Liutkus, Cynthia M. Pobiner, Briana L. Dingwall, Heather Moita, Godfrey Olle Brett, Jim TI Early modern human footprints from Engare Sero, Tanzania. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Hatala, Kevin G.] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Washington, DC 20052 USA. [Hatala, Kevin G.; Richmond, Brian G.; Dingwall, Heather] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.; Pobiner, Briana L.] Smithsonian Inst, Natl Museum Amer Hist, Human Origins Program, Washington, DC 20560 USA. [Harcourt-Smith, William E. H.] CUNY Herbert H Lehman Coll, Dept Anthropol, Bronx, NY 10468 USA. [Harcourt-Smith, William E. H.] CUNY, Grad Ctr, Dept Anthropol, New York, NY USA. [Harcourt-Smith, William E. H.] Amer Museum Nat Hist, Div Vertebrate Paleontol, New York, NY 10024 USA. [Rossi, Vincent; Metallo, Adam] Smithsonian Inst, Off Exhibits Cent, Washington, DC 20560 USA. [Liutkus, Cynthia M.] Appalachian State Univ, Dept Geol, Boone, NC 28608 USA. [Moita, Godfrey Olle] Tanzania Dept Antiqu, Tanga, Tanzania. [Brett, Jim] Naturecorp, Kempton, PA USA. NR 0 TC 2 Z9 2 U1 2 U2 7 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 158 EP 158 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000334 ER PT J AU Hinde, K Jin, L Tao, L AF Hinde, Katie Jin, Ling Tao, Lin TI Mother's milk and commensal gut bacteria: what we know and what we need to find out SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Hinde, Katie] Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA USA. [Hinde, Katie] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. [Jin, Ling; Tao, Lin] Univ Illinois, Coll Dent, Dept Oral Biol, Chicago, IL USA. NR 0 TC 1 Z9 1 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 163 EP 164 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000358 ER PT J AU Hinton, J AF Hinton, Janine TI Photographs, radiographs, PENDING, and summary paragraphs in Osteoware SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Hinton, Janine] Smithsonian Inst, Natl Museum Nat Hist, Repatriat Osteol Lab, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 164 EP 164 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000359 ER PT J AU Jones, EB AF Jones, Erica B. TI Documenting dental inventories, development, and wear in Osteoware. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Jones, Erica B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 180 EP 180 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000422 ER PT J AU London, MR AF London, Marilyn R. TI Documentation of pathological conditions in Osteoware SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [London, Marilyn R.] Smithsonian Inst, Repatriat Osteol Lab, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 200 EP 200 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000500 ER PT J AU McFarlin, SC Eriksen, AB Bromage, TG Fawcett, KA Hunt, D Nawrocki, SP Cranfield, MR Mudakikwa, A AF McFarlin, Shannon C. Eriksen, Amandine B. Bromage, Timothy G. Fawcett, Kathyrn A. Hunt, David Nawrocki, Stephen P. Cranfield, Michael R. Mudakikwa, Antoine TI Skeletal pathology in mountain gorillas (Gorilla beringei beringei) from Parc National des Volcans, Rwanda SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [McFarlin, Shannon C.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Eriksen, Amandine B.; Nawrocki, Stephen P.] Univ Indianapolis, Archeol & Forens Lab, Indianapolis, IN USA. [Bromage, Timothy G.] NYU, Coll Dent, Dept Biomat & Biomimet, Hard Tissue Res Unit, New York, NY 10003 USA. [Hunt, David] Smithsonian Inst, Natl Museum Nat Hist, Div Phys Anthropol, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 211 EP 211 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000543 ER PT J AU Milligan, LA Power, ML AF Milligan, Lauren A. Power, Michael L. TI Longitudinal changes in the composition of milk from Gorilla gorilla SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Milligan, Lauren A.] Univ Calif Berkeley, Dept Anthropol, Berkeley, CA 94720 USA. [Milligan, Lauren A.; Power, Michael L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DC USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. NR 0 TC 0 Z9 0 U1 1 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 217 EP 217 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000567 ER PT J AU O'Brien, C AF O'Brien, Claire TI Documenting taphonomy and cranial modification in Osteoware. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [O'Brien, Claire] Smithsonian Inst, Natl Museum Nat Hist, Repatriat Osteol Lab, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 227 EP 227 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000608 ER PT J AU Orr, CM Tocheri, MW Arrott, JL Due, RA Saptomo, EW Sutikna, T Jatmiko Wasisto, S Morwood, MJ Jungers, WL AF Orr, Caley M. Tocheri, Matthew W. Arrott, Jessica L. Due, Rokus Awe Saptomo, E. Wahyu Sutikna, Thomas Jatmiko Wasisto, Sri Morwood, Michael J. Jungers, William L. TI New wrist bones from Homo floresiensis. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Orr, Caley M.; Jungers, William L.] SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY USA. [Tocheri, Matthew W.; Arrott, Jessica L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. [Arrott, Jessica L.] George Washington Univ, Dept Forens Sci, Washington, DC 20052 USA. [Morwood, Michael J.] Univ Wollongong, Wollongong, NSW 2522, Australia. NR 0 TC 2 Z9 2 U1 1 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 230 EP 231 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000620 ER PT J AU Potts, R Tocheri, MW Tryon, CA Kovarovic, K Campisano, CJ Walton, N Halvorsen, B Bjorkevoll, L Hodnefjell, A AF Potts, Richard Tocheri, Matthew W. Tryon, Christian A. Kovarovic, Kris Campisano, Christopher J. Walton, Nick Halvorsen, Bente Bjorkevoll, Lars Hodnefjell, Audun TI The Smithsonian Institution's Human Origins Program Database: development, accessibility, and goals for research and education. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Potts, Richard; Tocheri, Matthew W.] Smithsonian Inst, Human Origins Program, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Tryon, Christian A.] NYU, Dept Anthropol, New York, NY 10003 USA. [Kovarovic, Kris] Univ Durham, Dept Anthropol, Durham DH1 3HP, England. [Campisano, Christopher J.] Arizona State Univ, Inst Human Origins, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Walton, Nick] Legend Club Management Syst UK Ltd, York, N Yorkshire, England. NR 0 TC 2 Z9 2 U1 1 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 242 EP 243 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000667 ER PT J AU Richmond, BG Green, DJ Braun, DR Mbua, E Griffin, NL Chirchir, H Harris, JWK AF Richmond, Brian G. Green, David J. Braun, David R. Mbua, Emma Griffin, Nicole L. Chirchir, Habiba Harris, John W. K. TI New fossils from Ileret, Kenya, and the evolution of hominin hand function SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Richmond, Brian G.; Green, David J.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. [Braun, David R.] Univ Cape Town, Dept Archaeol, ZA-7700 Rondebosch, South Africa. [Griffin, Nicole L.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA. [Chirchir, Habiba] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Washington, DC 20052 USA. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA. NR 0 TC 1 Z9 1 U1 1 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 253 EP 253 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000707 ER PT J AU Schroer, K Wood, B AF Schroer, Katherine Wood, Bernard TI Mandibular premolar molarization: a platyrrhine comparative model. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Schroer, Katherine] George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Schroer, Katherine; Wood, Bernard] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Wood, Bernard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 266 EP 266 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000755 ER PT J AU Skinner, MM Schroer, KE Gunz, P Alemseged, Z Wood, BA Hublin, JJQ AF Skinner, Matthew M. Schroer, Katherine E. Gunz, Philipp Alemseged, Zeresenay Wood, Bernard A. Hublin, Jean-Jac-Ques TI Mandibular P4 morphology among Plio-Pleistocene hominins: taxonomic implications and morphological trends. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Skinner, Matthew M.; Gunz, Philipp; Hublin, Jean-Jac-Ques] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, Leipzig, Germany. [Schroer, Katherine E.] George Washington Univ, Hominid Paleobiol Doctoral Program, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Alemseged, Zeresenay] Calif Acad Sci, Dept Anthropol, San Francisco, CA 94118 USA. [Wood, Bernard A.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Wood, Bernard A.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RI Skinner, Matthew/D-1104-2010; Gunz, Philipp/C-7748-2009 OI Skinner, Matthew/0000-0001-8321-3543; Gunz, Philipp/0000-0002-2350-4450 NR 0 TC 0 Z9 0 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 276 EP 276 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000795 ER PT J AU Sobolewski, ME Mitani, JC Brown, JL AF Sobolewski, Marissa E. Mitani, John C. Brown, Janine L. TI Testosterone and aggression in chimpanzees: novel tests of the challenge hypothesis SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Sobolewski, Marissa E.; Mitani, John C.] Univ Michigan, Dept Anthropol, Ann Arbor, MI 48109 USA. [Brown, Janine L.] Smithsonian Inst, Reprod Endocrinol Lab, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 279 EP 279 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000808 ER PT J AU Tocheri, MW AF Tocheri, Matthew W. TI The evolutionary implications of significant carpal and tarsal variation among gorilla taxa. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 295 EP 295 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000870 ER PT J AU Vernon, DS Tocheri, MW Menter, CG AF Vernon, Danielle Sarah Tocheri, Matthew W. Menter, Colin G. TI A hominin first metatarsal base from Drimolen, South Africa SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Vernon, Danielle Sarah; Menter, Colin G.] Univ Johannesburg, Dept Anthropol & Dev Studies, Johannesburg, South Africa. [Tocheri, Matthew W.] Smithsonian Inst, Human Origins Program, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 299 EP 300 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000888 ER PT J AU Williams, EM Gordon, AD Richmond, BG AF Williams, Erin Marie Gordon, Adam D. Richmond, Brian G. TI Achieving efficiency and accuracy in Oldowan stone tool production SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 80th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 11-16, 2011 CL Minneapolis, MN SP Amer Assoc Phys Anthropol C1 [Williams, Erin Marie] George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Williams, Erin Marie; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Gordon, Adam D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2011 VL 144 SU 52 BP 312 EP 312 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 730LE UT WOS:000288034000938 ER PT J AU Smith, JAM Reitsma, LR Marra, PP AF Smith, Joseph A. M. Reitsma, Leonard R. Marra, Peter P. TI INFLUENCE OF MOISTURE AND FOOD SUPPLY ON THE MOVEMENT DYNAMICS OF A NONBREEDING MIGRATORY BIRD (PARKESIA NOVEBORACENSIS) IN A SEASONAL LANDSCAPE SO AUK LA English DT Article DE dry season; habitat quality; movement ecology; nonbreeding season; Northern Waterthrush; Parkesia noveboracensis ID WARBLERS DENDROICA-CORONATA; WINTERING HERMIT THRUSHES; NON-BREEDING SEASON; HOME-RANGE SIZE; SITE FIDELITY; HABITAT OCCUPANCY; BODY CONDITION; VENEZUELAN MANGROVES; POPULATION-DYNAMICS; NEARCTIC MIGRANTS AB We radiotracked Northern Waterthrushes (Parkesia noveboracensis) in four habitats in Puerto Rico during two winters (i.e., January-April) in 2003 and 2004 to determine the ecological determinants of diurnal space use and overwinter site-persistence in this species. The majority of birds (69%) were sedentary and used a contiguous area within a single habitat over the winter period. A smaller percentage (31%) initially used a contiguous area within a single habitat but then permanently moved from that area to another disjunct location (mean = 418 m). Most of these movements were out of the two habitats (dry forest and Black Mangrove) that became the driest from January to mid-March and into wetter mangrove areas. The primary determinants of movement probability were moisture and food availability on each bird's home range. Foraging areas of birds that eventually moved were drier and had lower food availability than areas used by site-persistent individuals. The sites that these itinerant birds moved to were wetter and had higher food availability, which suggests that individuals moved in response to changing resources. Our results (1) indicate that habitats used by this species differ in suitability and (2) support previous findings that turnover rates within a habitat could serve as an indicator of habitat quality. The ability to predict behavioral responses of individuals to habitat conditions that vary across space and time is essential for understanding individual and population responses to habitat loss and the effects of a changing climate in the New World tropics. Received 17 October 2010, accepted 7 December 2010. C1 [Smith, Joseph A. M.; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Reitsma, Leonard R.] Plymouth State Univ, Dept Biol Sci, Plymouth, NH 03264 USA. RP Smith, JAM (reprint author), Nature Conservancy, Delmont, NJ 08314 USA. EM joseph_smith@tnc.org FU U.S. Department of Defense FX Our research was supported by a grant from the U.S. Department of Defense Legacy Resources Management Program. We thank D. Brown, R. Papish, R. Peters, M. Pollock, T. J. Robinson, and J. Woodcock for their excellent and dedicated work in the field. Additional long hours and able field assistance were provided by A. Byrd, S. Campbell, B. Deluca, B. Gibbons, B. Reitsma, and K. Roux. We thank C. Eberly, W. Martinez, and O. Diaz for facilitating our work at Roosevelt Roads Naval Station and the staff of the U.S. Forest Service Sabana Field Station for generously providing lodging and laboratory space. We thank B. Gould and G. Potts of the U.S. Forest Service International Institute for Tropical Forestry for devoting time to finding and providing appropriate scenes of satellite imagery. Thanks to C. Rimmer and an anonymous reviewer for their comments and suggestions that improved the manuscript. Finally, we thank J. Lodge and J. Wunderle for all of the assistance and hospitality they extended during our stay in Puerto Rico. NR 71 TC 9 Z9 9 U1 2 U2 27 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 JAN PY 2011 VL 128 IS 1 BP 43 EP 52 DI 10.1525/auk.2011.10240 PG 10 WC Ornithology SC Zoology GA 733CJ UT WOS:000288237700005 ER PT J AU Smith, JAM Reitsma, LR Marra, PP AF Smith, Joseph A. M. Reitsma, Leonard R. Marra, Peter P. TI MULTIPLE SPACE-USE STRATEGIES AND THEIR DIVERGENT CONSEQUENCES IN A NONBREEDING MIGRATORY BIRD (PARKESIA NOVEBORACENSIS) SO AUK LA English DT Article DE aggression; habitat quality; nonbreeding season; Northern Waterthrush; Parkesia noveboracensis ID IDEAL DESPOTIC DISTRIBUTION; SEA-LEVEL RISE; AMERICAN REDSTARTS; HABITAT OCCUPANCY; POPULATION REGULATION; TERRITORIAL BEHAVIOR; REPRODUCTIVE SUCCESS; VENEZUELAN MANGROVES; ARTHROPOD ABUNDANCE; NEOTROPICAL MIGRANT AB We investigated the relationships among space-use patterns, home-range attributes, and individual characteristics to determine the consequences of different space-use strategies for the overwinter physical condition of Northern Waterthrushes (Parkesia noveboracensis). We have elsewhere demonstrated that heterogeneity in food availability drives the movement decisions of site-persistent and itinerant individuals during the nonbreeding period. Here, we show that intraspecific competition played an important role in determining where individuals initially and eventually settled. Territoriality, characterized by aggression, site-persistence, and exclusive home ranges, was more often found in males. Territorial birds gained mass over the winter, whereas birds that made midseason home-range shifts or that had home ranges with high intraspecific overlap tended to lose mass over the winter. The benefits associated with territoriality may be the result of maintaining higher-quality territories that were both wetter and had higher food availability than less exclusive home ranges. Our results suggest that despotism in the form of territoriality drives patterns of habitat occupancy, and in this system, high-quality habitat appears to be limiting for the Northern Waterthrush. This may have long-term consequences for the success of individual birds, because continued destruction of naturally limited habitats such as coastal mangroves, and predictions of a drying climate on wintering areas, have the potential to severely affect populations. Received 17 October 2010, accepted 2 December 2010. C1 [Smith, Joseph A. M.; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Reitsma, Leonard R.] Plymouth State Univ, Dept Biol Sci, Plymouth, NH 03264 USA. RP Smith, JAM (reprint author), Nature Conservancy, Delmont, NJ 08314 USA. EM joseph_smith@tnc.org FU U.S. Department of Defense FX Our research was supported by a grant from the U.S. Department of Defense Legacy Resources Management Program. We thank D. Brown, R. Papish, R. Peters, M. Pollock, T. J. Robinson, and J. Woodcock for their excellent and dedicated work in the field. Additional long hours and able field assistance were provided by A. Byrd, S. Campbell, B. Deluca, B. Gibbons, B. Reitsma, and K. Roux. We thank C. Eberly, W. Martinez, and O. Diaz for facilitating our work at Roosevelt Roads Naval Station and the staff of the U.S. Forest Service Sabana Field Station for generously providing lodging and laboratory space. We thank B. Gould and G. Potts of the U.S. Forest Service International Institute for Tropical Forestry for devoting time to finding and providing appropriate scenes of satellite imagery. Thanks to two anonymous reviewers for their comments and suggestions for improvements to the manuscript. Finally, we thank J. Lodge and J. Wunderle for all of the assistance and hospitality they extended during our stay in Puerto Rico. NR 59 TC 10 Z9 10 U1 1 U2 16 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD JAN PY 2011 VL 128 IS 1 BP 53 EP 60 DI 10.1525/auk.2011.10241 PG 8 WC Ornithology SC Zoology GA 733CJ UT WOS:000288237700006 ER PT J AU Frick, MG Zardus, JD Ross, A Senko, J Montano-Valdez, D Bucio-Pacheco, M Sosa-Cornejo, I AF Frick, Michael G. Zardus, John D. Ross, Arnold Senko, Jesse Montano-Valdez, Dulce Bucio-Pacheco, Marcos Sosa-Cornejo, Ingmar TI Novel records and observations of the barnacle Stephanolepas muricata (Cirripedia: Balanomorpha: Coronuloidea); including a case for chemical mediation in turtle and whale barnacles SO JOURNAL OF NATURAL HISTORY LA English DT Article DE sea turtle; barnacle; Stephanolepas muricata; epibiont; symbiosis; chemical mediation ID BALANOIDEA; MORPHOLOGY; LINNAEUS; GRAY AB We report new distribution and host records of the turtle barnacle Stephanolepas muricata Fischer. Ours is the first study to document this species' occurrence in Mexico and in the Atlantic Ocean (North Carolina, Georgia and Florida: USA). We also present the first record of S. muricata from olive ridley sea turtles, Lepidochelys olivacea (Eschscholtz). We discuss the physical and ecological characteristics associated with the specimens collected and present evidence suggesting the likelihood of chemical mediation between embedding coronuloid barnacles like S. muricata and host turtles. We provide the first data on the diet and fecundity of S. muricata. C1 [Frick, Michael G.] Smithsonian Natl Zool Pk, Friends Natl Zoo, Washington, DC 20013 USA. [Zardus, John D.] The Citadel, Dept Biol, Charleston, SC 29409 USA. [Ross, Arnold] Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. [Senko, Jesse] Univ Florida, Florida Cooperat Fish & Wildlife Res Unit, Gainesville, FL 32611 USA. [Senko, Jesse] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Montano-Valdez, Dulce; Bucio-Pacheco, Marcos; Sosa-Cornejo, Ingmar] Escuela Biol, Culiacan Rosales 80030, Sinaloa, Mexico. RP Frick, MG (reprint author), Smithsonian Natl Zool Pk, Friends Natl Zoo, POB 37012,MRC 5516, Washington, DC 20013 USA. EM frickm@si.edu NR 27 TC 10 Z9 12 U1 2 U2 14 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 EI 1464-5262 J9 J NAT HIST JI J. Nat. Hist. PY 2011 VL 45 IS 11-12 BP 629 EP 640 DI 10.1080/00222933.2010.534563 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 732PA UT WOS:000288198400001 ER PT J AU Funk, VA Koekemoer, M AF Funk, V. A. Koekemoer, Marinda TI A Monograph of the Small Tribe Platycarpheae (Compositae: Cichorioideae) SO SYSTEMATIC BOTANY LA English DT Article DE Asteraceae; Arctotideae; biogeography; Botswana; Great Escarpment; Namibia; pollen; South Africa ID ASTERACEAE; POLLEN; EREMOTHAMNEAE; EVOLUTION AB The tribe Platycarpheae has three species; they are found from South Africa, to Namibia and Botswana. The three species have traditionally been placed in a single genus but were recently divided into two (Platycarpha and Platycarphella). All have 'secondary heads' formed by tightly clustered heads on the crown of the rhizome. The three species are easily separated from one another based on characters such as leaf type, head size, style and corolla length, and pollen type. Morphological and molecular data support Platycarpheae as a monophyletic group within the subfamily Cichorioideae but no firm sister-group relationship has been determined. The three species form a monophyletic group on a long branch: Platycarphella carlinoides and Platycarphella parvifolia share more characters and are sister-taxa; Platycarpha glomerata has the largest number of unique features and is the sister taxon to the other two species. The distributions and flowering times of the three species are different. Platycarphella carlinoides is the most widespread of the species and grows in northwestern South Africa, the central highlands of Namibia, and southwestern Botswana; its peak flowering time is March-July. Platycarphella parvifolia is found in north central to northeast South Africa and flowers mostly in August to October, and Platycarpha glomerate is from inland eastern South Africa and usually flowers from November to early February. The biogeographic pattern is consistent with one of a widespread ancestral species that became fragmented by the rise of the Great Escarpment and climate change. C1 [Funk, V. A.] Natl Museum Nat Hist, Smithsonian Inst, US Natl Herbarium, Washington, DC 20013 USA. [Koekemoer, Marinda] S African Natl Biodivers Inst, ZA-0001 Pretoria, South Africa. RP Funk, VA (reprint author), Natl Museum Nat Hist, Smithsonian Inst, US Natl Herbarium, Washington, DC 20013 USA. EM funkv@si.edu FU Smithsonian Institution FX Our thanks go to J. Gregson (BM), D. J. N. Hind (K), N. Biggs (K), and M. Hjertson (UPS), for helping track down types at their respective institutions and for sending the scanned images; also to A. Anderberg (S) and F. Schuhwerk (M) for taking the time to scan the images of the collections housed at their institutions. Thanks to the Smithsonian Institution's Restricted Endowment Program for provided funding for field work; and SANBI for assistance in field work and for supplying an electronic list of Platycarpha specimens. Thanks also to E. Klaassen and C. Mannheimer (WIND) who kindly helped with the locations in Namibia, and H. Steyn (PRE) for generating the distribution map. We appreciate the photographs taken by C. Mannheimer (WIND). Also, we thank Peter Linder and Richard Cowling who provided helpful information on possible explanations of the distribution of the taxa and Santiago Ortiz, an anonymous reviewer, and the editors for their helpful comments. We are especially grateful for all the time Alice Tangerini (US) spent on the beautiful pencil illustrations. Many of her illustrations are available on the SI Department of Botany website http://botanysi.edu/botart/. NR 49 TC 0 Z9 0 U1 0 U2 2 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JAN-MAR PY 2011 VL 36 IS 1 BP 191 EP 208 DI 10.1600/036364411X553270 PG 18 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 727BQ UT WOS:000287772700022 ER PT J AU Rowland, CE Cahill, CL Post, JE AF Rowland, Clare E. Cahill, Christopher L. Post, Jeffrey E. TI The structure of braitschite, a calcium rare earth borate SO AMERICAN MINERALOGIST LA English DT Article DE Braitschite; borate; rare earth mineral; crystal structure ID CRYSTAL-STRUCTURE; POWDER DIFFRACTION AB The crystal structure of braitschite, Ca6.15Na0.85RE2.08[B6O7(OH)(3)(O,OH)(3)](4)(H2O), is reported here in space group P6/m with unit-cell parameters a = 12.1506(6), c = 7.3678(4) angstrom, and V= 942.03(8) angstrom(3). Data were collected from a single crystal using a MoK alpha source and a CCD detector, solved by direct methods, and refined to an R factor of 2.81%. The mineral structure consists of hexaborate fundamental building blocks that polymerize along [001] and are bound by Ca2+ and REE3+ counterions. The framework forms hexagonal channels, which are occupied alternately by Ca2+ cations and water molecules. In an investigation or its thermal stability, braitschite maintains its crystallinity to a temperature of 400 degrees C, after which it undergoes decomposition. Using Rietveld refinements against powder X-ray diffraction data, we were able to track the loss of water molecules in channels and hydroxyl groups in the covalent B-O network with increasing temperature. C1 [Rowland, Clare E.; Cahill, Christopher L.] George Washington Univ, Dept Chem, Washington, DC 20052 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Rowland, CE (reprint author), George Washington Univ, Dept Chem, Washington, DC 20052 USA. EM postj@si.edu RI Rowland, Clare/C-2704-2013 OI Rowland, Clare/0000-0002-5474-5257 FU U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-SC0001089]; National Science Foundation [DMR-0419754] FX This work was a side project for C.E.R. while supported by an Energy Frontier Research Center funded by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences under Award Number DE-SC0001089. X-ray diffraction equipment was purchased with National Science Foundation funding (DMR-0419754). We are grateful to two thoughtful reviewers whose suggestions made this an improved manuscript. NR 22 TC 0 Z9 0 U1 1 U2 4 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD JAN PY 2011 VL 96 IS 1 BP 197 EP 201 DI 10.2138/am.2011.3592 PG 5 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 703OP UT WOS:000285988400021 ER PT J AU Ivanenko, VN Ferrari, FD Defaye, D Sarradin, PM Sarrazin, J AF Ivanenko, Viatcheslav N. Ferrari, Frank D. Defaye, Danielle Sarradin, Pierre-Marie Sarrazin, Jozee TI Description, distribution and microhabitats of a new species of Tisbe (Copepoda: Harpacticoida: Tisbidae) from a deep-sea hydrothermal vent field at the Mid-Atlantic Ridge (37 degrees N, Lucky Strike) SO CAHIERS DE BIOLOGIE MARINE LA English DT Article DE Copepoda; Harpacticoida; Tisbidae; Deep-sea; Hydrothermal vent; Mid-Atlantic Ridge; Systematics; Ecology; Microhabitat; In situ experiments; Physico-chemical factors ID EAST PACIFIC RISE; TEGASTES-FALCATUS NORMAN; AZORES TRIPLE JUNCTION; COLD SEEP; CRUSTACEA; COMMUNITIES; ANTARCTICA; TUBEWORM; ECOLOGY; MEXICO AB A new species, Tisbe dahmsi sp. nov. (Crustacea, Copepoda: Harpacticoida: Tisbidae) is described from the Eiffel Tower edifice located in the Lucky Strike vent field (37 degrees N) (Mid-Atlantic Ridge MAR, 1698 m). The samples were collected in colonization experiments (SMAC arrays) that were deployed in 1997 during the MARVEL cruise and recovered in 1998 during the PICO cruise. Other specimens were collected during the MoMARETO cruise during which a physico-chemical characterization of copepod microhabitats was done. The new species belongs to the T. gracilis group based on similarities of the spine-like inner seta on the proximal endopodal segment of the male second swimming leg, which is terminally bifurcate. Re-examination of the closest relative and shallow-water species T. gracilis revealed a number of distinctions, including differences in shape and ornamentation of this terminally bifurcate seta. Tisbe dahmsi sp. nov. is found abundantly in the in situ colonization experiments (SMAC arrays) deployed on Bathymodiolus azoricus mussel assemblages at the Eiffel Tower edifice, together with the cyclopoid copepod Hepterina confusa Ivanenko & Defaye, 2004 (Cyclopoida: Cyclopinidae), the harpacticoid copepod Smacigastes micheli Ivanenko & Defaye, 2004 (Harpacticoida: Tegastidae) and the dirivultid copepod Aphotopontius atlanteus Humes, 1996 (Siphonostomatoida: Dirivultidae). Another colonization experiment, deployed near a black smoker, exhibits a different pattern with dominance of the harpacticoid families Ameiridae and Argestidae of the Ectinosomatidae family. These colonization experiments revealed that copepods of the genus Tisbe were substantially more abundant in the trays deployed on mussel assemblages than to those in the vicinity of black smokers. Nevertheless, no clear response regarding the effect of organic enrichment on copepod abundance was observed. The type of environment where the arrays were deployed appears to have a stronger influence on copepod abundances and composition than the treatment applied within each tray. Directly on the Eiffel Tower edifice, Tisbe copepods were found within different Bathymodiolus azoricus assemblages. These assemblages were alternatively dominated (in terms of copepods) by the Dirivultidae or the Tegastidae, the former being dominant in 67% of the samples. In terms of environmental conditions, Tisbe dahmsi was found in microhabitats characterized by low temperatures C1 [Sarradin, Pierre-Marie; Sarrazin, Jozee] IFREMER, Ctr Brest, Dept Etud Ecosyst Profonds, Lab Environm Profond, F-29280 Plouzane, France. [Ivanenko, Viatcheslav N.] Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. [Ferrari, Frank D.] IZ MSC, Natl Museum Nat Hist, Smithsonian Inst, MRC 534, Suitland, MD 20746 USA. [Defaye, Danielle] Museum Natl Hist Nat, Dept Milieux & Peuplements Aquat, UMR 7208, F-75005 Paris, France. RP Sarrazin, J (reprint author), IFREMER, Ctr Brest, Dept Etud Ecosyst Profonds, Lab Environm Profond, BP 70, F-29280 Plouzane, France. EM jozee.sarrazin@ifremer.fr RI Ivanenko, Viatcheslav/B-8198-2008; MNHN/CNRS/UPMC/IRD, UMR BOREA/B-2312-2012 OI Ivanenko, Viatcheslav/0000-0003-1255-0491; FU MAST3 [MAST3 CT 95-0040]; Ifremer; EXOCET/D European program; Museum national d'Histoire naturelle and Ifremer (France); Smithsonian Institution (USA); Russian Foundation for Basic Research [09-04-01523-a]; Ministry of Education and Science of the Russian Federation [02.740.11.0280, Pi1291]; MarBEF; CeDAMar; ANR DEEP-OASES [ANR06BDV005]; GDR ECCHIS FX The MARVEL cruise was led by Daniel Desbruyeres and Anne-Marie Alayse (chief scientists); the PICO cruise was led by Daniel Desbruyeres (chief scientist). These cruises were supported by the MAST3 program AMORES (MAST3 CT 95-0040) and Ifremer. The MoMARETO cruise was led by Jozee Sarrazin and Pierre-Marie Sarradin (chief scientists) and part of it was supported by the EXOCET/D European program. Thanks are due to Philippe Crassous who prepared the sampling arrays, whereas Michel Segonzac and Patrick Briand provided the sorted material and sampling data (Ifremer, France) for the colonization experiments. Regis Cleva (Museum national d'Histoire naturelle, France) assisted during SEM study realized at the Service Commun des Sciences de la Vie du Museum national d'Histoire naturelle (Paris, France). The study of copepods was supported by grants from the Museum national d'Histoire naturelle and Ifremer (France), Smithsonian Institution (USA), the Russian Foundation for Basic Research (09-04-01523-a), the Ministry of Education and Science of the Russian Federation: 02.740.11.0280 & Pi 1291), MarBEF, CeDAMar, ANR DEEP-OASES (ANR06BDV005), and GDR ECCHIS. NR 51 TC 5 Z9 5 U1 0 U2 4 PU CAHIERS DE BIOLOGIE MARINE PI ROSCOFF PA STATION BIOLOGIQUE PLACE GEORGES TEISSIER, 29680 ROSCOFF, FRANCE SN 0007-9723 EI 2262-3094 J9 CAH BIOL MAR JI Cah. Biol. Mar. PY 2011 VL 52 IS 1 BP 89 EP 106 PG 18 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 710HN UT WOS:000286501900010 ER PT J AU Orem, W Gilmour, C Axelrad, D Krabbenhoft, D Scheidt, D Kalla, P McCormick, P Gabriel, M Aiken, G AF Orem, William Gilmour, Cynthia Axelrad, Donald Krabbenhoft, David Scheidt, Daniel Kalla, Peter McCormick, Paul Gabriel, Mark Aiken, George TI Sulfur in the South Florida Ecosystem: Distribution, Sources, Biogeochemistry, Impacts, and Management for Restoration SO CRITICAL REVIEWS IN ENVIRONMENTAL SCIENCE AND TECHNOLOGY LA English DT Review DE Everglades; methylmercury; sulfate; sulfur; water quality ID CLADIUM-JAMAICENSE CYPERACEAE; FERTILIZER-DERIVED URANIUM; FRESH-WATER WETLANDS; NEW-JERSEY PINELANDS; TYPHA-DOMINGENSIS; EVERGLADES RESTORATION; NORTHERN EVERGLADES; HYDROGEN SULFIDE; TROPHIC GRADIENT; SULFATE AB Sulfur is broadly recognized as a water quality issue of significance for the freshwater Florida Everglades. Roughly 60% of the remnant Everglades has surface water sulfate concentrations above 1 mg l-1, a restoration performance measure based on present sulfate levels in unenriched areas. Highly enriched marshes in the northern Everglades have average sulfate levels of 60 mg l-1. Sulfate loading to the Everglades is principally a result of land and water management in South Florida. The highest concentrations of sulfate (average 60-70 mg l-1) in the ecosystem are in canal water in the Everglades Agricultural Area (EAA). Potential sulfur sourcesin the watershed are many, but geochemical data and a preliminary sulfur mass balance for the EAA are consistent with sulfur presently used in agricultural, and sulfur released by oxidation of organic EAA soils (including legacy agricultural applications and natural sulfur) as the primary sources of sulfate enrichment in the EAA canals. Sulfate loading to the Everglades increases microbial sulfate reduction in soils, leading to more reducing conditions, greater cycling of nutrients in soils, production of toxic sulfide, and enhanced methylmercury (MeHg) production and bioaccumulation. Wetlands are zones of naturally high MeHg production, but the combination of high atmospheric mercury deposition rates in South Florida and elevated sulfate loading leads to increased MeHg production and MeHg risk to Everglades wildlife and human consumers. Sulfate from the EAA drainage canals penetrates deep into the Everglades Water Conservation Areas, and may extend into Everglades National Park. Present plans to restore sheet flow and to deliver more water to the Everglades may increase overall sulfur loads to the ecosystem, and move sulfate-enriched water further south. However, water management practices that minimize soil drying and rewetting cycles can mitigate sulfate release during soil oxidation. A comprehensive Everglades restoration strategy should include reduction of sulfur loads as a goal because of the many detrimental impacts of sulfate on the ecosystem. Monitoring data show that the ecosystem response to changes in sulfate levels is rapid, and strategies for reducing sulfate loading may be effective in the near term. A multifaceted approach employing best management practices for sulfur in agriculture, agricultural practices that minimize soil oxidation, and changes to stormwater treatment areas that increase sulfate retention could help achieve reduced sulfate loads to the Everglades, with resulting benefits. C1 [Orem, William] US Geol Survey, Reston, VA 20192 USA. [Gilmour, Cynthia] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Axelrad, Donald] Florida Dept Environm Protect, Tallahassee, FL USA. [Krabbenhoft, David] US Geol Survey, Middleton, WI USA. [Scheidt, Daniel; Kalla, Peter] US EPA, Athens, GA USA. [McCormick, Paul; Gabriel, Mark] S Florida Water Management Dist, W Palm Beach, FL USA. [Aiken, George] US Geol Survey, Boulder, CO USA. RP Orem, W (reprint author), US Geol Survey, 959 Natl Ctr, Reston, VA 20192 USA. EM borem@usgs.gov RI Gilmour, Cynthia/G-1784-2010 OI Gilmour, Cynthia/0000-0002-1720-9498 FU U.S. Geological Survey; U.S. Environmental Protection Agency; National Park Service; Army Corps of Engineers; South Florida Water Management District; Florida Department of Environmental Protection FX The research described in this report was supported by funding from a number of Federal and State agencies: the U.S. Geological Survey (Priority Ecosystems Studies for South Florida-G. Ronnie Best, Program Executive), the U.S. Environmental Protection Agency, the National Park Service, the Army Corps of Engineers, the South Florida Water Management District, and the Florida Department of Environmental Protection. The authors thank Alan Kolker and Mark Engle from the USGS, Samira Daroub of the University of Florida, Garth Redfield (South Florida Water Management District), and one anonymous reviewer for their helpful comments on the manuscript. NR 130 TC 30 Z9 32 U1 6 U2 51 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1064-3389 J9 CRIT REV ENV SCI TEC JI Crit. Rev. Environ. Sci. Technol. PY 2011 VL 41 SU 1 BP 249 EP 288 AR PII 933735549 DI 10.1080/10643389.2010.531201 PG 40 WC Environmental Sciences SC Environmental Sciences & Ecology GA 723GG UT WOS:000287494000010 ER PT J AU Brawn, JD Angehr, G Davros, N Robinson, WD Styrsky, JN Tarwater, CE AF Brawn, Jeffrey D. Angehr, George Davros, Nicole Robinson, W. Douglas Styrsky, Jennifer N. Tarwater, Corey E. TI Sources of variation in the nesting success of understory tropical birds SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID LIFE-HISTORY; CLUTCH SIZE; EL-NINO; FOREST; PREDATION; SNAKES; PANAMA; SURVIVAL; AMERICA; SITES AB Survival of offspring is a key fitness component and, for birds, the threat of predation on nests is especially influential. Data on rates of nest success from tropical regions are comparatively few, conservation-relevant, and essential for assessing the validity of models comparing the life histories and behavior or birds across latitudinal gradients. We monitored over 2 000 nests in the lowland forests of central Panama and, using the logistic exposure to model the fate of nests, explored the importance of variation in rate of nest success according to type of nest, height of nests, among years, in early versus late nests, and at different stages of the nest cycle. Analyses of over 1 400 nests for 18 species revealed considerable variation among species in the daily survival rate of nests (range among 18 species=0.91 to 0.98), but nest type and stage of the nesting cycle were generally influential on the probability of nest success. Cavity or enclosed nesters experienced greater nest success than open cup nesters and rates of nest loss were generally greatest in the nestling stage. We found limited evidence that height of nests affected probability of success, but no indication that timing of nesting effort was influential. Despite the occurrence of a severe ENSO event during our sampling, annual variation in nest success was not consistent among species. Interspecific variation in the rates and patterns of nest predation in our study, coupled with reports of high rates of nest loss at temperate latitudes, lead us to question long standing assumptions about latitudinal trends in rates of nest loss. We urge further work to understand the implications of nest predation on the evolutionary ecology of tropical birds. C1 [Brawn, Jeffrey D.] Univ Illinois, Dept Nat Resources & Environm Sci, Champaign, IL 61820 USA. [Angehr, George] Smithsonian Trop Res Inst, Balboa, Panama. [Davros, Nicole; Tarwater, Corey E.] Univ Illinois, Progr Ecol Evol & Cons Biol, Champaign, IL 61820 USA. [Robinson, W. Douglas] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. RP Brawn, JD (reprint author), Univ Illinois, Dept Nat Resources & Environm Sci, 1102 S Goodwin Ave,606 E Healy St, Champaign, IL 61820 USA. EM jbrawn@illinois.edu FU U. S. Department of Defense; National Science Foundation [IBN-0212587]; University of Illinois; Smithsonian Tropical Research Institute FX We thank the patient and indefatigable field assistants, especially C. Bastista, M. Libsch, I. Ochoa, and J. Ortega. Scott K. Robinson and Tara R. Robinson provided valuable assistance in all phases. The Autoridad Nacional del Ambiente kindly granted us permission to work in the Republic of Panama. Deep appreciation to the Smithsonian Tropical Research Institute for providing logistical support, especially Raineldo Urriola and Orelis Arosemena. The University of Illinois Institutional Animal Care and Use Committee and the Smithsonian Tropical Research Institute approved this research. This work was funded by the U. S. Department of Defense Legacy Resource Management Program, the National Science Foundation grant IBN-0212587, grants from University of Illinois, and the Environmental Science Program from the Smithsonian Tropical Research Institute. NR 43 TC 23 Z9 23 U1 4 U2 34 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD JAN PY 2011 VL 42 IS 1 BP 61 EP 68 DI 10.1111/j.1600-048X.2010.04897.x PG 8 WC Ornithology SC Zoology GA 726UX UT WOS:000287753000009 ER PT J AU Zipfel, J Schroder, C Jolliff, BL Gellert, R Herkenhoff, KE Rieder, R Anderson, R Bell, JF Bruckner, J Crisp, JA Christensen, PR Clark, BC de Souza, PA Dreibus, G d'Uston, C Economou, T Gorevan, SP Hahn, BC Klingelhofer, G McCoy, TJ McSween, HY Ming, DW Morris, RV Rodionov, DS Squyres, SW Wanke, H Wright, SP Wyatt, MB Yen, AS AF Zipfel, Jutta Schroeder, Christian Jolliff, Bradley L. Gellert, Ralf Herkenhoff, Kenneth E. Rieder, Rudolf Anderson, Robert Bell, James F., III Brueckner, Johannes Crisp, Joy A. Christensen, Philip R. Clark, Benton C. de Souza, Paulo A., Jr. Dreibus, Gerlind d'Uston, Claude Economou, Thanasis Gorevan, Steven P. Hahn, Brian C. Klingelhoefer, Goestar McCoy, Timothy J. McSween, Harry Y., Jr. Ming, Douglas W. Morris, Richard V. Rodionov, Daniel S. Squyres, Steven W. Waenke, Heinrich Wright, Shawn P. Wyatt, Michael B. Yen, Albert S. TI Bounce Rock-A shergottite-like basalt encountered at Meridiani Planum, Mars SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID X-RAY SPECTROMETER; FE-BEARING CLINOPYROXENES; MARTIAN METEORITES; OPPORTUNITY ROVER; GUSEV CRATER; MOSSBAUER SPECTROMETER; TEMPERATURE-DEPENDENCE; HYPERFINE PARAMETERS; CA-RICH; CHEMISTRY AB The Opportunity rover of the Mars Exploration Rover mission encountered an isolated rock fragment with textural, mineralogical, and chemical properties similar to basaltic shergottites. This finding was confirmed by all rover instruments, and a comprehensive study of these results is reported here. Spectra from the miniature thermal emission spectrometer and the Panoramic Camera reveal a pyroxene-rich mineralogy, which is also evident in Mossbauer spectra and in normative mineralogy derived from bulk chemistry measured by the alpha particle X-ray spectrometer. The correspondence of Bounce Rock's chemical composition with the composition of certain basaltic shergottites, especially Elephant Moraine (EET) 79001 lithology B and Queen Alexandra Range (QUE) 94201, is very close, with only Cl, Fe, and Ti exhibiting deviations. Chemical analyses further demonstrate characteristics typical of Mars such as the Fe/Mn ratio and P concentrations. Possible shock features support the idea that Bounce Rock was ejected from an impact crater, most likely in the Meridiani Planum region. Bopolu crater, 19.3 km in diameter, located 75 km to the southwest could be the source crater. To date, no other rocks of this composition have been encountered by any of the rovers on Mars. The finding of Bounce Rock by the Opportunity rover provides further direct evidence for an origin of basaltic shergottite meteorites from Mars. C1 [Zipfel, Jutta] Senckenberg Forschungsinst, Sekt Meteoritenforsch, D-60325 Frankfurt, Germany. [Zipfel, Jutta] Nat Museum Frankfurt, D-60325 Frankfurt, Germany. [Schroeder, Christian; Klingelhoefer, Goestar; Rodionov, Daniel S.] Johannes Gutenberg Univ Mainz, Inst Anorgan Chem & Analyt Chem, D-55128 Mainz, Germany. [Jolliff, Bradley L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Gellert, Ralf] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Herkenhoff, Kenneth E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Rieder, Rudolf; Brueckner, Johannes; Dreibus, Gerlind; Waenke, Heinrich] Max Planck Inst Chem, Abt Geochem, D-55020 Mainz, Germany. [Anderson, Robert; Crisp, Joy A.; Yen, Albert S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bell, James F., III; Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Christensen, Philip R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Clark, Benton C.] Lockheed Martin Corp, Littleton, CO 80127 USA. [de Souza, Paulo A., Jr.] CSIRO, Tasmanian ICT Ctr, Hobart, Tas 7001, Australia. [d'Uston, Claude] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. [Economou, Thanasis] Univ Chicago, Enrico Fermi Inst, Lab Atmospher & Space Res, Chicago, IL 60637 USA. [Gorevan, Steven P.] Honeybee Robot, New York, NY 10012 USA. [Hahn, Brian C.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Ming, Douglas W.; Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wright, Shawn P.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Wyatt, Michael B.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Zipfel, J (reprint author), Senckenberg Forschungsinst, Sekt Meteoritenforsch, Senckenberganlage 25, D-60325 Frankfurt, Germany. EM jzipfel@senckenberg.de RI de Souza, Paulo/B-8961-2008; Centre, TasICT/D-1212-2011; Schroder, Christian/B-3870-2009; Crisp, Joy/H-8287-2016 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; Crisp, Joy/0000-0002-3202-4416 FU National Aeronautics and Space Administration FX The authors thank the Meteorite Working Group and the curator for Antarctic meteorites, Kevin Righter, for loan of an unpolished butt of EETA79001. Some of this research was carried out at and for the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration. This article has benefitted greatly from reviews of an earlier version of the manuscript by Phil Bland, Cyrena Goodrich, Takashi Mikouchi, Deon van Niekerk, and Larry Nittler. We also thank M. Schmidt, E. Walton, and Alan Treiman for their reviews. NR 72 TC 22 Z9 22 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JAN PY 2011 VL 46 IS 1 BP 1 EP 20 DI 10.1111/j.1945-5100.2010.01127.x PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 719YR UT WOS:000287247900001 ER PT J AU Santiago-Blay, JA Lambert, JB Creasman, PP AF Santiago-Blay, Jorge A. Lambert, Joseph B. Creasman, Pearce Paul TI EXPANDED APPLICATION OF DENDROCHRONOLOGY COLLECTIONS: COLLECT AND SAVE EXUDATES SO TREE-RING RESEARCH LA English DT Editorial Material C1 [Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Lambert, Joseph B.] Trinity Univ, Dept Chem, San Antonio, TX 78212 USA. [Lambert, Joseph B.] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. [Creasman, Pearce Paul] Univ Arizona, Tree Ring Res Lab, Tucson, AZ 85721 USA. RP Santiago-Blay, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121, Washington, DC 20013 USA. EM BLAYJ@si.edu; pcreasman@ltrr.arizona.edu NR 13 TC 2 Z9 2 U1 0 U2 3 PU TREE-RING SOC PI TUCSON PA UNIV ARIZONA, TREE-RING LABORATORY, BLDG 58, TUCSON, AZ 85721 USA SN 1536-1098 J9 TREE-RING RES JI Tree-Ring Res. PY 2011 VL 67 IS 1 BP 67 EP 68 DI 10.3959/2010-7.1 PG 2 WC Forestry SC Forestry GA 707RX UT WOS:000286304800009 ER PT J AU Liu, F McShea, WJ Garshelis, DL Zhu, XJ Wang, DJ Shao, LK AF Liu, Fang McShea, William J. Garshelis, David L. Zhu, Xiaojian Wang, Dajun Shao, Liangkun TI Human-wildlife conflicts influence attitudes but not necessarily behaviors: Factors driving the poaching of bears in China SO BIOLOGICAL CONSERVATION LA English DT Article DE Asiatic black bear; Bear parts trade; Crop damage; Interview survey; Livestock predation ID ASIATIC BLACK BEARS; JAGUAR PANTHERA-ONCA; NATIONAL-PARK; PROTECTED AREAS; CONSERVATION IMPLICATIONS; ENVIRONMENTAL ATTITUDES; LIVESTOCK PREDATION; LARGE CARNIVORES; LYCAON-PICTUS; LOCAL PEOPLE AB Human-wildlife conflicts often spur retaliatory killing, which may be a major threat to some wildlife species. Asiatic black bears depredate crops and livestock and also attack humans. We investigated whether human-bear conflicts in Sichuan Province, southwestern China, resulted in increased bear poaching. We conducted semi-structured interviews within 429 15 x 15-km cells across the province, asking villagers about bear occurrence, population trends, attitudes toward bears, human-bear conflicts, responses to bear damage, and bear poaching. Bears raided crops (n = 174 cells), killed livestock (n = 114 cells), and attacked people (n = 49 cells). Fifty percent and 43% of villagers held negative and neutral attitudes toward bears, respectively; attitudes were more negative among people who had previous interactions with bears or lived where bear encounters were more likely. Although killing bears was illegal, villagers in 117 cells (38%) indicated that bear poaching occurred around their villages. However, killing bears was not significantly linked to damage: indeed, killing was more common in areas without human-bear conflicts. Poachers killed bears mainly for trade of their valuable parts (gall bladder and paws, 78.5%). Tibetan people experienced bear damage and also had negative attitudes toward bears, but reported less poaching than Han or Yi people, due to their religious beliefs. Our study indicated that human-wildlife conflicts shaped people's attitudes toward bears, but strong economic incentives, not attitudes, prompted illegal killing. Whereas mitigation of human-bear conflicts could help foster more positive attitudes toward bears and the nature reserves that protect bears, this strategy will not remove the primary threat against this species. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Liu, Fang; Zhu, Xiaojian; Wang, Dajun] Peking Univ, Coll Life Sci, Beijing 100871, Peoples R China. [McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Garshelis, David L.] Minnesota Dept Nat Resources, Grand Rapids, MN 55744 USA. [Shao, Liangkun] Wanglang Natl Nat Reserve, Pingwu County 22550, Sichuan, Peoples R China. RP Liu, F (reprint author), Chinese Acad Forestry, Inst Forest Ecol Environm & Protect, Xiangshan Rd, Beijing 100089, Peoples R China. EM fangliu.pku@gmail.com FU Smithsonian Institution; National Zoo; World Society of Protected Animals (WSPA); International Association of Bear Research and Management (IBA); Earth Watch; Animals Asia Foundation FX This research was funded by the Smithsonian Institution, Friends of the National Zoo, World Society of Protected Animals (WSPA), the International Association of Bear Research and Management (IBA), Earth Watch, and Animals Asia Foundation. We appreciate Sichuan Forestry Department for giving us permission to do the survey. In all surveyed counties, the local forestry bureaus facilitated the fieldwork. We are grateful to Ke Ding (Sichuan University), Lu Zhang and Sheng Li (Peking University), and Earthwatch volunteers for help with the fieldwork. Also key to our field operations were director Shiwei Jiang and the staff of Wanglang Nature Reserve, particularly, Lianjun Zhao, Luogui Yan, Yinzhu Zhang, Jian Liu, Hualong Zhou, Shaojun Zhang, Yuanming Wen, Gaoshan Lan, Zhiwei Yuan, Jianhua Zhao, Chunping Liang, Ansong Long, and Jinyuan Cui. NR 74 TC 29 Z9 29 U1 13 U2 112 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD JAN PY 2011 VL 144 IS 1 BP 538 EP 547 DI 10.1016/j.biocon.2010.10.009 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 719AA UT WOS:000287168100058 ER PT J AU Lee, CF Bezdek, J Staines, CL AF Lee, Chi-Feng Bezdek, Jan Staines, Charles L. TI A Review of the Genus Haplosomoides Duvivier, 1890 in Taiwan and Japan (Coleoptera: Chrysomelidae: Galerucinae) SO ZOOLOGICAL STUDIES LA English DT Review DE Taxonomy; New species; Leaf beetles AB Chi-Feng Lee, Jan Bezdek, and Charles L. Staines (2011) A review of the genus Haplosomoides Duvivier, 1890 in Taiwan and Japan (Coleoptera: Chrysomelidae: Galerucinae). Zoological Studies 50(1): 118-138. Species of the genus Haplosomoides Duvivier in Japan and Taiwan are reviewed taxonomically. Four new species, Haplosomoides chengi sp. nov., H. changi sp. nov., and H. tsoui sp. nov. from Taiwan and H. ryukyuensis sp. nov. from Japan are described. Two known species are redescribed: H. miyamotoi Kimoto and H. abdominalis Kimoto. Their allied species, H. costata (Baly) and H. annamita (Allard) are also redescribed for comparison. A key to the species of Haplosomoides in Japan and Taiwan and their allied species is provided. http://zoolstud.sinica.edu.tw/Journals/50.1/118.pdf C1 [Lee, Chi-Feng] Agr Res Inst Taiwan, Appl Zool Div, Taichung 413, Taiwan. [Bezdek, Jan] Mendel Univ Brno, Dept Zool, Brno 61300, Czech Republic. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, MRC 187, Dept Entomol, Washington, DC 20013 USA. RP Lee, CF (reprint author), Agr Res Inst Taiwan, Appl Zool Div, 189 Chung Cheng Rd, Taichung 413, Taiwan. EM chifeng@tari.gov.tw; bezdek@mendelu.cz; stainesc@si.edu RI stud, zool/G-4030-2011 NR 37 TC 2 Z9 2 U1 0 U2 3 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1021-5506 EI 1810-522X J9 ZOOL STUD JI Zool. Stud. PD JAN PY 2011 VL 50 IS 1 BP 118 EP 138 PG 21 WC Zoology SC Zoology GA 710TA UT WOS:000286538700014 ER PT J AU Morgan, GA Head, JW Marchant, DR AF Morgan, Gareth A. Head, James W. Marchant, David R. TI Preservation of Late Amazonian Mars ice and water-related deposits in a unique crater environment in Noachis Terra: Age relationships between lobate debris tongues and gullies SO ICARUS LA English DT Article DE Mars, Climate; Mars, Surface; Planetary dynamics ID MCMURDO DRY VALLEYS; SURFACE GROUND ICE; FAN-SHAPED DEPOSIT; LIQUID WATER; MARTIAN GULLIES; CLIMATE-CHANGE; SOUTHERN MIDLATITUDES; COVERED GLACIER; HIGH OBLIQUITY; IMPACT CRATER AB The Amazonian period of Mars has been described as static, cold, and dry. Recent analysis of high-resolution imagery of equatorial and mid-latitude regions has revealed an array of young landforms produced in association with ice and liquid water; because near-surface ice in these regions is currently unstable, these ice-and-water-related landforms suggest one or more episodes of martian climate change during the Amazonian. Here we report on the origin and evolution of valley systems within a degraded crater in Noachis Terra, Asimov Crater. The valleys have produced a unique environment in which to study the geomorphic signals of Amazonian climate change. New high-resolution images reveal Hesperian-aged layered basalt with distinctive columnar jointing capping interior crater fill and providing debris, via mass wasting, for the surrounding annular valleys. The occurrence of steep slopes (>20 degrees), relatively narrow (sheltered) valleys, and a source of debris have provided favorable conditions for the preservation of shallow-ice deposits. Detailed mapping reveals morphological evidence for viscous ice flow, in the form of several lobate debris tongues (LDT). Superimposed on LDT are a series of fresh-appearing gullies, with typical alcove, channel, and fan morphologies. The shift from ice-rich viscous-flow formation to gully erosion is best explained as a shift in martian climate, from one compatible with excess snowfall and flow of ice-rich deposits, to one consistent with minor snow and gully formation. Available dating suggests that the climate transition occurred >8 Ma, prior to the formation of other small-scale ice-rich flow features identified elsewhere on Mars that have been interpreted to have formed during the most recent phases of high obliquity. Taken together, these older deposits suggest that multiple climatic shifts have occurred over the last tens of millions of years of martian history. (C) 2010 Elsevier Inc. All rights reserved. C1 [Morgan, Gareth A.; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Marchant, David R.] Boston Univ, Dept Earth Sci, Boston, MA 02215 USA. RP Morgan, GA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM MorganGA@si.edu FU NASA [NASA MFRP NNX06AE32G, NNG05GQ46G] FX We gratefully acknowledge financial support from the NASA Mars Fundamental Research Program (NASA MFRP NNX06AE32G) and the NASA Mars Data Analysis Program (NNG05GQ46G). We thank Vic Baker and Alfred McEwen for reviews which significantly improved the manuscript. We are also grateful to Caleb Fassett and James Dickson for their technical contribution to the preparation of the manuscript and useful insights during scientific discussions. NR 91 TC 8 Z9 8 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JAN PY 2011 VL 211 IS 1 BP 347 EP 365 DI 10.1016/j.icarus.2010.08.004 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709MK UT WOS:000286443600025 ER PT J AU Watters, WA Grotzinger, JP Bell, J Grant, J Hayes, AG Li, RX Squyres, SW Zuber, MT AF Watters, Wesley A. Grotzinger, John P. Bell, James, III Grant, John Hayes, Alex G. Li, Rongxing Squyres, Steven W. Zuber, Maria T. TI Origin of the structure and planform of small impact craters in fractured targets: Endurance Crater at Meridiani Planum, Mars SO ICARUS LA English DT Article DE Impact processes; Mars, Surface; Geological processes ID BURNS FORMATION; METEOR CRATER; LANDING SITE; OPPORTUNITY; EXPLORATION; ARIZONA; EJECTA; SOILS AB We present observations and models that together explain many hallmarks of the structure and growth of small impact craters forming in targets with aligned fractures. Endurance Crater at Meridiani Planum on Mars (diameter approximate to 150 m) formed in horizontally-layered aeolian sandstones with a prominent set of wide, orthogonal joints. A structural model of Endurance Crater is assembled and used to estimate the transient crater planform. The model is based on observations from the Mars Exploration Rover Opportunity: (a) bedding plane orientations and layer thicknesses measured from stereo image pairs; (b) a digital elevation model of the whole crater at 0.3 m resolution; and (c) color image panoramas of the upper crater walls. This model implies that the crater's current shape was mostly determined by highly asymmetric excavation rather than long-term wind-mediated erosion. We show that modal azimuths of conjugate fractures in the surrounding rocks are aligned with the square component of the present-day crater planform, suggesting excavation was carried farther in the direction of fracture alignments. This was previously observed at Barringer Crater in Arizona and we show the same relationship also holds for Tswaing Crater in South Africa. We present models of crater growth in which excavation creates a "stellate" transient cavity that is concave-cuspate in planform. These models reproduce the "lenticular-crescentic" layering pattern in the walls of some polygonal impact craters such as Endurance and Barringer Craters, and suggest a common origin for tear faults and some crater rays. We also demonstrate a method for detailed error analysis of stereogrammetric measurements of bedding plane orientations. (C) 2010 Elsevier Inc. All rights reserved. C1 [Watters, Wesley A.; Bell, James, III; Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Grotzinger, John P.; Hayes, Alex G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Grant, John] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. [Li, Rongxing] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Watters, WA (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM wesley.andres.watters@gmail.com RI Hayes, Alexander/P-2024-2014 OI Hayes, Alexander/0000-0001-6397-2630 NR 55 TC 13 Z9 13 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JAN PY 2011 VL 211 IS 1 BP 472 EP 497 DI 10.1016/j.icarus.2010.08.030 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 709MK UT WOS:000286443600032 ER PT J AU Buzas-Stephens, P Buzas, MA Ellioti, BA AF Buzas-Stephens, Pamela Buzas, Martin A. Ellioti, Brent A. TI FORAMINIFERAL POPULATION RESPONSE TO FLUCTUATING INFLOW INTO NUECES BAY, TEXAS SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID FRESH-WATER INFLOW; BENTHIC FORAMINIFERA; POLLUTION SOURCES; HEAVY-METALS; ESTUARIES; SCALE AB Freshwater input into Texas estuaries is critical to maintaining habitat, and foraminiferal populations can provide a means for assessing the effects of natural inflow as well as mandated releases. Nueces Bay receives freshwater from the Nueces River, which enters on the southwest shore. From 2002-2007 foraminifera were sampled on a mid-bay, north-south transect at five different stations. The populations were sampled during periods of low inflow (2002), high inflow (2003), and then low/moderate inflow (2007). During low inflow, the Central Power and Lighting Plant (CPL) was in operation at the south shore, pumping heated, more saline coolant water into the bay. Salinities were nearly constant, ranging from 23-27 at the stations, population densities were low, and there was a high incidence of shell dissolution. The high-inflow samples were taken after the CPL closed and the area received abundant precipitation, with salinities in the bay varying from 12 at the south shore to 21 at the north shore. Foraminiferal abundance was 6-98X greater than it was during low inflow, and there was a low percentage of shell dissolution. With lowmoderate inflow, salinities were from 21-30, densities were somewhat higher than those observed during low inflow, and shell dissolution again increased. Statistical analysis of all three discharge periods shows that population density varies with flow regime. At low and low/moderate discharge there are pronounced density differences among the stations, with higher densities near river input. At high discharge, population density is high at each station. This study establishes the receptivity of foraminifera to relatively short-term changes in freshwater inflow, and highlights their value for monitoring the effects of inflow on biota in Texas estuaries. The unique geographic distribution of each species may be a characteristic that imparts species resilience through time. C1 [Buzas-Stephens, Pamela; Ellioti, Brent A.] Midwestern State Univ, Dept Geosci, Wichita Falls, TX 76310 USA. [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. RP Buzas-Stephens, P (reprint author), Midwestern State Univ, Dept Geosci, 3410 Taft Blvd, Wichita Falls, TX 76310 USA. EM pamela.stephens@mwsu.edu FU Midwestern State University FX The authors would like to thank William Stephens, Ian Stephens, and C. Jerry Bowen for help with sampling. This work was partially supported through University and College Grants from Midwestern State University. NR 33 TC 6 Z9 6 U1 1 U2 3 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JAN PY 2011 VL 41 IS 1 BP 14 EP 21 DI 10.2113/gsjfr.41.1.14 PG 8 WC Paleontology SC Paleontology GA 710WB UT WOS:000286546600003 ER PT J AU Ge, BM Guan, TP Powell, D McShea, WJ Song, YL AF Ge, Bao-Ming Guan, Tian-Pei Powell, David McShea, William J. Song, Yan-Ling TI Effects of an earthquake on wildlife behavior: a case study of takin (Budorcas taxicolor) in Tangjiahe National Nature Reserve, China SO ECOLOGICAL RESEARCH LA English DT Article DE Home range; Behavior; Migration; Movement; Takin; Tangjiahe ID FEMALE SIKA-DEER; PLANT PHENOLOGY; QINLING MOUNTAINS; EASTERN HOKKAIDO; GOLDEN TAKIN; HOME-RANGE; MIGRATION; PREDICTION; MOVEMENTS; BENEFITS AB The question of whether large-scale disturbances, such as earthquakes, impact an animal's behavior significantly is an important question, but one that is difficult to answer due to the unpredictability of these types of events. Here, we collected 323 GPS locations of four takin (Budorcas taxicolor tibetana) in 13 days before and after a powerful (8.0 magnitude) earthquake on May 12, 2008 in Sichuan Province, China. The movement during this period was compared to that of three of the same animals during a corresponding period in 2009 (April 30 to May 25) and a slightly later 2009 period based on the start of migration (May 6 to May 31). We found that home ranges reduced in size during each study period, due to the migration process, but with no discernable differences due to the earthquake. The takin also showed the same pattern of elevation change and linear travel distance during 2008 and 2009, indicating no detectable effect of the earthquake on spatial behavior of takin. These findings add to our knowledge of how animals respond to catastrophic natural events in the wild. C1 [Ge, Bao-Ming; Song, Yan-Ling] Chinese Acad Sci, Key Lab Anim Ecol & Conservat Biol, Inst Zool, Beijing 100101, Peoples R China. [Ge, Bao-Ming] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Guan, Tian-Pei] Beijing Normal Univ, Coll Life Sci, Beijing 100875, Peoples R China. [Powell, David] Bronx Zoo, Dept Mammal, Wildlife Conservat Soc, Bronx, NY 10460 USA. [McShea, William J.] Natl Zool Pk, Smithsonians Conservat Biol Inst, Front Royal, VA 22630 USA. RP Song, YL (reprint author), Chinese Acad Sci, Key Lab Anim Ecol & Conservat Biol, Inst Zool, Beijing 100101, Peoples R China. EM songyl@ioz.ac.cn RI Ge, Bao-Ming/F-4827-2011 FU National Zoo; National Geographic Society; Columbus Zoo; Potawatomi Zoo; Ocean Park Hong Kong; Chinese Academy of Science [KSCX2-YW-Z-0959]; The Wilds FX This work was supported by the National Zoo, National Geographic Society, Columbus Zoo, Potawatomi Zoo, Ocean Park Hong Kong, the Chinese Academy of Science (KSCX2-YW-Z-0959) and The Wilds. We thank Sheng Li, Xiao-Gen Liu, Li-Min Chen, Wen-Hu Ma, Zhong-Huai Zhang, Jun Yang, and all the other staff of Tangjiahe National Nature Reserve for their help when we worked there. We thank the Evan S. Blumer and Barbara Wolfe from The Wilds for their help to anaesthetize and collar the animals; and Yi Tao, Zhi-Gao Zeng, and Qiong Zhang for recommendations on the earlier manuscript. The authors appreciated Dr. Bram Van Moorter and Dr. Roel May for their valuable comments. All experimental procedures on animals were licensed by the Animal Care and Use Committee of the Institute of Zoology, Chinese Academy of Sciences, and all animal work was approved by State Forestry Administration, People's Republic of China. NR 33 TC 1 Z9 2 U1 4 U2 39 PU SPRINGER TOKYO PI TOKYO PA 1-11-11 KUDAN-KITA, CHIYODA-KU, TOKYO, 102-0073, JAPAN SN 0912-3814 J9 ECOL RES JI Ecol. Res. PD JAN PY 2011 VL 26 IS 1 BP 217 EP 223 DI 10.1007/s11284-010-0759-2 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 709IO UT WOS:000286431900023 ER PT J AU DiMichele, WA Looy, CV Chaney, DS AF DiMichele, William A. Looy, Cindy V. Chaney, Dan S. TI A NEW GENUS OF GIGANTOPTERID FROM THE MIDDLE PERMIAN OF THE UNITED STATES AND CHINA AND ITS RELEVANCE TO THE GIGANTOPTERID CONCEPT SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE gigantopterid; Permian; Gigantopteridium; Euparyphoselis; cuticle ID NORTH-CENTRAL TEXAS; GUIZHOU PROVINCE; WEST TEXAS; PLANT; FLORA; GIGANTONOCLEA; AFFINITIES; ANATOMY; COUNTY; NOV. AB The gigantopterids are a poorly understood group of plants defined primarily on the basis of a particular type of reticulate leaf venation in combination with stratigraphic distribution. It is generally agreed that many, if not all, are seed plants. A new genus of gigantopterid, Euparyphoselis gen. nov., is described from foliage only, derived from the Middle Permian of the southwestern United States and eastern China. One species occurs in each area: Euparyphoselis gibsonii sp. nov. in the United States and Euparyphoselis marginervum (Yao and Liu) comb. nov. in China. The most significant characteristic of the new genus is a marginal vein. The foliage displays three and occasionally four orders of venation, with a variably distinct suture vein between second-order veins, formed by the fusion of tertiary veins from adjacent secondaries. The leaves are obovate in shape and unforked, tapering toward the base. Leaf margins are smooth or bluntly toothed with broad, shallow sinuses between the teeth. Secondary veins end or dissipate into the teeth, where present. Leaves are amphistomatic; stomatal complexes are haplocheilic and monocyclic. The two species differ mainly in the characteristics of the epidermal surfaces, including the shape and size of the epidermal and subsidiary cells, stomatal complexes, number of subsidiary cells, orientation of the stomatal complexes, and secretory structures. Euparyphoselis marginervum was originally described as a species of Gigantopteridium, with which it shares certain characteristics of venation. However, it clearly differs from Gigantopteridium in the details of venation and in leaf architecture. It is argued that leaf venation should not be given primacy over all other characteristics when assessing gigantopterid relationships and therefore as a basis for taxonomy. As previously suggested, the gigantopterids, as presently construed, may not be a monophyletic group. C1 [DiMichele, William A.; Chaney, Dan S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Looy, Cindy V.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM dimichel@si.edu RI DiMichele, William/K-4301-2012 FU Smithsonian Institution FX We thank Mike Gibson of the 6666 Ranch in Guthrie, Texas, for permission to examine the fossiliferous exposures and for his generous assistance with this study. We also thank the late Sergius Mamay for his insights into gigantopterid morphology, without which this study could not have been completed, and Wang Jun for help with access to the Chinese literature. Scott Whittaker, NMNH, provided assistance with SEM. Robert Hook, Austin, Texas, provided assistance with fieldwork and geological characterization of the collecting site. Ian Glasspool, Jason Hilton, and an anonymous reviewer provided most helpful critical comments on an earlier draft of the manuscript. This work was supported by the Research Endowment Fund of the Smithsonian Institution. NR 26 TC 5 Z9 5 U1 0 U2 34 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 JAN PY 2011 VL 172 IS 1 BP 107 EP 119 DI 10.1086/657276 PG 13 WC Plant Sciences SC Plant Sciences GA 708RD UT WOS:000286381100007 ER PT J AU Connahs, H Aiello, A Van Bael, S Rodriguez-Castaneda, G AF Connahs, Heidi Aiello, Annette Van Bael, Sunshine Rodriguez-Castaneda, Genoveva TI Caterpillar abundance and parasitism in a seasonally dry versus wet tropical forest of Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE canopy; Diptera; external feeders; Hymenoptera; parasitoids; rainfall; shelter builders ID CLIMATE-CHANGE; PRECIPITATION GRADIENT; HERBIVORE OUTBREAK; INSECT HERBIVORY; NATURAL ENEMIES; RAINFALL; CANOPY; LEAF; CONSEQUENCES; FLUCTUATIONS AB Rainfall seasonality can strongly influence biotic interactions by affecting host plant quality, and thus potentially regulating herbivore exposure to natural enemies. Plant defences are predicted to increase from dry to wet forests, rendering wet-forest caterpillars more vulnerable to parasitoids due to the slow-growth-high-mortality hypothesis. We collected and reared caterpillars from the understorey and trail edges of a wet forest and a seasonally dry forest to determine whether wet-forest caterpillars suffered a higher prevalence of parasitism and were less abundant than dry-forest caterpillars. In the two forests, caterpillar abundances (on average 8 h(-1)) and prevalence of parasitism (18%) were very similar regardless of feeding niche for both parasitism (27% versus 29% in shelter builders, and 16% versus 11% in external feeders) and caterpillar abundances (shelter builders: 1.42 versus 2.39, and external feeders: 8.27 versus 5.49 caterpillars h(-1)) in the dry and wet forests, respectively. A similar comparative analysis conducted in the canopy and understorey of the dry forest revealed a higher prevalence of parasitism in the canopy (43%) despite caterpillar densities similar to those in the understorey. Overall, shelter builders suffered higher parasitism than external feeders (32% versus 14.9%), and were attacked primarily by flies, whereas external feeders were more vulnerable to attack by parasitoid wasps. C1 [Connahs, Heidi] Univ N Dakota, Dept Biol, Grand Forks, ND 58202 USA. [Connahs, Heidi; Aiello, Annette; Van Bael, Sunshine] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Rodriguez-Castaneda, Genoveva] Umea Univ, Landscape Ecol Lab, SE-09187 Umea, Sweden. RP Connahs, H (reprint author), Univ N Dakota, Dept Biol, Grand Forks, ND 58202 USA. EM hconnahs@gmail.com FU Smithsonian Tropical Research Institute FX This research was funded in part by a short-term fellowship to H. Connahs from the Smithsonian Tropical Research Institute. Thanks also to E. A. Herre who funded part of this research and E. Teppe who assisted with Piper identifications. We are also grateful to an anonymous reviewer whose comments improved the manuscript. NR 43 TC 8 Z9 9 U1 4 U2 36 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2011 VL 27 BP 51 EP 58 DI 10.1017/S0266467410000568 PN 1 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 700FD UT WOS:000285722500005 ER PT J AU Wester, S Zotz, G AF Wester, Stefan Zotz, Gerhard TI Seed comas of bromeliads promote germination and early seedling growth by wick-like water uptake SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Catopsis sessiliflora; germination; growth; plant water relations; regeneration niche; seed morphology ID DISPERSAL; EPIPHYTE C1 [Wester, Stefan; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Inst Biol & Environm Sci, AG Funct Ecol, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Biol & Environm Sci, AG Funct Ecol, Box 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 19 TC 7 Z9 7 U1 0 U2 4 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 EI 1469-7831 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2011 VL 27 BP 115 EP 119 DI 10.1017/S0266467410000593 PN 1 PG 5 WC Ecology SC Environmental Sciences & Ecology GA 700FD UT WOS:000285722500014 ER PT S AU Wilson, RW AF Wilson, Robert W. BE Koch, M TI Millimeter and Sub-millimeter Wave Technology for Astronomy: From Early Bell Labs Work to ALMA SO 2011 36TH INTERNATIONAL CONFERENCE ON INFRARED, MILLIMETER, AND TERAHERTZ WAVES (IRMMW-THZ) SE International Conference on Infrared Millimeter and Terahertz Waves LA English DT Proceedings Paper CT 36th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz) CY OCT 02-07, 2011 CL Houston, TX SP Rice Univ, IEEE Microwave Theory & Tech Soc, NASA, California Inst Technol, Jet Prop Lab, Univ Wollongong ID TUNNEL-JUNCTIONS AB Bell Labs was an early developer of millimeter-wave technology. At the peak of its development there, Arno Penzias, Keith Jefferts and I were privileged to use it to discover CO in what turned out to be star forming interstellar clouds. Interest in mm and sub-mm wave astronomy has blossomed since. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilson, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2162-2027 BN 978-1-4577-0509-0 J9 INT CONF INFRA MILLI PY 2011 PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BJT73 UT WOS:000330296300028 ER PT S AU Cass, CAP Hazari, Z Sadler, PM Sonnert, G AF Cass, Cheryl A. P. Hazari, Zahra Sadler, Philip Michael Sonnert, Gerhard GP ASEE TI ENGINEERING PERSISTERS AND NON-PERSISTERS: UNDERSTANDING INFLOW AND OUTFLOW TRENDS BETWEEN MIDDLE SCHOOL AND COLLEGE SO 2011 ASEE ANNUAL CONFERENCE & EXPOSITION SE ASEE Annual Conference & Exposition LA English DT Proceedings Paper CT ASEE Annual Conference and Exposition CY JUN 26-29, 2011 CL Vancouver, CANADA SP ASEE DE engineering pipeline; persistence; science identity ID OF-THE-LITERATURE; SCIENCE; IDENTITY; STUDENTS; PARTICIPATION; ASPIRATIONS; PHYSICS; GENDER AB A science identity framework was applied to discern how pre-college science experiences can affect persistence in engineering career trajectories. Engineering persisters (n=751) and non-persisters (n=528) were isolated from a nationally-representative dataset, and groups were compared against a number of self-reported factors associated with performance, competence, recognition, and interest in science. Results demonstrated that persisters reported significantly higher values for factors that contribute to science identity formation, particularly in physics. It was concluded that physics courses can be used as arenas in which to develop science identity, with the ultimate goal of increasing inflow and persistence in engineering career paths. C1 [Cass, Cheryl A. P.] Clemson Univ, Dept Engn & Sci Educ, Clemson, SC 29631 USA. [Hazari, Zahra] Clemson Univ, Dept Engn & Sci Educ, Dept Math Sci, Clemson, SC 29631 USA. [Sadler, Philip Michael] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Cass, CAP (reprint author), Clemson Univ, Dept Engn & Sci Educ, Clemson, SC 29631 USA. NR 42 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC ENGINEERING EDUCATION PI WASHINGTON PA 1818 N STREET, NW SUITE 600, WASHINGTON, DC 20036 USA SN 2153-5965 J9 ASEE ANNU CONF EXPO PY 2011 PG 16 WC Education & Educational Research; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Education & Educational Research; Engineering GA BF0CG UT WOS:000378522705070 ER PT S AU Chang, GQ Li, CH Phillips, DF Walsworth, RL Kartner, FX AF Chang, Guoqing Li, Chih-Hao Phillips, David F. Walsworth, Ronald L. Kaertner, Franz X. GP IEEE TI Broadband, large-spacing frequency-comb employing complementary interleavers for mode filtering SO 2011 CONFERENCE ON LASERS AND ELECTRO-OPTICS (CLEO) SE Conference on Lasers and Electro-Optics LA English DT Proceedings Paper CT Conference on Lasers and Electro-Optics (CLEO) CY MAY 01-06, 2011 CL Baltimore, MD ID CALIBRATION; PRECISION AB We propose and analyze an approach to generate broadband large-spacing frequency-combs using complementary interleavers for mode-filtering and nonlinear fibers for spectral broadening. 350-nm bandwidth with negligible side-mode asymmetry is achieved. (C) 2011 Optical Society of America C1 [Chang, Guoqing; Kaertner, Franz X.] MIT, Elect Res Lab, 77 Mass Ave, Cambridge, MA 02139 USA. [Li, Chih-Hao; Phillips, David F.; Walsworth, Ronald L.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chang, GQ (reprint author), MIT, Elect Res Lab, 77 Mass Ave, Cambridge, MA 02139 USA. EM guoqing@mit.edu NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2160-9020 BN 978-1-55752-910-7 J9 CONF LASER ELECTR PY 2011 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BXB77 UT WOS:000295612402220 ER PT S AU Chang, GQ Li, CH Phillips, DF Walsworth, RL Kartner, FX AF Chang, Guoqing Li, Chih-Hao Phillips, David F. Walsworth, Ronald L. Kaertner, Franz X. GP IEEE TI Power amplification of astro-combs: optimization of filtering schemes SO 2011 CONFERENCE ON LASERS AND ELECTRO-OPTICS (CLEO) SE Conference on Lasers and Electro-Optics LA English DT Proceedings Paper CT Conference on Lasers and Electro-Optics (CLEO) CY MAY 01-06, 2011 CL Baltimore, MD ID FREQUENCY COMBS; CALIBRATION; PRECISION AB We develop an analytical approach to analyze the performance of astro-combs when amplified by a fiber amplifier. Five filtering schemes are compared to optimize side-mode suppression and radial-velocity calibration accuracy of an amplified astro-comb. (C) 2011 Optical Society of America C1 [Chang, Guoqing; Kaertner, Franz X.] MIT, Elect Res Lab, 77 Mass Ave, Cambridge, MA 02139 USA. [Li, Chih-Hao; Phillips, David F.; Walsworth, Ronald L.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Chang, GQ (reprint author), MIT, Elect Res Lab, 77 Mass Ave, Cambridge, MA 02139 USA. EM guoqing@mit.edu NR 6 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2160-9020 BN 978-1-55752-910-7 J9 CONF LASER ELECTR PY 2011 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BXB77 UT WOS:000295612402219 ER PT J AU Vallo, P Benda, P Martinkova, N Kanuch, P Kalko, EKV Cerveny, J Koubek, P AF Vallo, Peter Benda, Petr Martinkova, Natalia Kanuch, Peter Kalko, Elisabeth K. V. Cerveny, Jaroslav Koubek, Petr TI Morphologically uniform bats Hipposideros aff. ruber (Hipposideridae) exhibit high mitochondrial genetic diversity in southeastern Senegal SO ACTA CHIROPTEROLOGICA LA English DT Article DE cytochrome b; Hipposideros caffer complex; cryptic species; phylogeny ID ECHOLOCATION CALLS; PHYLOGENETIC INFERENCE; TAXONOMIC IMPLICATIONS; CRYPTIC DIVERSITY; EUROPEAN BATS; CHIROPTERA; DNA; EVOLUTION; DIVERGENCE; MAMMALS AB Two mitochondrial lineages of bats that are morphologically attributed to Hipposideros ruber have been shown to occur sympatrically in southeastern Senegal. We studied genetic diversity in these bats in the Niokolo Koba National Park using sequences of mitochondrial cytochrome b gene to determine the taxonomic status of the two genetic forms, and included skull morphology for comparison. Detailed multidimensional analysis of skull measurements indicated slight morphological differences between the two genetic forms. Exploration of peak frequency of the constant-frequency echolocation signals in a local population of Hipposideros aff. ruber was not available for both groups. Phylogenetic comparison with other available West African representatives of H. aff. ruber revealed paraphyletic relationship of the two Senegalese forms, with the less abundant form from Senegal forming a monophyletic group with that from Benin. Based on genetic divergence and sympatric occurrence, the two forms from Senegal might represent cryptic species. However, absence of nuclear gene flow between them is yet to be investigated to demonstrate their reproductive isolation. C1 [Vallo, Peter; Martinkova, Natalia; Kanuch, Peter; Cerveny, Jaroslav; Koubek, Petr] Acad Sci Czech Republic, Inst Vertebrate Biol, CS-60365 Brno, Czech Republic. [Benda, Petr] Natl Museum Nat Hist, Dept Zool, Prague 11579 1, Czech Republic. [Benda, Petr] Charles Univ Prague, Dept Zool, CR-12844 Prague 2, Czech Republic. [Martinkova, Natalia] Masaryk Univ, Inst Biostat & Anal, Brno 62500, Czech Republic. [Kanuch, Peter] Slovak Acad Sci, Inst Forest Ecol, Zvolen 96053, Slovakia. [Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Cerveny, Jaroslav; Koubek, Petr] Czech Univ Life Sci, Fac Forestry & Wood Sci, Dept Forest Protect & Game Management, Prague 16521 6, Czech Republic. RP Vallo, P (reprint author), Acad Sci Czech Republic, Inst Vertebrate Biol, Kvetna 8, CS-60365 Brno, Czech Republic. EM vallo@ivb.cz RI Martinkova, Natalia/C-2939-2008; Benda, Petr/B-5437-2011; Vallo, Peter/F-9650-2014; Koubek, Petr/G-1110-2014; Cerveny, Jaroslav/A-2809-2015; Kanuch, Peter/A-5416-2011; OI Martinkova, Natalia/0000-0003-4556-4363; Kanuch, Peter/0000-0003-2001-4541 FU Grant Agency of the Academy of Sciences of the Czech Republic [IAA6093404]; Ministry of Culture of the Czech Republic [MK00002327201] FX We thank Adam Konecny Josef Bryja and other colleagues from the Institute of Vertebrate Biology AS CR, v.v.i., Brno, for their assistance in capturing of bats in Senegal. Field work in the NKNP and collecting of bat specimens was approved and supervised by the Direction des Pares Nationaux du Senegal, Dakar, and we thank the director Col. Manic Balla Gueye for his kind support. Further we thank Burton Lim (Royal Ontario Museum, Toronto, Canada) for providing tissue samples of bats from Ivory Coast, and Christian Drosten (University of Bonn Medical Centre, Germany) and his team for acquiring samples from Ghana within the project 01KI0701 by the German Federal Ministry of Education and Research. This study was supported by the grant No. IAA6093404 of the Grant Agency of the Academy of Sciences of the Czech Republic and grant No. MK00002327201 of the Ministry of Culture of the Czech Republic. We also thank Jakob Fahr (University of Ulm, Germany) for critical comments and suggestions on the manuscript. NR 40 TC 8 Z9 9 U1 0 U2 7 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2011 VL 13 IS 1 BP 79 EP 88 DI 10.3161/150811011X578633 PG 10 WC Zoology SC Zoology GA 776YV UT WOS:000291578100006 ER PT S AU Eberhard, WG Wcislo, WT AF Eberhard, William G. Wcislo, William T. BE Casas, J TI Grade Changes in Brain-Body Allometry: Morphological and Behavioural Correlates of Brain Size in Miniature Spiders, Insects and Other Invertebrates SO ADVANCES IN INSECT PHYSIOLOGY, VOL 40: SPIDER PHYSIOLOGY AND BEHAVIOUR - PHYSIOLOGY SE Advances in Insect Physiology LA English DT Review; Book Chapter ID ORB-WEAVING SPIDERS; CENTRAL-NERVOUS-SYSTEM; VISUAL-SYSTEM; PLETHODONTID SALAMANDERS; LEUCAUGE-MARIANA; REGENERATED LEGS; SENSORY SYSTEMS; SYNAPTIC NOISE; METABOLIC-RATE; MUSHROOM BODY AB We use a recent wave of data to confirm that Hailer's rule of brain body allometry, for smaller species to have relatively larger brains, holds for invertebrates as well as vertebrates. But different invertebrate taxa fall on several different allometric lines (grades). In the smallest animals in several grades, the brain occupies a large fraction (up to approximately 16%) of the total body mass. The brain and the structures enclosing it show morphological alterations suggesting a lack of housing capacity in the head for the brain (e.g. the brain extends into other parts of the body such as the legs or thorax), and other structures normally enclosed in the same area are displaced. Miniature animals may thus sacrifice some morphological aspects of body design to accommodate their disproportionately large CNS. The smallest animals of one such group, orb web spiders, do not show signs of behavioural limitation in web construction compared with larger relatives. We speculate that, because of selection resulting from the high metabolic costs of nervous tissue, grade changes may involve substantial modifications of how brains function, and help explain differences between neuron-profligate vertebrates and invertebrates having far fewer neurons (as few as approximately 200-500 neurons in two groups). Scaling problems associated with small size are of general importance, because many moderate-sized animals have very small free-living immature stages. C1 [Eberhard, William G.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 211 TC 21 Z9 21 U1 5 U2 31 PU ACADEMIC PRESS LTD-ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL ROAD, LONDON NW1 7DX, ENGLAND SN 0065-2806 BN 978-0-12-387668-3 J9 ADV INSECT PHYSIOL JI Adv. Insect Physiol. PY 2011 VL 40 BP 155 EP 214 DI 10.1016/B978-0-12-387668-3.00004-0 PG 60 WC Entomology SC Entomology GA BYM03 UT WOS:000299298700004 ER PT J AU Plath, M Mody, K Potvin, C Dorn, S AF Plath, Mirco Mody, Karsten Potvin, Catherine Dorn, Silvia TI Do multipurpose companion trees affect high value timber trees in a silvopastoral plantation system? SO AGROFORESTRY SYSTEMS LA English DT Article DE Cedrela odorata; Multipurpose companion trees; REDD; Silvopastoral systems; Tabebuia rosea; Timber tree performance ID HYPSIPYLA-GRANDELLA LEPIDOPTERA; BIOLOGICAL NITROGEN-FIXATION; MAHOGANY SHOOT BORER; TROPICAL PASTURE; BIODIVERSITY EXPERIMENT; LEUCAENA-LEUCOCEPHALA; FOREST PLANTATIONS; GLIRICIDIA-SEPIUM; SPECIES RICHNESS; HUMID TROPICS AB Establishment of native timber trees on deforested land may contribute to the livelihood of farmers, to improved ecosystem services and to increased greenhouse gas uptake. Here, we present a new silvopastoral planting design to assess species performance and interspecific competition or facilitation effects among native timber and multipurpose trees in Central America. Two timber species, Tabebuia rosea and Cedrela odorata, were established in three low-density planting regimes allowing combined tree and future livestock production: (1) solitary planting, (2) companion planting with Guazuma ulmifolia, and (3) companion planting with the nitrogen-fixing Gliricidia sepium. We quantified survival, growth and reforestation potential of the two timber species subjected to the different planting regimes for the first 2 years after establishment. Nitrogen concentration as well as stable nitrogen and carbon isotope composition (delta N-15, delta C-13) of leaves of the timber saplings were determined. T. rosea showed higher survival and better growth than C. odorata under varying environmental conditions (soil, concomitant vegetation). Performance of the timber saplings was unaffected by either companion species. Planting regimes had no effect on foliar nitrogen concentration and delta N-15 of the two timber species, although delta N-15 values indicated nitrogen fixation activity in G. sepium trees. Planting regimes affected foliar delta C-13 values in T. rosea. delta C-13 values were significantly higher in solitarily growing individuals, suggesting lower exposition to water stress conditions in saplings surrounded by companion species. As we found positively correlated growth traits among timber and multipurpose trees, a combined planting may benefit farmers by providing additional goods and services. C1 [Plath, Mirco; Mody, Karsten; Dorn, Silvia] ETH, Inst Plant Anim & Agroecosyst Sci, CH-8092 Zurich, Switzerland. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Mody, K (reprint author), ETH, Inst Plant Anim & Agroecosyst Sci, Schmelzbergstr 9,LFO, CH-8092 Zurich, Switzerland. EM mirco.plath@ipw.agrl.ethz.ch; karsten.mody@ipw.agrl.ethz.ch; catherine.potvin@mcgill.ca; silvia.dorn@ipw.agrl.ethz.ch FU ETH North-South Centre FX We acknowledge the support by the Smithsonian Tropical Research Institute in administration and logistics, and of the related Native Species Reforestation Project (PRORENA) providing the tree seedlings. We thank the University of Panama, in particular Hector Barrios, for infrastructure and reliable support. The Panamanian National Environmental Authority (ANAM) granted research, collecting and export permits. The ETH Grassland Science group provided technical equipment for chemical analyses. We thank Nina Buchmann and Sebastian Wolf for valuable interactions, Jose Monteza and all local assistants in Sardinilla for help with fieldwork, and Adriana Najar and an anonymous referee for useful comments on the manuscript. This study has been supported by a grant of the ETH North-South Centre to S.D. and K.M. NR 69 TC 16 Z9 18 U1 1 U2 30 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-4366 J9 AGROFOREST SYST JI Agrofor. Syst. PD JAN PY 2011 VL 81 IS 1 BP 79 EP 92 DI 10.1007/s10457-010-9308-9 PG 14 WC Agronomy; Forestry SC Agriculture; Forestry GA 689TX UT WOS:000284953600008 ER PT S AU Lentz, RCF McCoy, TJ Collins, LE Corrigan, CM Benedix, GK Taylor, GJ Harvey, RP AF Lentz, R. C. F. McCoy, T. J. Collins, L. E. Corrigan, C. M. Benedix, G. K. Taylor, G. J. Harvey, R. P. BE Garry, WB Bleacher, JE TI Theo's Flow, Ontario, Canada: A terrestrial analog for the Martian nakhlite meteorites SO ANALOGS FOR PLANETARY EXPLORATION SE Geological Society of America Special Papers LA English DT Article; Book Chapter ID MUNRO-TOWNSHIP; MAGMA; MARS AB Martian meteorites provide our only samples for laboratory investigations of Mars, yet the lack of geologic context severely limits their utility. Strong petrologic similarities between the pyroxenitic layer of a 120-m-thick, mafic Archean lava flow in Ontario, Canada, called Theo's Flow, and the nakhlite meteorite group may elucidate geologic processes that operated on Mars. Theo's Flow is in the Abitibi greenstone belt, an area that is well known as a komatiite location. The type locality, and best outcrop, of Theo's Flow is an upturned (similar to 70 degrees) section stretching east-west for similar to 500 m. Theo's Flow can be divided into distinct lithologic units: a thin basal peridotite (0-9 m), a thick pyroxenite (50-60 m), a gabbro (35-40 m), and a hyaloclastic, brecciated top (8-10 m). It is the thick pyroxenitic layer that bears a striking textural similarity to the Martian nakhlites. Serpentinization of olivine, chloritization of orthopyroxene, and alteration (e. g., pseudomorphic replacement) of plagioclase and minor phases have transformed the original mineral assemblage, though augites remain largely unaltered, and textural relationships are well preserved throughout the flow. Variations in iron and minor-element abundances in augite cores exhibit typical trends for an evolving melt. Bulk rock analyses exhibit elemental trends consistent with an evolving melt, though they exhibit evidence of elemental remobilization by later metamorphism. An average of the peridotite, pyroxenite, and gabbro compositions compares well to that of the quenched top hyaloclastite, suggesting it is a single flow that was differentiated by crystal settling. The lithologic diversity within Theo's Flow suggests that nakhlites may also have complementary lithologies that remain unsampled. C1 [Lentz, R. C. F.; Taylor, G. J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [McCoy, T. J.; Collins, L. E.; Corrigan, C. M.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. [Collins, L. E.] Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. [Benedix, G. K.] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. [Harvey, R. P.] Case Western Reserve Univ, Dept Geol, Cleveland, OH 44106 USA. RP Lentz, RCF (reprint author), St Andrews Priory Sch, 224 Queen Emma Sq, Honolulu, HI 96813 USA. OI Benedix, Gretchen/0000-0003-0990-8878 NR 26 TC 8 Z9 8 U1 0 U2 1 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2483-6 J9 GEOL SOC AM SPEC PAP PY 2011 VL 483 BP 263 EP 277 DI 10.1130/2011.2483(17) D2 10.1130/9780813724836 PG 15 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BHX33 UT WOS:000326925100018 ER PT S AU Williams, RME Irwin, RP Zimbelman, JR Chidsey, TC Eby, DE AF Williams, Rebecca M. E. Irwin, Rossman P., III Zimbelman, James R. Chidsey, Thomas C., Jr. Eby, David E. BE Garry, WB Bleacher, JE TI Field guide to exhumed paleochannels near Green River, Utah: Terrestrial analogs for sinuous ridges on Mars SO ANALOGS FOR PLANETARY EXPLORATION SE Geological Society of America Special Papers LA English DT Article; Book Chapter ID ALLUVIAL CHANNEL PATTERN; MORRISON FORMATION; COLORADO PLATEAU; RECONNAISSANCE ORBITER; SEDIMENT TRANSPORT; MARTIAN HIGHLANDS; VALLES MARINERIS; DEPOSITS; CRATER; SURFACE AB Multiple cemented channel-fill deposits from the Late Jurassic and Early Cretaceous, once buried beneath 2400 m of sediment, are now exposed at the surface in arid east-central Utah due to erosion of the less resistant surrounding material. This field guide focuses on examples near the town of Green River where there is public access to several different types of exhumed paleochannels within a small geographic region. We describe the geologic setting of these landforms based on previous work, discuss the relevance to analogous sinuous ridges that are interpreted to be inverted paleochannels on Mars, and present a detailed road log with descriptive stops in Emery County, Utah. C1 [Williams, Rebecca M. E.; Irwin, Rossman P., III] Planetary Sci Inst, Tucson, AZ 85179 USA. [Zimbelman, James R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Chidsey, Thomas C., Jr.] Utah Geol & Min Survey, Salt Lake City, UT 84114 USA. [Eby, David E.] Eby Petrog & Consulting, Denver, CO 80204 USA. RP Williams, RME (reprint author), Planetary Sci Inst, 1700 East Ft Lowell Rd,Suite 106, Tucson, AZ 85179 USA. NR 132 TC 3 Z9 3 U1 0 U2 0 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2483-6 J9 GEOL SOC AM SPEC PAP PY 2011 VL 483 BP 483 EP 505 DI 10.1130/2011.2483(29) D2 10.1130/9780813724836 PG 23 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BHX33 UT WOS:000326925100030 ER PT J AU Senda, A Kobayashi, R Fukuda, K Saito, T Hood, WR Kunz, TH Oftedal, OT Urashima, T AF Senda, Akitsugu Kobayashi, Rui Fukuda, Kenji Saito, Tadao Hood, Wendy R. Kunz, Thomas H. Oftedal, Olav T. Urashima, Tadasu TI Chemical characterization of milk oligosaccharides of the island flying fox (Pteropus hypomelanus) (Chiroptera: Pteropodidae) SO ANIMAL SCIENCE JOURNAL LA English DT Article DE bat; Chiroptera; island flying fox; milk oligosaccharides; Pteropidae ID COLOSTRUM; LACTATION; BATS AB Although a considerable amount of information has accumulated about oligosaccharides in the milk and colostrum of representatives of various mammalian orders, nothing is so far known concerning these sugars in the milk of any bat species (order Chiroptera). In this study, we determined that the following oligosaccharides occur in milk of the island flying fox, Pteropus hypomelanus (Chiroptera: Pteropidae): Gal(a13)Gal(beta 14)Glc (isoglobotriose), Gal(beta 14)GlcNAc(beta 13)Gal(beta 14)Glc (lacto-N-neotetraose), Gal(beta 14)GlcNAc(beta 13)[Gal(eta 14)GlcNAc(beta 16)]Gal(beta 14)Glc (lacto-N-neohexaose) and Neu5Gc(a23)Gal(beta 14)Glc (3'-NGc-SL). However, lactose was found to be the dominant saccharide in this milk, as in most eutherian mammals. The biologic importance of oligosaccharides in Chiropteran milks warrants further study. C1 [Senda, Akitsugu; Fukuda, Kenji; Urashima, Tadasu] Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Kobayashi, Rui] Obihiro Univ Agr & Vet Med, Dept Bioresource Chem, Obihiro, Hokkaido 0808555, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Aoba Ku, Sendai, Miyagi 980, Japan. [Hood, Wendy R.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Kunz, Thomas H.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. EM urashima@obihiro.ac.jp FU Ministry of Education, Culture, Sports, Science, and Technology, Japan; Lubee Foundation FX This study was partially supported from a grant from Global COE Program 'Frontier Program for Animal Global Health and Hygiene', Ministry of Education, Culture, Sports, Science, and Technology, Japan. We thank J. Seyjagat and the Lubee Foundation for supporting this research by permitting the collection of milk and providing a grant to T. H. Kunz for this purpose. We also acknowledge the assistance of keepers at the Lubee Foundation in milk collection and Michael Jakubasz at the Smithsonian National Zoological Park in intial carbohydrate extraction procedures. NR 23 TC 0 Z9 0 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1344-3941 J9 ANIM SCI J JI Anim. Sci. J. PY 2011 VL 82 IS 6 BP 782 EP 786 DI 10.1111/j.1740-0929.2011.00906.x PG 5 WC Agriculture, Dairy & Animal Science SC Agriculture GA 852DT UT WOS:000297329400011 PM 22111635 ER PT S AU Frisch, PC Redfield, S Slavin, JD AF Frisch, Priscilla C. Redfield, Seth Slavin, Jonathan D. BE Faber, SM VanDishoeck, E TI The Interstellar Medium Surrounding the Sun SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, VOL 49 SE Annual Review of Astronomy and Astrophysics LA English DT Review; Book Chapter DE interstellar medium; heliosphere; interstellar dust; magnetic fields; interstellar abundances; exoplanets ID LINE-OF-SIGHT; TURBULENT MIXING LAYERS; HUBBLE-SPACE-TELESCOPE; SPECTROSCOPIC-EXPLORER OBSERVATIONS; SOLAR CHEMICAL-COMPOSITION; INTER-STELLAR MEDIUM; LOCAL BUBBLE; MAGNETIC-FIELD; X-RAY; LOOP-I AB The Solar System is embedded in a flow of low-density, warm, and partially ionized interstellar material that has been sampled directly by in situ measurements of interstellar neutral gas and dust in the heliosphere. Absorption line data reveal that this interstellar gas is part of a larger cluster of local interstellar clouds, which is spatially and kinematically divided into additional small-scale structures indicating ongoing interactions. An origin for the clouds that is related to star formation in the Scorpius-Centaurus OB association is suggested by the dynamic characteristics of the flow. Variable depletions observed within the local interstellar medium (ISM) suggest an inhomogeneous Galactic environment, with shocks that destroy grains in some regions. Although photoionization models of the circumheliospheric ISM do an excellent job of reproducing the observed properties of the surrounding ISM, the unknown characteristics of the very low-density hot plasma filling the Local Bubble introduces uncertainty about the source of ionization and nature of cloud boundaries. Recent observations of small cold clouds provide new insight into the processes affecting the local ISM. A fuller understanding of the local ISM can provide insights into the past and future Galactic environment of the Sun, and deeper knowledge of the astrospheres of nearby stars. C1 [Frisch, Priscilla C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Redfield, Seth] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frisch, PC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM frisch@oddjob.uchicago.edu; sredfield@wesleyan.edu; jslavin@cfa.harvard.edu OI Slavin, Jonathan/0000-0002-7597-6935; Redfield, Seth/0000-0003-3786-3486 NR 151 TC 77 Z9 77 U1 2 U2 26 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2011 VL 49 BP 237 EP 279 DI 10.1146/annurev-astro-081710-102613 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXD57 UT WOS:000295819800007 ER PT S AU Bush, AM Bambach, RK AF Bush, Andrew M. Bambach, Richard K. BE Jeanloz, R Freeman, KH TI Paleoecologic Megatrends in Marine Metazoa SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES, VOL 39 SE Annual Review of Earth and Planetary Sciences LA English DT Review; Book Chapter DE Phanerozoic; predation; diversity; theoretical ecospace; mass extinction; radiation ID PERMIAN MASS EXTINCTION; FOSSIL RECORD; BODY-SIZE; ALPHA-DIVERSITY; THEORETICAL ECOSPACE; PREDATION INTENSITY; ECOSYSTEM ENGINEERS; CAMBRIAN TRANSITION; ADAPTIVE RADIATION; ANIMAL DIVERSITY AB Since their appearance in the Neoproterozoic, marine metazoan ecosystems have increased in ecological diversity, complexity, energy use, motility, predation, infaunality, and biological disturbance. A common theme is an increase in organismal control over internal physiology and the external environment. Often, these changes have been examined in the context of discrete events (e.g., the Cambrian Explosion, Mesozoic Marine Revolution), but they may represent linked, ongoing megatrends. This review examines changes in ecological composition in the context of changes in taxonomic composition, as represented by a more detailed version of Sepkoski's evolutionary fauna analysis. Ecological change occurred during major radiations and extinctions, as well as between them. Due to its ecological selectivity, the Permian-Triassic extinction had particularly significant ecological effects on the biota. Recoveries from mass extinctions may be important episodes of ecological change. Further research could help elucidate the fundamental causes of long-term ecological change, including any role played by the environment. C1 [Bush, Andrew M.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Bush, Andrew M.] Univ Connecticut, Ctr Integrat Geosci, Storrs, CT 06269 USA. [Bambach, Richard K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Bush, AM (reprint author), Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. EM andrew.bush@uconn.edu NR 127 TC 34 Z9 35 U1 4 U2 40 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 0084-6597 BN 978-0-8243-2039-3 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 2011 VL 39 BP 241 EP 269 DI 10.1146/annurev-earth-040809-152556 PG 29 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BVF28 UT WOS:000291366800009 ER PT S AU McInerney, FA Wing, SL AF McInerney, Francesca A. Wing, Scott L. BE Jeanloz, R Freeman, KH TI The Paleocene-Eocene Thermal Maximum: A Perturbation of Carbon Cycle, Climate, and Biosphere with Implications for the Future SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES, VOL 39 SE Annual Review of Earth and Planetary Sciences LA English DT Review; Book Chapter DE PETM; global warming; paleoclimate; paleoecology; carbon cycle ID CALCAREOUS NANNOFOSSIL ASSEMBLAGES; OCEANIC METHANE HYDRATE; CLAY-MINERAL EVIDENCE; VENETIAN PRE-ALPS; BIGHORN BASIN; ISOTOPE EXCURSION; PLANKTONIC-FORAMINIFERA; WILLWOOD FORMATION; EARLIEST EOCENE; ORGANIC-MATTER AB During the Paleocene-Eocene Thermal Maximum (PETM), similar to 56 Mya, thousands of petagrams of carbon were released into the ocean-atmosphere system with attendant changes in the carbon cycle, climate, ocean chemistry, and marine and continental ecosystems. The period of carbon release is thought to have lasted <20 ka, the duration of the whole event was similar to 200 ka, and the global temperature increase was 5-8 degrees C. Terrestrial and marine organisms experienced large shifts in geographic ranges, rapid evolution, and changes in trophic ecology, but few groups suffered major extinctions with the exception of benthic foraminifera. The PETM provides valuable insights into the carbon cycle, climate system, and biotic responses to environmental change that are relevant to long-term future global changes. C1 [McInerney, Francesca A.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL 60208 USA. [Wing, Scott L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP McInerney, FA (reprint author), Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL 60208 USA. EM cesca@earth.northwestern.edu; wings@si.edu RI McInerney, Francesca/B-7894-2009; OI McInerney, Francesca/0000-0002-2020-6650; Wing, Scott/0000-0002-2954-8905 NR 180 TC 186 Z9 190 U1 19 U2 179 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 0084-6597 BN 978-0-8243-2039-3 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 2011 VL 39 BP 489 EP 516 DI 10.1146/annurev-earth-040610-133431 PG 28 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BVF28 UT WOS:000291366800017 ER PT J AU Le Boeuf, BJ Condit, R Morris, PA Reiter, J AF Le Boeuf, Burney J. Condit, Richard Morris, Patricia A. Reiter, Joanne TI The Northern Elephant Seal (Mirounga angustirostris) Rookery at Ano Nuevo: A Case Study in Colonization SO AQUATIC MAMMALS LA English DT Article DE northern elephant seals; Mirounga angustirostris; colonization process; density-dependence; dispersion; immigration; recruitment ID POPULATION BOTTLENECK; BEHAVIOR; CALIFORNIA; IMPACT AB Our aim was to examine the colonization process in a large mammal, documenting the development of a breeding colony from its inception to reaching equilibrium numbers. We describe the development of a colony of northern elephant seals (Mirounga angustirostris) at Ano Nuevo in central California from initial colonization in 1961 to 2010, a period when the worldwide population was expanding rapidly. We recorded pup production and pup mortality prior to weaning from censuses of animals by sex and age categories. Colony growth was rapid initially, and pup production reached approximately 2,700 births during the period 1995 to 2006. Pups born declined subsequently. The pattern of colony growth and decline is explained by species-specific seal behavior; population variables that influence immigration rates; and local environmental factors such as breeding space, animal density, and tidal and surf conditions at peak season that increase pup mortality. Colony growth was driven primarily by external recruitment of young females from large southern rookeries rather than internal recruitment. Births on the island segment of the colony, where breeding space was limited, peaked in 1980 then declined subsequently by 50% in association with increased density and pup mortality. Births on the adjacent mainland stabilized from 1995 to 2006, despite ample breeding space and low pup mortality; cessation of growth here was associated with reduced external recruitment of females. Primiparous females pioneer the establishment of new colonies, settling new sites to avoid low weaning success in crowded natal rookeries where they are dominated by older females. We conclude that the long-term study of the development of a single colony provides vital information on colony and population processes that have wide applicability to other mammals. The colonization of Ano Nuevo recapitulated the process employed at other colonies during the recent growth and expansion of the population and signals the pattern to be expected in future colonies. C1 [Le Boeuf, Burney J.; Morris, Patricia A.; Reiter, Joanne] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA. [Condit, Richard] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Le Boeuf, BJ (reprint author), Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA. EM leboeuf@ucsc.edu FU National Science Foundation FX We thank colleagues and numerous students for invaluable assistance with censuses and other operations in the field and laboratory. We are grateful for help from students of D. Costa in recent years. We thank Gary Strachan and the rangers at Ano Nuevo State Reserve for providing access. This research was supported in part by several grants from the National Science Foundation, and censuses were conducted under permit #87-1743-04 from the National Marine Fisheries Service. NR 51 TC 11 Z9 11 U1 3 U2 16 PU EUROPEAN ASSOC AQUATIC MAMMALS PI MOLINE PA C/O DR JEANETTE THOMAS, BIOLOGICAL SCIENCES, WESTERN ILLIONIS UNIV-QUAD CITIES, 3561 60TH STREET, MOLINE, IL 61265 USA SN 0167-5427 J9 AQUAT MAMM JI Aquat. Mamm. PY 2011 VL 37 IS 4 BP 486 EP 501 DI 10.1578/AM.37.4.2011.486 PG 16 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 882DM UT WOS:000299541700006 ER PT J AU Park, MG Lee, H Kim, KY Kim, S AF Park, Myung Gil Lee, Hwayoung Kim, Kwang Young Kim, Sunju TI Feeding behavior, spatial distribution and phylogenetic affinities of the heterotrophic dinoflagellate Oxyphysis oxytoxoides SO AQUATIC MICROBIAL ECOLOGY LA English DT Article DE Dinophysiales; Myrionecta rubra; Oxyphysis oxytoxoides; Peduncle feeding; Phylogeny ID DINOPHYSIS DINOPHYCEAE; MIXED MODELS; CILIATE; SYMBIONTS; CAUDATA; GENUS; PREY AB We documented the abundance of the heterotrophic dinoflagellate Oxyphysis oxytoxoides Kofoid along the Korean coast, cultured it (food source: the marine ciliate Myrionecta rubra Jankowski [= Mesodinium rubrum Lohmann]), sequenced its nuclear-encoded large-subunit (LSU) rDNA, and resolved its phylogenetic relationship within the Dinophysiales. Abundance was low, usually < 9.7 x 10(3) cells l(-1), in samples from 2005 and 2006. It co-occurred with the mixotrophic dinoflagellate Dinophysis acuminata, possibly indicating a common pool of prey. Growth on M. rubra reached a density of 38 x 10(5) cells l(-1). Observations on live cells from our established cultures revealed that O. oxytoxoides uses a peduncle to suck up the cell contents of M. rubra, the number of food vacuoles increasing as feeding proceeds. No regional variability was found in partial LSU rDNA sequences (domains D1-D2) of our strains, despite different sampling sites and dates. Phylogenetic analysis, based on LSU rDNA, showed that while Amphisolenia forms an early divergent basal group in the Dinophysiales, the other dinophysoids form 2 separate groups: (1) Oxyphysis and Phalacroma, and (2) Histioneis, Ornithocercus, Citharistes and Dinophysis. The presence of a peduncle in several genera, and the widespread distribution of pedunculate dinophysoids, indicate that these species may be fundamentally heterotrophic with a common feeding mechanism. Our results shed light on the feeding ecology and phylogenetic position of O. oxytoxoides. C1 [Kim, Sunju] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Park, Myung Gil; Lee, Hwayoung; Kim, Kwang Young] Chonnam Natl Univ, Dept Oceanog, Kwangju 500757, South Korea. RP Kim, S (reprint author), Smithsonian Environm Res Ctr, 647 Contees Whari Rd, Edgewater, MD 21037 USA. EM sunjukim75@gmail.com FU Korean government (MEST) [2007-0055898]; Korean Government [2009-0066796] FX This work was supported by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MEST) (No. 2007-0055898) to K.Y.K and a National Research Foundation of Korea grant funded by the Korean Government (2009-0066796) to M.G.P. We thank Prof. Wonho Yih for allowing us to use the strain of Myrionecta rubra as a food source during this study. We also thank the 3 anonymous reviewers, whose comments and suggestions greatly improved the manuscript. NR 41 TC 3 Z9 4 U1 0 U2 5 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. PY 2011 VL 62 IS 3 BP 279 EP 287 DI 10.3354/ame01474 PG 9 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 719KP UT WOS:000287203900006 ER PT S AU Crowell, AL AF Crowell, Aron L. BE Croucher, SK Weiss, L TI Ethnicity and Periphery: The Archaeology of Identity in Russian America SO ARCHAEOLOGY OF CAPITALISM IN COLONIAL CONTEXTS: POSTCOLONIAL HISTORICAL ARCHAEOLOGIES SE Contributions to Global Historical Archaeology LA English DT Proceedings Paper CT Society-for-Historical-Archaeology 2008 Conference on Historical and Underwater Archaeology CY JAN 09-13, 2008 CL Albuquerque, NM ID KODIAK-ISLAND; ALASKA; COLONIZATION; CULTURE C1 [Crowell, Aron L.] Smithsonian Inst, Arctic Studies Ctr, Natl Museum Nat Hist, Alaska Programs, Washington, DC 20560 USA. EM Crowella@si.edu NR 105 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1574-0439 BN 978-1-4614-0191-9 J9 CONTRIB GLOB HIST AR PY 2011 BP 85 EP 104 PG 20 WC Anthropology; Archaeology SC Anthropology; Archaeology GA BWM90 UT WOS:000294266800004 ER PT B AU Christensen, SO Dunlop, D AF Christensen, Stephanie Ogeneski Dunlop, Doug GP IS & T TI The Case for Implementing Core Descriptive Embedded Metadata at the Smithsonian SO ARCHIVING 2011: PRESERVATION STRATEGIES AND IMAGING TECHNOLOGIES FOR CULTURAL HERITAGE INSTITUTIONS AND MEMORY ORGANIZATIONS LA English DT Proceedings Paper CT 8th IS & T and Archiving Conference CY MAY 16-19, 2011 CL Salt Lake City, UT SP Family Search, Image Engn, Lifewood, MAM A, Oracle, Tessella AB The long-term goal, as established by the institutional strategic plan, to digitize collections at the Smithsonian Institution along with the increasing need to share data and increase access to collections has made it essential to establish institution-wide metadata standards, including those for embedding metadata. This paper documents the ongoing process of establishing core embedded metadata within the institution through the work of the Smithsonian Embedded Metadata Working Group (EmDaWG), which is pan-institutional in nature and includes museums, libraries, archives, and research institutes. The focus of the working group described within this paper is the creation of core embedded metadata fields for use in still images. C1 [Christensen, Stephanie Ogeneski] Smithsonian Inst, Washington, DC 20560 USA. NR 7 TC 0 Z9 0 U1 1 U2 1 PU SOC IMAGING SCIENCE & TECHNOLOGY PI SPRINGFIELD PA 7003 KILWORTH LANE, SPRINGFIELD, VA 22151 USA BN 978-0-89208-294-0 PY 2011 BP 116 EP 120 PG 5 WC Information Science & Library Science; Imaging Science & Photographic Technology SC Information Science & Library Science; Imaging Science & Photographic Technology GA BVO71 UT WOS:000292115400028 ER PT B AU Fuhrig, LS AF Fuhrig, Lynda Schmitz GP IS & T TI Swinging in the Archives: In-House File Transfer of DATs SO ARCHIVING 2011: PRESERVATION STRATEGIES AND IMAGING TECHNOLOGIES FOR CULTURAL HERITAGE INSTITUTIONS AND MEMORY ORGANIZATIONS LA English DT Proceedings Paper CT 8th IS & T and Archiving Conference CY MAY 16-19, 2011 CL Salt Lake City, UT SP Family Search, Image Engn, Lifewood, MAM A, Oracle, Tessella AB Not long ago Digital Audio Tapes (DATs) were a popular medium for professional digital recording. The Smithsonian Institution Archives holds almost 2,000 DATs in its accessions but until recently lacked equipment to retrieve the rich collections of music, interviews, and programs from across the Institution Very few archives have conducted in-house transfers of DATs. The Smithsonian Institution Archives launched a successful pilot in 2010 to transfer the audio from the DATs to its secure servers and LTO tapes. These DATs contain priceless material from Smithsonian Jazz Masterworks Orchestra concerts to Native American radio programs to events at the Freer-Sackler Galleries of Art. This project is making these recordings accessible for the long term, as DAT machines are hard to acquire. The audio is being saved in the WAV/BWF preservation formats. Best practice procedures include checksums, quality assurance reviews, and regular backups. This paper discusses how the pilot operated and the challenges SIA encountered. C1 [Fuhrig, Lynda Schmitz] Smithsonian Inst Arch, Washington, DC USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU SOC IMAGING SCIENCE & TECHNOLOGY PI SPRINGFIELD PA 7003 KILWORTH LANE, SPRINGFIELD, VA 22151 USA BN 978-0-89208-294-0 PY 2011 BP 153 EP 157 PG 5 WC Information Science & Library Science; Imaging Science & Photographic Technology SC Information Science & Library Science; Imaging Science & Photographic Technology GA BVO71 UT WOS:000292115400035 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water Summary SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Editorial Material; Book Chapter C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP 1 EP 10 PG 10 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600002 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water Preface SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Editorial Material; Book Chapter C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP VII EP IX PG 3 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600001 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Setting the Invasive Species Management Stage SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Article; Book Chapter ID SHIPS BALLAST WATER; LAURENTIAN GREAT-LAKES; BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; MARINE ORGANISMS; TRANSPORT; PORT; COMMUNITIES; SEDIMENT; EXCHANGE C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 68 TC 0 Z9 0 U1 0 U2 1 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP 11 EP 34 PG 24 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600003 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Policy Context for Regulating Live Organisms in Ballast Discharge SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Article; Book Chapter ID VIRUSES; WATER C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 26 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP 35 EP 54 PG 20 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600004 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Sources of Variation Influencing the Probability of Invasion and Establishment SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Article; Book Chapter ID INCREASED COMPETITIVE ABILITY; SAN-FRANCISCO BAY; BALLAST WATER; MACROFAUNAL COMMUNITIES; PHRAGMITES-AUSTRALIS; BIOLOGICAL INVASIONS; LITTORINA-SAXATILIS; PROPAGULE PRESSURE; CRYPTIC INVASION; GLOBAL PATTERNS C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 62 TC 0 Z9 0 U1 0 U2 3 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP 55 EP 71 PG 17 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600005 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Relationship between Propagule Pressure and Establishment Risk SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Article; Book Chapter ID POPULATION VIABILITY ANALYSIS; LAURENTIAN GREAT-LAKES; BALLAST-WATER; BIOLOGICAL INVASIONS; NORTH-AMERICA; SPECIES INVASIONS; PLANT INVASIONS; SPATIAL SPREAD; LOW-DENSITY; MODEL C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 99 TC 0 Z9 0 U1 0 U2 2 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP 72 EP 113 PG 42 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600006 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Other Approaches to Setting a Ballast Water Discharge Standard SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Article; Book Chapter ID RISK-ASSESSMENT; SYSTEM; PLANTS C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP 114 EP 121 PG 8 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600007 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI The Path Forward SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Article; Book Chapter ID PROPAGULE PRESSURE; INVASION ECOLOGY; PLANT INVASIONS; BALLAST WATER; NORTH-AMERICA; UNITED-STATES; PATTERNS; ESTABLISHMENT; COMMUNITIES; ECOSYSTEMS C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 31 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 BP 122 EP 136 PG 15 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600008 ER PT J AU Carlton, JT Ruiz, GM AF Carlton, James T. Ruiz, Gregory M. GP Natl Res Council TI Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water SO Assessing the Relationship Between Propagule Pressure and Invasion Risk in Ballast Water LA English DT Main Cite; Book Chapter C1 [Carlton, James T.] Williams Coll, Marine Sci, Williamstown, MA 01267 USA. [Carlton, James T.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Carlton, James T.] Marine Biodivers Comm, London, England. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Ruiz, Gregory M.] Natl Ballast Informat Clearinghouse, Washington, DC USA. RP Carlton, JT (reprint author), Williams Coll, Marine Sci, Williamstown, MA 01267 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21562-6 PY 2011 PG 156 WC Water Resources SC Water Resources GA BC5OT UT WOS:000353418600009 ER PT B AU Galle, EC Anderson, CS Bonaventura, NR Burke, DJ Fruscione, A Lee, NP McDowell, JC AF Galle, Elizabeth C. Anderson, Craig S. Bonaventura, Nina R. Burke, D. J. Fruscione, Antonella Lee, Nicholas P. McDowell, Jonathan C. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Python Scripting for CIAO Data Analysis SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB The Chandra X-ray Center has adopted Python as the primary scripting language in the Chandra Interactive Analysis of Observations software package (CIAO). Python is a dynamic object-oriented programming language that offers strong support for integration with other languages and tools and conies with extensive standard libraries. Integrating Python into CIAO allows us to develop powerful new scripts for data analysis, as well as rewrite and improve upon popular CIAO contributed scripts. We discuss the coding guidelines that we have developed during this process, using specific CIAO contributed scripts - available for download online - as examples. C1 [Galle, Elizabeth C.; Anderson, Craig S.; Bonaventura, Nina R.; Burke, D. J.; Fruscione, Antonella; Lee, Nicholas P.; McDowell, Jonathan C.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Galle, EC (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 131 EP 134 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100030 ER PT B AU Lee, NP Karovska, M Galle, EC Bonaventura, NR AF Lee, Nicholas P. Karovska, Margarita Galle, Elizabeth C. Bonaventura, Nina R. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Chandra X-ray Center Science Data Systems Regression Testing of CIAO SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB The Chandra Interactive Analysis of Observations' (CIAO) is a software system developed for the analysis of Chandra X-ray Observatory observations. An important component of a successful CIAO release is the repeated testing of the tools across various platforms to ensure consistent and scientifically valid results. We describe the procedures of the scientific regression testing of CIAO and the enhancements made to the testing system to increase the efficiency of run time and result validation. C1 [Lee, Nicholas P.; Karovska, Margarita; Galle, Elizabeth C.; Bonaventura, Nina R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Lee, NP (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 135 EP 138 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100031 ER PT B AU Anderson, CS Mossman, AE Kim, DW Allen, GE Glotfelty, KJ Fabbiano, G AF Anderson, Craig S. Mossman, Amy E. Kim, Dong-Woo Allen, Glenn E. Glotfelty, Kenny J. Fabbiano, Giuseppina BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI ACIS Sub-Pixel Resolution: Improvement in Point Source Detection SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr ID SPATIAL-RESOLUTION; EVENTS AB We investigate how to achieve the best possible ACIS spatial resolution by binning in ACTS sub-pixel and applying an event repositioning algorithm after removing pixel-randomization from the pipeline data. We quantitatively assess the improvement in spatial resolution by (1) measuring point source sizes and (2) detecting faint point sources. The size of a bright (but no pile-up), on-axis point source can be reduced by 20-30%. With the improved resolution, we detect similar to 20% more faint sources when embedded in the extended, diffuse emission in a crowded field. We further discuss the false source rate of similar to 10% among the newly detected sources, using a few ultra-deep observations. C1 [Anderson, Craig S.; Mossman, Amy E.; Kim, Dong-Woo; Glotfelty, Kenny J.; Fabbiano, Giuseppina] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Anderson, CS (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 6 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 139 EP 142 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100032 ER PT B AU Arcand, KK Watzke, M Smith, LF Smith, JK AF Arcand, Kimberly Kowal Watzke, Megan Smith, Lisa F. Smith, Jeffrey K. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI The Aesthetics of Astronomy: Exploring the Public's Perception of Astronomy Images and the Science Within SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB Every year, hundreds of astronomical images are released to the public via the efforts of professional education and public outreach (EPO) specialists, as well as from scientists themselves and amateur astronomers. Each of these images represents a variety of decisions from the individual or team that assembled it. These choices include cropping, color, contextualization, and many more. But how effective are these choices in both engaging the public's interest and communicating scientific information to them? In 2008, the Smithsonian Astrophysical Observatory began a unique research study - dubbed the Aesthetics & Astronomy (A&A) project - to examine these very questions. The study included images from across the electromagnetic spectrum and probed the effects of the scientific and artistic choices in processing astronomical data. This paper provides an overview of the results of the preliminary 2008 A&A study and includes a synopsis of the direction of the ongoing 2010 study. C1 [Arcand, Kimberly Kowal; Watzke, Megan] Smithsonian Astrophys Observ, Chandra Xray Ctr, 60 Garden St, Cambridge, MA 02138 USA. RP Arcand, KK (reprint author), Smithsonian Astrophys Observ, Chandra Xray Ctr, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 1 Z9 1 U1 0 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 179 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100040 ER PT B AU Mink, DJ AF Mink, Douglas J. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Data Pipelines for the TRES Echelle Spectrograph SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr ID RADIAL-VELOCITIES; REDUCTION; ERA AB An IRAF-based processing pipeline has been written to reduce spectra from the Smithsonian Astrophysical Observatory's TRES (Tillinghast Reflector Echelle Spectrograph) two-fiber echelle spectrograph on Mt. Hopkins in Arizona. A modular system was written in IRAF so that the same software could be used at the telescope for quick-look processing and later with more accuracy for scientific processing. IRAF tasks developed for the SAO FAST long-slit and Hectospec multi-fiber spectrographs, as well as NOAO-developed echelle tasks, were adapted for this instrument. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Mink, DJ (reprint author), Smithsonian Astrophys Observ, 60 Garden Sr, Cambridge, MA 02138 USA. NR 6 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 305 EP 308 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100065 ER PT B AU Gibbs, DG Chen, JC Glotfelty, KJ Allen, GE Huenemoerder, DP Primini, FA AF Gibbs, D. G., II Chen, J. C. Glotfelty, K. J. Allen, G. E. Huenemoerder, D. P. Primini, F. A. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Maintaining Software for Active Missions: A Case Study of Chandra's Instrumentation Over Time SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB During eleven plus years of operation, ample knowledge has been gained regarding the Chandra X-ray Observatory's scientific instruments and how they are performing over time. In this paper we will summarize the significant software changes related to the performance and knowledge gained about the observatory's instrumentation specifically targeting the last five years of the mission. With this knowledge, numerous upgrades to the Chandra processing software have taken place to correct issues that have developed on orbit (ACIS CTI effects, LETG/ACIS rotation), to correct for hardware issues (HRC timing), and for our better understanding of the evolution of the instrumentation (temporal gain shifts in both instruments). In addition, we will discuss the challenges in maintaining software when the calibrations for different operating modes are incrementally made available. This includes challenges in maintaining an archive with a mixture of data products with different calibrations applied. This paper roughly covers the era of the 3rd reprocessing of the Chandra archive (Repro-3). C1 [Gibbs, D. G., II; Chen, J. C.; Glotfelty, K. J.; Primini, F. A.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RP Gibbs, DG (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 379 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100083 ER PT B AU Accomazzi, A Dave, R AF Accomazzi, Alberto Dave, Rahul BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Semantic Interlinking of Resources in the Virtual Observatory Era SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB In the coming era of data-intensive science, it will be increasingly important to be able to seamlessly move between scientific results, the data analyzed in them, and the processes used to produce them. As observations, derived data products, publications, and object metadata are curated by different projects and archived in different locations, establishing the proper linkages between these resources and describing their relationships becomes an essential activity in their curation and preservation. In this paper we describe initial efforts to create a semantic knowledge base allowing easier integration and linking of the body of heterogeneous astronomical resources which we call the Virtual Observatory (VO). The ultimate goal of this effort is the creation of a semantic layer over existing resources, allowing applications to cross boundaries between archives. The proposed approach follows the current best practices in Semantic Computing and the architecture of the web, allowing the use of off-the-shelf technologies and providing a path for VO resources to become part of the global web of linked data. C1 [Accomazzi, Alberto; Dave, Rahul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Accomazzi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 3 Z9 3 U1 0 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 415 EP 424 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100090 ER PT B AU Siemiginowska, A Kashyap, V Refsdal, B van Dyk, D Connors, A Park, T AF Siemiginowska, Aneta Kashyap, Vinay Refsdal, Brian van Dyk, David Connors, Alanna Park, Taeyoung BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI pyblocxs: Bayesian Low-Counts X-ray Spectral Analysis in Sherpa SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr ID LIKELIHOOD RATIO AB Typical X-ray spectra have low counts and should be modeled using the Poisson distribution. However, chi(2) statistic is often applied as an alternative and the data are assumed to follow the Gaussian distribution. A variety of weights to the statistic or a binning of the data is performed to overcome the low counts issues. However, such modifications introduce biases or/and a loss of information. Standard modeling packages such as XSPEC and Sherpa provide the Poisson likelihood and allow computation of rudimentary MCMC chains, but so far do not allow for setting a full Bayesian model. We have implemented a sophisticated Bayesian MCMC-based algorithm to carry out spectral fitting of low counts sources in the Sherpa environment. The code is a Python extension to Sherpa and allows to fit a predefined Sherpa model to high-energy X-ray spectral data and other generic data. We present the algorithm and discuss several issues related to the implementation, including flexible definition of priors and allowing for variations in the calibration information. C1 [Siemiginowska, Aneta; Kashyap, Vinay; Refsdal, Brian] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Siemiginowska, A (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 8 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 439 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100093 ER PT B AU Kim, DW Protopapas, P Alcock, C Byun, YI Khardon, R AF Kim, Dae-Won Protopapas, Pavlos Alcock, Charles Byun, Yong-Ik Khardon, Roni BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Automatic QSO Selection Using Machine Learning: Application on Massive Astronomical Database SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr ID ACTIVE GALACTIC NUCLEI; LARGE-MAGELLANIC-CLOUD; SPACED DATA; DIFFERENCE AB We present a new QSO (Quasi-Stellar Object) selection algorithm using Support Vector Machine (SVM), a supervised classification method, on a set of multiple extracted times series features such as period, amplitude, color, and autocorrelation value. We train a model that separates QSOs from variable stars, non-variable stars and microlensing events using the richest possible training set consisting of all known types of variables including QSOs from the MAssive Compact Halo Object (MACHO) database. We applied the trained model on the MACHO Large Magellanic Cloud (LMC) dataset, which consists of 40 million lightcurves, and found 1,620 QSO candidates. During the selection none of the 33,242 known MACHO variables were misclassified as QSO candidates. In order to estimate the true false positive rate, we crossmatched the candidates with astronomical catalogs including the Spitzer Surveying the Agents of a Galaxy's Evolution (SAGE) LMC catalog. The results further suggest that the majority of the candidates, more than 70%, are QSOs. C1 [Kim, Dae-Won; Protopapas, Pavlos; Alcock, Charles] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 16 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 447 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100095 ER PT B AU Lyn, J Burke, D Cresitello-Dittmar, M Evans, I Evans, JD AF Lyn, Janine Burke, Doug Cresitello-Dittmar, Mark Evans, Ian Evans, Janet DePonte BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI The Crates Library: The Redesigned Python Interface for Scripting Languages SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB Crates is a Python module produced by the Chandra X-ray Center (CXC) that provides a convenient high-level user interface for accessing and manipulating data stored in a variety of formats. Crates is currently utilized by Chandra's plotting, modeling and fitting tools. This paper will highlight the design changes and improvements made to Crates. This version of Crates has been completely rewritten in Python and has been optimized to conserve time and memory resources through lazy initialization. It provides increased functionality for data and metadata manipulation along with better memory management. In addition, Crates will be able to interface with several different backend modules, allowing the user to effortlessly switch between the CXC Data Model (DM), Virtual Observatory (VO), and pyFITS formats. C1 [Lyn, Janine; Burke, Doug; Cresitello-Dittmar, Mark; Evans, Ian; Evans, Janet DePonte] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Lyn, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 509 EP 512 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100110 ER PT B AU Burke, DJ AF Burke, D. J. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Charming Users into Scripting CIAO with Python SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB The Science Data Systems group of the Chandra X-ray Center provides a number of scripts and Python modules that extend the capabilities of CIAO.(1) Experience in converting the existing scripts-written in a variety of languages such as bash, csh/tcsh, Pert and S-Lang-to Python, and conversations with users, led to the development of the ciao_contrib.runtool module. This allows users to easily run CIAO tools from Python scripts, and utilizes the metadata provided by the parameter-file system to create an API that provides the flexibility and safety guarantees of the command-line. The module is provided to the user community and is being used within our group to create new scripts. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Burke, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 513 EP 516 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100111 ER PT B AU Nguyen, D Doe, S Evans, I Hain, R Primini, F AF Nguyen, D. Doe, S. Evans, I. Hain, R. Primini, F. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI The Sherpa Maximum Likelihood Estimator SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr ID SOURCE CATALOG AB A primary goal for the second release of the Chandra Source Catalog (CSC) is to include X-ray sources with as few as 5 photon counts detected in stacked observations of the same field, while maintaining acceptable detection efficiency and false source rates. Aggressive source detection methods will result in detection of many false positive source candidates. Candidate detections will then be sent to a new tool, the Maximum Likelihood Estimator (MLE), to evaluate the likelihood that a detection is a real source. MLE uses the Sherpa modeling and fitting engine to fit a model of a background and source to multiple overlapping candidate source regions. A background model is calculated by simultaneously fitting the observed photon flux in multiple background regions. This model is used to determine the quality of the fit statistic for a background-only hypothesis in the potential source region. The statistic for a background-plus-source hypothesis is calculated by adding a Gaussian source model convolved with the appropriate Chandra point spread function (PSF) and simultaneously fitting the observed photon flux in each observation in the stack. Since a candidate source may be located anywhere in the field of view of each stacked observation, a different PSF must be used for each observation because of the strong spatial dependence of the Chandra PSF. The likelihood of a valid source being detected is a function of the two statistics (for background alone, and for background-plus-source). The MLE tool is an extensible Python module with potential for use by the general Chandra user. C1 [Nguyen, D.; Doe, S.; Evans, I.; Hain, R.; Primini, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nguyen, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 517 EP 520 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100112 ER PT B AU Glotfelty, KJ Miller, J Chen, J AF Glotfelty, Kenny J. Miller, Joseph Chen, Judy BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI dax: DS9 Analysis Extensions in CIAO SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB dax is a suite of scripts that allows various CIAO tools (written to support the Chandra X-ray Observatory) to be run using the analysis framework provided by SAOImage DS9. This allows users to quickly leverage the functionality CIAO provides without having to invest in learning the syntax and semantics of each of the tools. This simplification of the interface benefits all astronomers since many of the CIAO tools are sufficiently generic that they can work with data sets from arbitrary observatories. We present the dax design and discuss some of the pitfalls and limitations we encountered while building dux. C1 [Glotfelty, Kenny J.; Miller, Joseph; Chen, Judy] Smithsonian Astrophys Observ, Cambridge, MA 01238 USA. RP Glotfelty, KJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 01238 USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 629 EP 632 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100137 ER PT B AU Joye, W AF Joye, William BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI SAOImage DS9 Frequently Asked Questions SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr ID ACCESS PROGRAMMING TECHNIQUES; DATA VISUALIZATION; SAOTK AB SAOImage DS9 is an astronomical imaging and data visualization application. It supports FITS images and binary tables, multiple frame buffers, region manipulation, and many scale algorithms and colormaps. It provides for easy communication with external analysis tasks and is highly configurable and extensible via XPA and SAMP. This article will highlight some of the more popular questions which have been submitted by users. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Joye, W (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 633 EP 636 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100138 ER PT B AU Miller, J Burke, DJ Evans, I Evans, JD McLaughlin, W AF Miller, Joseph Burke, Douglas J. Evans, Ian Evans, Janet D. McLaughlin, Warren BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Imaging in ChIPS SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB The Chandra Interactive Plotting System (ChIPS) included in CIAO now allows users to incorporate and manipulate images in their plots. ChIPS uses the Visualization Toolkit (VTK) as a back end to provide basic imaging support, which includes displaying images in pseudo color or RGBA true color, adjusting the translucency of images, and several ways to threshold images. Users also have the ability to enhance them with annotations and place curves and contours directly onto the image. ChIPS imaging support provides a mechanism to adjust the image display resolution as necessary to provide high quality publication ready output. Beyond basic imaging, ChIPS includes the ability to recognize and incorporate WCS metadata into plots. ChIPS accurately calculates the intersections of world coordinate grids and plot axes, ensuring that these elements distort correctly with a tangent plane projection. Multiple image overlays are handled by reprojecting the overlaid images onto the reference image's coordinate system. New zooming and panning functions, and existing limits commands, use the WCS information from the image overlays to update the axes to reflect the new field of view being displayed. Although ChIPS already provides a number of user interactive commands, additional interactive capabilities are being considered for future releases. Enhanced interactive interfaces alongside the ability to script ChIPS in Python provide a more capable and user-friendly system. C1 [Miller, Joseph; Burke, Douglas J.; Evans, Ian; Evans, Janet D.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [McLaughlin, Warren] Northrop Grumman Informat Syst, Cambridge, MA USA. RP Miller, J (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. FU National Aeronautics and Space Administration through the Chandra X-ray Center; National Aeronautics and Space Administration [NAS8-03060] FX Support of the development of ChIPS is provided by the National Aeronautics and Space Administration through the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 637 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100139 ER PT B AU Watry, AC Rots, AH AF Watry, Aaron C. Rots, Arnold H. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Chandra Footprint Service: Visualizing Chandra's Sky Coverage SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB The Chandra Footprint Service(1) (CFS) provides a visual interface to data in the public Chandra Data Archive and the Chandra Source Catalog. Users of the service can directly see which areas of the sky have been observed by the Chandra X-Ray Observatory near any target of interest. The browser based interface provides visualization of the sky coverage of Chandra instruments for any region of the sky along with tabular data for observations. The service provides an interactive client-based overlay of the instrument region data on top of a Digitized Sky Survey (DSS) background image, previews of observation images, access to data products, and access to the VOTable data used to create the interface. C1 [Watry, Aaron C.; Rots, Arnold H.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Watry, AC (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 641 EP 644 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100140 ER PT B AU Van Stone, D Harbo, P Tibbetts, M Zografou, P AF Van Stone, D. Harbo, P. Tibbetts, M. Zografou, P. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI CSCview: A Graphical User Interface to the Chandra Source Catalog SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB CSCview is a graphical user interface to the Chandra Source Catalog. The interface uses a Java applet which accesses the catalog through a middle-tier Java EE application server. A tabbed interface allows the user to navigate through the main functions of the application: selecting from a list of catalog versions, creating a query, displaying the results, and downloading products. The application includes other features, such as a persistent set of user preferences and a guided help screen. CSCview had its initial release in 2009 and is being updated to include new features and to accommodate evolving requirements. C1 [Van Stone, D.; Harbo, P.; Tibbetts, M.; Zografou, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Van Stone, D (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 649 EP 652 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100142 ER PT B AU Goodman, AA Udomprasert, PS Kent, B Sathiapal, H Smareglia, R AF Goodman, Alyssa A. Udomprasert, Patricia S. Kent, Brian Sathiapal, Hanna Smareglia, Riccardo BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Astronomy Visualization for Education and Outreach SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB About 50 participants came to a discussion on the benefits and potential obstacles of using astronomy visualization tools for education and public outreach (EPO). Representatives of five different EPO organizations shared information on their project goals and outcomes. Public users need support to learn how to use these programs effectively for education, but the efforts are worthwhile because the thrill that comes from working with real data and the natural beauty of astronomical imagery are great attractors for new science enthusiasts. C1 [Goodman, Alyssa A.; Udomprasert, Patricia S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. RP Goodman, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 2 TC 1 Z9 1 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 659 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100144 ER PT B AU Refsdal, B Doe, S Nguyen, D Siemiginowska, A Burke, D Evans, J Evans, I AF Refsdal, B. Doe, S. Nguyen, D. Siemiginowska, A. Burke, D. Evans, J. Evans, I. BE Evans, IN Accomazzi, A Mink, DJ Rots, AH TI Advanced Python Scripting Using Sherpa SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 20th Annual Conference on Astronomical Data Analysis Software and Systems CY NOV 07-11, 2010 CL Seaport World Trade Ctr, Boston, MA SP Harvard Smithsonian Ctr Astrophys, Wolfram Res, NetApp, Hinode XRay Telescope Sci Team HO Seaport World Trade Ctr AB Sherpa is a general purpose modeling and fitting application written in Python. The dynamism of Python allows Sherpa to be a powerful and extensible software package ready for the modern challenges of data analysis. Primarily developed for the Chandra Interactive Analysis of Observations (CIAO) package, it provides a flexible environment for resolving spectral and image properties, analyzing time series, and modeling generic types of data. Complex model expressions are supported using Sherpa's general purpose definition syntax. Sherpa's parameterized data modeling is achieved using robust optimization methods implementing the forward fitting technique. Sherpa includes functions to calculate goodness-of-fit and parameter confidence limits. CPU intensive routines are written in C++/FORTRAN. But since all other data structures are contained in Python modules, users can easily add their own data structures, models, statistics or optimization methods to Sherpa. We will introduce a scripted example that highlights Sherpa's ability to estimate energy and photon flux errors using simulations. The draws from these simulations, accessible as NumPy ndarrays, can be sampled from uni-variate and multi-variate normal distributions and can be binned and visualized with simple high level functions. We will demonstrate how Sherpa can be extended with user-defined model and statistic classes written in Python. Sherpa's open design even allows users to incorporate prior statistics derived from the source model. C1 [Refsdal, B.; Doe, S.; Nguyen, D.; Siemiginowska, A.; Burke, D.; Evans, J.; Evans, I.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Refsdal, B (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-764-3 J9 ASTR SOC P PY 2011 VL 442 BP 687 EP 690 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVM57 UT WOS:000291892100150 ER PT J AU Basri, G Walkowicz, LM Batalha, N Gilliland, RL Jenkins, J Borucki, WJ Koch, D Caldwell, D Dupree, AK Latham, DW Marcy, GW Meibom, S Brown, T AF Basri, Gibor Walkowicz, Lucianne M. Batalha, Natalie Gilliland, Ronald L. Jenkins, Jon Borucki, William J. Koch, David Caldwell, Doug Dupree, Andrea K. Latham, David W. Marcy, Geoffrey W. Meibom, Soeren Brown, Tim TI PHOTOMETRIC VARIABILITY IN KEPLER TARGET STARS. II. AN OVERVIEW OF AMPLITUDE, PERIODICITY, AND ROTATION IN FIRST QUARTER DATA SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: activity; starspots; stars: rotation; stars: solar-type; stars: statistics; stars: variables: general ID OSCILLATIONS AB We provide an overview of stellar variability in the first quarter data from the Kepler mission. The intent of this paper is to examine the entire sample of over 150,000 target stars for periodic behavior in their light curves and relate this to stellar characteristics. This data set constitutes an unprecedented study of stellar variability given its great precision and complete time coverage (with a half hour cadence). Because the full Kepler pipeline is not currently suitable for a study of stellar variability of this sort, we describe our procedures for treating the "raw" pipeline data. About half of the total sample exhibits convincing periodic variability up to two weeks, with amplitudes ranging from differential intensity changes of less than 10(-4) up to more than 10%. K and M dwarfs have a greater fraction of period behavior than G dwarfs. The giants in the sample have distinctive quasi-periodic behavior, but are not periodic in the way we define it. Not all periodicities are due to rotation, and the most significant period is not necessarily the rotation period. We discuss properties of the light curves, and in particular look at a sample of very clearly periodic G dwarfs. It is clear that a large number of them do vary because of rotation and starspots, but it will take further analysis to fully exploit this. C1 [Basri, Gibor; Walkowicz, Lucianne M.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Batalha, Natalie; Jenkins, Jon; Borucki, William J.; Koch, David; Caldwell, Doug] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dupree, Andrea K.; Latham, David W.; Meibom, Soeren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Tim] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. RP Basri, G (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU Kepler Fellowship for the Study of Planet-Bearing Stars; NSF [AST-0606748]; NASA's Science Mission Directorate FX The authors thank the entire Kepler mission team, including the engineers and managers who were so pivotal in the ultimate success of the mission. L. W. is grateful for the support of the Kepler Fellowship for the Study of Planet-Bearing Stars. G. B. thanks the NSF through grant AST-0606748 for partial support of this work. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. NR 15 TC 96 Z9 96 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2011 VL 141 IS 1 AR 20 DI 10.1088/0004-6256/141/1/20 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 694IW UT WOS:000285291100020 ER PT B AU Krejny, M Li, HB Matthews, T Novak, G Shinnaga, H Vaillancourt, J Whitney, B AF Krejny, Megan Li, Hua-bai Matthews, Tristan Novak, Giles Shinnaga, Hiroko Vaillancourt, John Whitney, Barbara BE Bastien, P Manset, N Clemens, DP StLouis, N TI Submillimeter Spectropolarimetry as a Probe for Grain Growth in DG Tau SO ASTRONOMICAL POLARIMETRY 2008: SCIENCE FROM SMALL TO LARGE TELESCOPES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astronomical Polarimetry 2008 - Science from Small to Large Telescopes CY JUL 06-11, 2008 CL La Malbaie, CANADA SP Canadian Inst Theoret Astrophys, Univ Montreal, Fac Arts & Sci, Ctr Rech Astrophys Quebec ID DISKS; STARS; DUST AB We present 350 mu m polarization data for DG Tau, obtained at the Caltech Submillimeter Observatory (CSO) with the SHARP polarimeter. We compare this result with polarization data previously taken at 850 mu m by Tamura at al. (1999). Polarized light for DG Tau at these wavelengths is believed to be caused by dust grains in the surrounding dust and gas disk. Our results suggest considerable structure in the submillimeter polarization spectrum, which is not predicted by current models. C1 [Krejny, Megan; Matthews, Tristan; Novak, Giles] Northwestern Univ, Dept Phys & Astron, 2131 Tech Dr, Evanston, IL 60208 USA. [Li, Hua-bai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shinnaga, Hiroko] CALTECH, Submillimeter Observ, Hilo, HI 96720 USA. [Vaillancourt, John] CALTECH, Pasadena, CA 91125 USA. [Whitney, Barbara] Space Sci Inst, Boulder, CO USA. RP Krejny, M (reprint author), Northwestern Univ, Dept Phys & Astron, 2131 Tech Dr, Evanston, IL 60208 USA. EM megan@lennon.astro.northwestern.edu; hli@cfa.harvard.edu; g-novak@northwestern.edu NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-780-3 J9 ASTR SOC P PY 2011 VL 449 BP 338 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBY34 UT WOS:000308674100059 ER PT S AU Paine, S AF Paine, S. CA RHUBC-II Team BE Cure, M Otarola, A Marin, J Sarazin, M TI ADVANCING THE UNDERSTANDING OF RADIATIVE PROPERTIES IN THE UPPER TROPOSPHERE: THE RHUBC CAMPAIGN ON CERRO TOCO SO ASTRONOMICAL SITE TESTING DATA IN CHILE SE Revista Mexicana de Astronomia y Astrofisica-Serie de Conferencias LA English DT Proceedings Paper CT Conference on the Astronomical Site Testing Data in Chile Conference CY DEC 01-03, 2010 CL Valparaiso, CHILE C1 [Paine, S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Paine, S (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM spaine@cfa.harvard.edu NR 1 TC 1 Z9 1 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 BN 978-607-02-2880-3 J9 REV MEX AST ASTR PY 2011 VL 41 BP 24 EP 24 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAL13 UT WOS:000304498000007 ER PT J AU Aladro, R Martin-Pintado, J Martin, S Mauersberger, R Bayet, E AF Aladro, R. Martin-Pintado, J. Martin, S. Mauersberger, R. Bayet, E. TI CS, HC3N, and CH3CCH multi-line analyses toward starburst galaxies The evolution of cloud structures in the central regions of galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; galaxies: starburst; galaxies: groups: individual: NGC 253; galaxies: groups: individual: M82; galaxies: groups: individual: IC 342; galaxies: groups: individual: Maffei 2 ID GALACTIC-CENTER REGION; DENSE MOLECULAR GAS; NEARBY GALAXIES; STAR-FORMATION; INTERSTELLAR CLOUDS; DOMINATED CHEMISTRY; COLOGNE DATABASE; SPIRAL GALAXIES; SUBMILLIMETER-C; SIO EMISSION AB Aims. We aim to study the properties of the dense molecular gas towards the inner few 100 pc of four nearby starburst galaxies dominated both by photo dissociation regions (M 82) and large-scale shocks (NGC 253, IC 342, and Maffei 2), and to connect the chemical and physical properties of the molecular clouds with the evolutionary stage of the nuclear starbursts. Methods. We have carried out multi-transitional observations and analyses of three dense gas molecular tracers, CS, HC3N (cyanoacetylene), and CH3CCH (methyl acetylene), using Boltzmann diagrams in order to determine the rotational temperatures and column densities of the dense gas, and using a large velocity gradients model to calculate the H-2 density structure in the molecular clouds. Results. The CS and HC3N data indicate the presence of density gradients in the molecular clouds. These two molecules show similar excitation conditions, suggesting that they arise from the same gas components. In M82, CH3CCH has the highest fractional abundance determined in an extragalactic source (1.1 x 10(-8)). Conclusions. The density and the chemical gradients we found in all galaxies can be explained in the framework of the starburst evolution, which affects the chemistry and the structure of molecular clouds around the galactic nuclei. The young shock-dominated starburst galaxies, like presumably Maffei 2, show a cloud structure with a fairly uniform density and chemical composition that suggests low star formation activity. Molecular clouds in galaxies with starburst in an intermediate stage of evolution, such as NGC 253 and IC 342, show clouds with a high density contrast (two orders of magnitude) between the denser regions (cores) and the less dense regions (halos) of the molecular clouds and relatively constant chemical abundance. Finally, the galaxy with the most evolved starburst, M 82, has clouds with a fairly uniform density structure, large envelopes of atomic/molecular gas subjected to UV photodissociating radiation from young star clusters, and very different chemical abundances of HC3N and CH3CCH. C1 [Aladro, R.] Inst Radioastron Milimetr IRAM, Granada 18012, Spain. [Martin-Pintado, J.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Martin, S.] European So Observ, Santiago 19, Chile. [Martin, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mauersberger, R.] Joint ALMA Observ, Santiago, Chile. [Bayet, E.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Aladro, R (reprint author), Inst Radioastron Milimetr IRAM, Avda Divina Pastora 7,Local 20, Granada 18012, Spain. EM aladro@iram.es RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU Leverhulme Trust; Spanish Ministerio de Ciencia e Innovacion [ESP2007-65812-C02-01]; MICINN [ESP2007-65812-C02-C01, AYA2010-21697-C05-01]; AstroMadrid [CAM S2009/ESP-1496] FX We thank the IRAM staff for their help with the observations and data reduction. R. Aladro acknowledges the hospitality of ESO Vitacura and the Joint ALMA Observatory. E.B. acknowledges financial support from the Leverhulme Trust. We thank the referee for numerous and constructive comments. This work has been partially supported by the Spanish Ministerio de Ciencia e Innovacion under project ESP2007-65812-C02-01, and J.M.-P. and S. M. have been partially funded by MICINN grants ESP2007-65812-C02-C01 and AYA2010-21697-C05-01, and J.M.-P. by AstroMadrid (CAM S2009/ESP-1496). NR 73 TC 25 Z9 25 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR A89 DI 10.1051/0004-6361/201014090 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700020 ER PT J AU Banzatti, A Testi, L Isella, A Natta, A Neri, R Wilner, DJ AF Banzatti, A. Testi, L. Isella, A. Natta, A. Neri, R. Wilner, D. J. TI New constraints on dust grain size and distribution in CQ Tauri SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; dust, extinction; circumstellar matter; stars: individual: CQ Tauri ID SPECTRAL ENERGY-DISTRIBUTIONS; INTERMEDIATE-MASS STARS; HERBIG AE SYSTEMS; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS; T-TAURI; PLANET FORMATION; HIGH-RESOLUTION; YOUNG STARS; GAS AB Context. Grain growth in circumstellar disks is expected to be the first step towards the formation of planetary systems. There is now evidence for grain growth in several disks around young stars. Aims. Radially resolved images of grain growth in circumstellar disks are believed to be a powerful tool to constrain the dust evolution models and the initial stage for the formation of planets. In this paper we attempt to provide these constraints for the disk surrounding the young star CQ Tau. This system was already suggested from previous studies to host a population of grains grown to large sizes. Methods. We present new high angular resolution (0 ''.3-0 ''.9) observations at wavelengths from 850 mu m to 3.6 cm obtained at the SMA, IRAM-PdBI and NRAO-VLA interferometers. We perform a combined analysis of the spectral energy distribution and of the high-resolution images at different wavelengths using a model to describe the dust thermal emission from the circumstellar disk. We include a prescription for the gas emission from the inner regions of the system. Results. We detect the presence of evolved dust by constraining the disk averaged dust opacity coefficient beta (computed between 1.3 and 7 mm) to be 0.6 +/- 0.1. This confirms the earlier suggestions that the disk contains dust grains grown to significant sizes and puts this on firmer grounds by tightly constraining the gas contamination to the observed fluxes at mm-cm wavelengths. We report some evidence of radial variations in dust properties, but current resolution and sensitivity are still too low for definitive results. C1 [Banzatti, A.] ETH, CH-8093 Zurich, Switzerland. [Banzatti, A.; Testi, L.] ESO, D-85748 Garching, Germany. [Testi, L.; Natta, A.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Isella, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Banzatti, A (reprint author), ETH, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM ltesti@eso.org FU NASA; [ASI COFIS I/016/07/0] FX We thank Luca Ricci for his help in computing the dust opacities and for many useful discussions on grain growth in protoplanetary disks. All the observations used in this paper were taken in service mode by the observatories staff at SMA, IRAM and NRAO, their excellent support is gratefully acknowledged. LT and AN were partly supported by the grant ASI COFIS I/016/07/0. This work was performed in part under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Michelson Fellowship Program. JPL is managed for NASA by the California Institute of Technology. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 39 TC 27 Z9 27 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 JAN PY 2011 VL 525 AR A12 DI 10.1051/0004-6361/201015206 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700085 ER PT J AU Bartkiewicz, A Szymczak, M Pihlstrom, YM van Langevelde, HJ Brunthaler, A Reid, MJ AF Bartkiewicz, A. Szymczak, M. Pihlstroem, Y. M. van Langevelde, H. J. Brunthaler, A. Reid, M. J. TI VLA observations of water masers towards 6.7 GHz methanol maser sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: molecules; masers; techniques: interferometric ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; INFRARED ARRAY CAMERA; H-II REGIONS; HIGH-RESOLUTION; TRIGONOMETRIC PARALLAXES; CIRCUMSTELLAR DISK; VLBI OBSERVATIONS; RADIO-CONTINUUM; GLIMPSE SURVEY AB Context. Both 22GHz water and 6.7GHz methanol masers are usually interpreted as signposts of early stages of high-mass star formation but little is known about their associations and the physical environments in which they occur. Aims. We attempt to derive accurate positions and morphologies of the water maser emission and relate them to the methanol maser emission mapped earlier with Very Long Baseline Interferometry. Methods. We searched for 22 GHz water masers in 31 methanol maser sources was searched for 22 GHz water masers using the VLA and observed in the 6.7GHz methanol maser line with the 32 m Torun dish simultaneously. Results. Water maser clusters are detected towards 27 sites leading to the identification of 15 new sources. The detection rate of water maser emission associated with methanol sources is as high as 71%. In a large number of objects (18/21), the structure of water maser is well aligned with that of the extended emission at 4.5 mu m confirming the origin of water emission in outflows. The sources of methanol emission with ring-like morphologies, which likely trace a circumstellar disc/torus, either do not show associated water masers or the distribution of water maser spots is orthogonal to the major axis of the ring. Conclusions. The two maser species are generally powered by the same high-mass young stellar object but probe different parts of its environment. The morphology of water and methanol maser emission in a minority of sources is consistent with a scenario where 6.7 GHz methanol masers trace a disc/torus around a protostar while the associated 22GHz water masers arise in outflows. The majority of sources in which methanol maser emission is associated with the water maser appear to trace outflows. The two types of associations may be related to different evolutionary phases. C1 [Bartkiewicz, A.; Szymczak, M.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Pihlstroem, Y. M.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Pihlstroem, Y. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [van Langevelde, H. J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [van Langevelde, H. J.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bartkiewicz, A (reprint author), Nicholas Copernicus Univ, Torun Ctr Astron, Gagarina 11, PL-87100 Torun, Poland. EM annan@astro.uni.torun.pl RI Bartkiewicz, Anna/D-6212-2014; Szymczak, Marian/D-6773-2014; OI van Langevelde, Huib Jan/0000-0002-0230-5946 FU Polish Ministry of Science and Higher Education [N N203 386937]; Nicolaus Copernicus University [364-A]; Associated Universities, Inc.; National Aeronautics and Space Administration FX A.B. and M.S. acknowledge support by the Polish Ministry of Science and Higher Education through grant N N203 386937. A.B. acknowledges support by the Nicolaus Copernicus University grant 364-A (2009). The Very Large Array (VLA) of the National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 42 TC 13 Z9 13 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR A120 DI 10.1051/0004-6361/201015235 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700088 ER PT J AU Busquet, G Estalella, R Zhang, Q Viti, S Palau, A Ho, PTP Sanchez-Monge, A AF Busquet, G. Estalella, R. Zhang, Q. Viti, S. Palau, A. Ho, P. T. P. Sanchez-Monge, A. TI N2H+ depletion in the massive protostellar cluster AFGL 5142 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: individual objects: AFGL 5142; ISM: clouds; ISM: molecules; ISM: abundances ID FAR-INFRARED SOURCES; STAR-FORMING REGION; DENSE CLOUD CORES; CHEMICAL DIFFERENTIATION; MOLECULAR CLOUDS; CARBON-MONOXIDE; H2O MASERS; AFGL-5142; EVOLUTION; OUTFLOWS AB Aims. We aim at investigating the NH3/N2H+ abundance ratio toward the high-mass star-forming region AFGL 5142 with high angular resolution in order to study whether the NH3/N2H+ ratio behaves similarly to the low-mass case, for which the ratio decreases from starless cores to cores associated with young stellar objects (YSOs). Methods. CARMA was used to observe the 3.2 mm continuum and N2H+ (1-0) emission toward AFGL 5142. We used NH3 (1, 1) and (2, 2), as well as HCO+ (1-0) and (HCO+)-C-13 (1-0) data available from the literature, to study the chemical environment. Additionally, we performed a time-dependent chemical modeling of the region. Results. The 3.2 mm continuum emission reveals a dust condensation of similar to 23 M-circle dot associated with the massive YSOs, deeply embedded in the strongest NH3 core (hereafter central core). The dense gas emission traced by N2H+ reveals two main cores, the western core of similar to 0.08 pc in size and the eastern core of similar to 0.09 pc, surrounded by a more extended and complex structure of similar to 0.5 pc, mimicking the morphology of the NH3 emission. The two cores are located to the west and to the east of the 3.2 mm dust condensation. Toward the central core the N2H+ emission drops significantly, indicating a clear chemical differentiation in the region. The N2H+ column density in the central core is one order of magnitude lower than in the western and eastern cores. Furthermore, we found low values of the NH3/N2H+ abundance ratio similar to 50-100 toward the western and eastern cores and high values up to 1000 associated with the central core. The chemical model used to explain the differences seen in the NH3/N2H+ ratio indicates that density along with temperature is a key parameter in determining the abundances of both NH3 and N2H+. The high density (n similar or equal to 106 cm(-3)) and temperature (T similar or equal to 70 K) reached in the central core allow molecules such as CO to evaporate from grain mantles. The CO desorption causes a significant destruction of N2H+, which favors the formation of HCO+. This result is supported by our observations, which show that N2H+ and HCO+ are anticorrelated in the central core. The observed values of the NH3/N2H+ ratio in the central core can be reproduced by our model for times of t similar or equal to 4.5-5.3 x 10(5) yr, while in the western and eastern cores the NH3/N2H+ ratio can be reproduced by our model for times in the range 10(4)-3 x 10(6) yr. Conclusions. The NH3/N2H+ abundance ratio in AFGL 5142 does not follow the same trend as in regions of low-mass star formation mainly because of the high temperature reached in hot cores. C1 [Busquet, G.; Estalella, R.; Sanchez-Monge, A.] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol IEEC UB, E-08028 Barcelona, Catalunya, Spain. [Zhang, Q.; Ho, P. T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Palau, A.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, Bellaterra 08193, Catalunya, Spain. [Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. RP Busquet, G (reprint author), Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol IEEC UB, Marti & Franques 1, E-08028 Barcelona, Catalunya, Spain. EM gbusquet@am.ub.es FU Spanish MEC [AYA2005-08523-C03]; MICINN [AYA2008-06189-C03]; FEDER; JAE-Doc CSIC; European Social Fund; Spanish MICINN [ESP2007-65475-C02-02, Consolider-CSD2006-00070]; Smithsonian Institute USS Endowment FX We thank the anonymous referee for his/her valuable comments and suggestions. G. B. is grateful to Dr. L. Testi and Dr. T. R. Hunter for providing the HCO+ and H13CO+ data. G. B., R. E., A. P., and A. S.-M. are supported by the Spanish MEC grant AYA2005-08523-C03 and the MICINN grant AYA2008-06189-C03 (co-funded with FEDER funds). A. P. is supported by a JAE-Doc CSIC fellowship co-funded with the European Social Fund. This research has been partially funded by Spanish MICINN under the ESP2007-65475-C02-02 and Consolider-CSD2006-00070 grants. Q. Z. acknowledges the support from the Smithsonian Institute USS Endowment funds. NR 57 TC 18 Z9 18 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR A141 DI 10.1051/0004-6361/201014152 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700022 ER PT J AU Chies-Santos, AL Larsen, SS Wehner, EM Kuntschner, H Strader, J Brodie, JP AF Chies-Santos, A. L. Larsen, S. S. Wehner, E. M. Kuntschner, H. Strader, J. Brodie, J. P. TI An optical/NIR survey of globular clusters in early-type galaxies I. Introduction and data reduction procedures SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: star clusters: general ID STELLAR POPULATION ANALYSIS; TELESCOPE ADVANCED CAMERA; MASSIVE STAR-CLUSTERS; VIRGO-CLUSTER; ELLIPTIC GALAXIES; SAURON PROJECT; COLOR DISTRIBUTIONS; INTERMEDIATE-AGE; SPECTROSCOPIC AGES; FORMATION HISTORY AB Context. The combination of optical and near-infrared (NIR) colours has the potential to break the age/metallicity degeneracy and offers a better metallicity sensitivity than optical colours alone. Previous tudies of extragalactic globular clusters (GCs) with this colour combination, however, have suffered from small samples or have been restricted to a few galaxies. Aims. We compile a homogeneous and representative sample of GC systems with multi-band photometry to be used in subsequent papers where ages and metallicity distributions will be studied. Methods. We acquired deep K-band images of 14 bright nearby early-type galaxies. The images were obtained with the LIRIS near-infrared spectrograph and imager at the William Herschel Telescope (WHT) and combined with optical ACS g and z images from the Hubble Space Telescope public archive. Results. For the first time we present homogeneous GC photometry in this wavelength regime for a large sample of galaxies, 14. We achieved a limitingmagnitude of K similar to 20-21. For the majority of the galaxies we detect about 70 GCs each. NGC 4486 and NGC4649, the cluster-richest galaxies in the sample contain 301 and 167 GCs, respectively. We present tables containing coordinates, photometry and sizes of the GCs. C1 [Chies-Santos, A. L.; Larsen, S. S.; Wehner, E. M.] Univ Utrecht, Astron Inst, NL-3584 Utrecht, Netherlands. [Wehner, E. M.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Kuntschner, H.] European So Observ, Space Telescope European Coordinating Facil, D-8046 Garching, Germany. [Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodie, J. P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Chies-Santos, AL (reprint author), Univ Utrecht, Astron Inst, Princetonpl 5, NL-3584 Utrecht, Netherlands. EM A.L.Chies@uu.nl RI Chies-Santos, Ana/A-2570-2015; OI Kuntschner, Harald/0000-0002-2768-1198 NR 89 TC 18 Z9 18 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR A19 DI 10.1051/0004-6361/201015681 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700147 ER PT J AU Chies-Santos, AL Larsen, SS Kuntschner, H Anders, P Wehner, EM Strader, J Brodie, JP Santos, JFC AF Chies-Santos, A. L. Larsen, S. S. Kuntschner, H. Anders, P. Wehner, E. M. Strader, J. Brodie, J. P. Santos, J. F. C., Jr. TI An optical/NIR survey of globular clusters in early-type galaxies II. Ages of globular cluster systems and the relation to galaxy morphology SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: star clusters: general ID STELLAR POPULATION ANALYSIS; 3-GYR-OLD MERGER REMNANT; LINE-STRENGTH MAPS; SAURON PROJECT; STAR-CLUSTERS; VIRGO-CLUSTER; LENTICULAR GALAXIES; SPECTROSCOPIC AGES; ELLIPTIC GALAXIES; VLT SPECTROSCOPY AB Context. Some photometric studies of extragalactic globular cluster (GC) systems using the optical and near-infrared colour combination have suggested the presence of a large fraction of intermediate-age (2-8Gyr) GCs. Aims. We investigate the age distributions of GC systems in 14 E/S0 galaxies. Methods. We carried out a differential comparison of the (g - z) vs. (g - K) two-colour diagrams for GC systems in the different galaxies in order to see whether there are any indications of age differences. We also compared the different GC systems with a few simple stellar population models. Results. No significant difference is detected in the mean ages of GCs among elliptical galaxies. S0 galaxies, on the other hand, show evidence for younger GCs. Surprisingly, this appears to be driven by the more metal-poor clusters. The age distribution of GCs in NGC 4365 seems to be similar to that of other large ellipticals (e. g. NGC4486, NGC 4649). Padova SSPs with recently released isochrones for old ages (14 Gyr) show less of an offset with respect to the photometry than previously published models. Conclusions. We suggest that E type galaxies assembled most of their GCs in a shorter and earlier period than S0 type galaxies. The latter galaxy type seems to have a more extended period of GC formation/assembly. C1 [Chies-Santos, A. L.; Larsen, S. S.; Anders, P.; Wehner, E. M.] Univ Utrecht, Astron Inst, NL-3584 Utrecht, Netherlands. [Wehner, E. M.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Kuntschner, H.] European So Observ, Space Telescope European Coordinating Facil, D-8046 Garching, Germany. [Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodie, J. P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Santos, J. F. C., Jr.] Univ Fed Minas Gerais, ICEx, Dept Fis, BR-31270901 Belo Horizonte, MG, Brazil. RP Chies-Santos, AL (reprint author), Univ Utrecht, Astron Inst, Princetonpl 5, NL-3584 Utrecht, Netherlands. EM A.L.Chies@uu.nl RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Chies-Santos, Ana/A-2570-2015; C. Santos Jr., Joao F./O-6572-2015; OI C. Santos Jr., Joao F./0000-0003-1794-6356; Kuntschner, Harald/0000-0002-2768-1198 FU Brazilian institution FAPEMIG [APQ-00117/08]; National Aeronautics and Space Administration FX We thank the referee for comments that improved the paper. We acknowledge Paula Coelho for interesting discussions. J.F.C.S.J. acknowledges the Brazilian institution FAPEMIG (grant APQ-00117/08). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration NR 59 TC 28 Z9 28 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR A20 DI 10.1051/0004-6361/201015683 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700148 ER PT J AU Giacintucci, S Markevitch, M Brunetti, G Cassano, R Venturi, T AF Giacintucci, S. Markevitch, M. Brunetti, G. Cassano, R. Venturi, T. TI A radio minihalo in the extreme cool-core galaxy cluster RXC J1504.1-0248 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms: non-thermal; galaxies: clusters: general; galaxies: clusters: individual: RXC J1504.1-0248 ID COLD FRONTS; HALOS; RAY; EMISSION; ORIGIN; TURBULENCE; SAMPLE AB Aims. We report the discovery of a radio minihalo in RXC J1504.1-0248, a massive galaxy cluster that has an extremely luminous cool core. To date, only 9 radio minihalos are known, thus the discovery of a new one in one of the most luminous cool-core clusters provides important information on this peculiar class of sources and sheds light on their origin. Methods. The diffuse radio source was detected using GMRT at 327 MHz and confirmed by pointed VLA data at 1.46 GHz. The minihalo has a radius of similar to 140 kpc. A Chandra gas temperature map shows that the minihalo emission fills the cluster cool core and has some morphological similarities to it, as has been previously observed for other minihalos. Results. The Chandra data reveal two subtle cold fronts in the cool core, likely created by sloshing of the core gas, as observed in most cool-core clusters. Following previous work, we speculate that the origin of the minihalo is related to sloshing. Sloshing may result in particle acceleration by generating turbulence and/or amplifying the magnetic field in the cool core, leading to the formation of a minihalo. C1 [Giacintucci, S.; Brunetti, G.; Venturi, T.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Giacintucci, S.; Markevitch, M.; Cassano, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cassano, R.] Univ Bologna, Dip Astron, I-40127 Bologna, Italy. RP Giacintucci, S (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM sgiaci_s@ira.inaf.it OI Cassano, Rossella/0000-0003-4046-0637; Brunetti, Gianfranco/0000-0003-4195-8613; Venturi, Tiziana/0000-0002-8476-6307 FU Chandra grant [AR0-11017X]; NASA [NAS8-39073]; INAF [PRIN-INAF2007, PRIN-INAF2008]; ASI-INAF [I/088/06/0] FX We thank the anonymous referee for constructive comments and suggestions that improved this work. We thank P. Mazzotta for useful discussions. R. C. and G. B. thank Harvard-Smithsonian Center for Astrophysics for hospitality. GMRT is run by the NCRA of the Tata Institute of Fundamental Research. Financial support for this work was partially provided by Chandra grant AR0-11017X, NASA contract NAS8-39073, by INAF under grants PRIN-INAF2007 and PRIN-INAF2008 and by ASI-INAF under grant I/088/06/0. NR 24 TC 22 Z9 22 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR L10 DI 10.1051/0004-6361/201015882 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700165 ER PT J AU Mottram, JC Hoare, MG Urquhart, JS Lumsden, SL Oudmaijer, RD Robitaille, TP Moore, TJT Davies, B Stead, J AF Mottram, J. C. Hoare, M. G. Urquhart, J. S. Lumsden, S. L. Oudmaijer, R. D. Robitaille, T. P. Moore, T. J. T. Davies, B. Stead, J. TI The Red MSX Source survey: the bolometric fluxes and luminosity distributions of young massive stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: massive; stars: pre-main sequence; H II regions; surveys ID GALACTIC RING SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; H-II REGIONS; RMS SURVEY; MOLECULAR CLOUDS; SOUTHERN-HEMISPHERE; STELLAR OBJECTS; (CO)-C-13 OBSERVATIONS; DUST CONTINUUM; HII-REGIONS AB Context. The Red MSX Source (RMS) survey is returning a large sample of massive young stellar objects (MYSOs) and ultra-compact (UC) H II regions using follow-up observations of colour-selected candidates from the MSX point source catalogue. Aims. We obtain the bolometric fluxes and, using kinematic distance information, the luminosities for young RMS sources with far-infrared fluxes. Methods. We use a model spectral energy distribution (SED) fitter to obtain the bolometric flux for our sources, given flux data from our work and the literature. The inputs to the model fitter were optimised by a series of investigations designed to reveal the effect varying these inputs had on the resulting bolometric flux. Kinematic distances derived from molecular line observations were then used to calculate the luminosity of each source. Results. Bolometric fluxes are obtained for 1173 young RMS sources, of which 1069 have uniquely constrained kinematic distances and good SED fits. A comparison of the bolometric fluxes obtained using SED fitting with trapezium rule integration and two component greybody fits was also undertaken, and showed that both produce considerable scatter compared to the method used here. Conclusions. The bolometric flux results allowed us to obtain the luminosity distributions of YSOs and UCH II regions in the RMS sample, which we find to be different. We also find that there are few MYSOs with L >= 10(5) L-circle dot, despite finding many MYSOs with 10(4) L-circle dot >= L >= 10(5) L-circle dot C1 [Mottram, J. C.] Univ Exeter, Dept Phys & Astron, Exeter EX4 4QL, Devon, England. [Mottram, J. C.; Hoare, M. G.; Lumsden, S. L.; Oudmaijer, R. D.; Davies, B.; Stead, J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Urquhart, J. S.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Sydney, NSW 2052, Australia. [Robitaille, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moore, T. J. T.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Davies, B.] Rochester Inst Technol, Rochester, NY 14623 USA. RP Mottram, JC (reprint author), Univ Exeter, Dept Phys & Astron, Exeter EX4 4QL, Devon, England. EM joe@astro.ex.ac.uk RI Davies, Ben/K-3996-2012; OI Davies, Ben/0000-0002-2010-2122; Robitaille, Thomas/0000-0002-8642-1329 FU Science and Technologies Research Council of the United Kingdom (STFC); National Aeronautics and Space Administration; National Science Foundation FX The authors would like to thank the referee, Barbara Whitney, for her helpful comments and suggestions which improved the quality and clarity of this paper. J.C.M. is partially funded by a Postgraduate Studentship and by a Postdoctoral Research Associate grant from the Science and Technologies Research Council of the United Kingdom (STFC). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This paper made use of information from the Red MSX Source survey database at www.ast.leeds.ac.uk/RMS which was constructed with support from the Science and Technology Facilities Council of the UK. NR 52 TC 36 Z9 36 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 JAN PY 2011 VL 525 AR A149 DI 10.1051/0004-6361/201014479 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700037 ER PT J AU Pizzo, RF de Bruyn, AG Bernardi, G Brentjens, MA AF Pizzo, R. F. de Bruyn, A. G. Bernardi, G. Brentjens, M. A. TI Deep multi-frequency rotation measure tomography of the galaxy cluster A2255 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual: Abell 2255; intergalactic medium; magnetic fields; polarization ID UNDERSTANDING RADIO POLARIMETRY; MAGNETIC-FIELDS; POLARIZED EMISSION; GALACTIC EMISSION; PERSEUS CLUSTER; ABELL 2255; 350 MHZ; DEPOLARIZATION; MERGER; SPECTRUM AB Aims. By studying the polarimetric properties of the radio galaxies and the radio filaments belonging to the galaxy cluster Abell 2255, we aim to unveil their 3-dimensional location within the cluster. Methods. We performed WSRT observations of A2255 at 18, 21, 25, 85, and 200 cm. The polarization images of the cluster were processed through rotation measure (RM) synthesis, producing three final RM cubes. Results. The radio galaxies and the filaments at the edges of the halo are detected in the high-frequency RM cube, obtained by combining the data at 18, 21, and 25 cm. Their Faraday spectra show different levels of complexity. The radio galaxies lying near by the cluster center have Faraday spectra with multiple peaks, while those at large distances show only one peak, as do the filaments. Similar RM distributions are observed for the external radio galaxies and for the filaments, with much lower average RM values and RM variance than those found in previous works for the central radio galaxies. The 85 cm RM cube is dominated by the Galactic foreground emission, but it also shows features associated with the cluster. At 2 m, no polarized emission from A2255 nor our Galaxy is detected. Conclusions. The radial trend observed in the RM distributions of the radio galaxies and in the complexity of their Faraday spectra favors the interpretation that the external Faraday screen for all the sources in A2255 is the ICM. Its differential contribution depends on the amount of medium that the radio signal crosses along the line of sight. The filaments should therefore be located at the periphery of the cluster, and their apparent central location comes from projection effects. Their high fractional polarization and morphology suggest that they are relics rather than part of a genuine radio halo. Their inferred large distance from the cluster center and their geometry could argue for an association with large-scale structure (LSS) shocks. C1 [Pizzo, R. F.; de Bruyn, A. G.; Bernardi, G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [de Bruyn, A. G.; Brentjens, M. A.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pizzo, RF (reprint author), Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands. EM pizzo@astro.rug.nl FU Netherlands Foundation for Scientific Research (NWO) FX The Westerbork Synthesis Radio Telescope is operated by ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands Foundation for Scientific Research (NWO). NR 57 TC 23 Z9 23 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR A104 DI 10.1051/0004-6361/201014158 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700023 ER PT J AU Tsujimoto, M Guainazzi, M Plucinsky, PP Beardmore, AP Ishida, M Natalucci, L Posson-Brown, JLL Read, AM Saxton, RD Shaposhnikov, NV AF Tsujimoto, M. Guainazzi, M. Plucinsky, P. P. Beardmore, A. P. Ishida, M. Natalucci, L. Posson-Brown, J. L. L. Read, A. M. Saxton, R. D. Shaposhnikov, N. V. TI Cross-calibration of the X-ray instruments onboard the Chandra, INTEGRAL, RXTE, Suzaku, Swift, and XMM-Newton observatories using G21.5-0.9 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: detectors; X-rays: individuals: G21.5-0.9 ID SUPERNOVA REMNANT G21.5-0.9; PHOTON IMAGING CAMERA; IN-ORBIT PERFORMANCE; PSR J1833-1034; BOARD SUZAKU; SNR G21.5-0.9; PULSAR; MISSION; HALO; DISCOVERY AB Context. For many years, X-ray astronomy missions have used the Crab nebula as a celestial calibration source for the X-ray flux and spectral shape. However, the object is often too bright for current and future missions equipped with instruments with improved sensitivity. Aims. We use G21.5-0.9, a pulsar-wind nebula with a time-constant power-law spectrum and a flux of a few milli-Crab in the X-ray band, as a viable, fainter substitute to the Crab. Using this source, we conduct a cross-calibration study of the instruments onboard currently active observatories: Chandra ACIS, Suzaku XIS, Swift XRT, and XMM-Newton EPIC (MOS and pn) for the soft-band, and INTEGRAL IBIS-ISGRI, RXTE PCA, and Suzaku HXD-PIN for the hard band. Methods. We extract spectra from all instruments and fit under the same astrophysical assumptions. We compare the spectral parameters of the G21.5-0.9 model: power-law photon index, H-equivalent column density of the interstellar photoelectric absorption, and flux in the soft (2-8 keV) or hard (15-50 keV) energy band. Results. We identify systematic differences in the best-fit parameter values unattributable to statistical scatter of the data alone. We interpret these differences as due to residual cross-calibration problems. The differences can be as large as 20% and 9% for the soft-band flux and power-law index, respectively, and 46% for the hard-band flux. The results are plotted and tabulated as a useful reference for future calibration and scientific studies using multiple missions. C1 [Tsujimoto, M.; Ishida, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan. [Guainazzi, M.; Saxton, R. D.] European Space Agcy, European Space Astron Ctr, Madrid 28691, Spain. [Plucinsky, P. P.; Posson-Brown, J. L. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beardmore, A. P.; Read, A. M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Natalucci, L.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-00133 Rome, Italy. [Shaposhnikov, N. V.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. RP Tsujimoto, M (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshino Dai, Kanagawa 2525210, Japan. EM tsujimot@astro.isas.jaxa.jp RI XRAY, SUZAKU/A-1808-2009 FU Science and Technology Facilities Council FX We thank the members of the IACHEC for sharing their results prior to publication and Marcus G. Kirsch who took a leadership role in setting up this consortium. We acknowledge Dai Takei and Kei Saitou for their help in Suzaku data reduction. A.P.B. and A.M.R. acknowledges support from the Science and Technology Facilities Council. NR 46 TC 58 Z9 58 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2011 VL 525 AR A25 DI 10.1051/0004-6361/201015597 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692ZF UT WOS:000285193700136 ER PT J AU Abdo, AA Ackermann, M Ajello, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Carrigan, S Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Costamante, L Cutini, S Davis, DS Dermer, CD de Palma, F Digel, SW Silva, EDE Drell, PS Dubois, R Dumora, D Favuzzi, C Fegan, SJ Fortin, P Frailis, M Fuhrmann, L Fukazawa, Y Funk, S Fusco, P Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guillemot, L Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hughes, RE Itoh, R Johannesson, G Johnson, AS Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Makeev, A Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nestoras, I Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reyes, LC Ripken, J Ritz, S Romani, RW Roth, M Sadrozinski, HFW Sanchez, D Sander, A Scargle, JD Sgro, C Shaw, MS Smith, PD Spandre, G Spinelli, P Strickman, MS Suson, DJ Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Usher, TL Vandenbroucke, J Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Ylinen, T Ziegler, M Acciari, VA Aliu, E Arlen, T Aune, T Beilicke, M Benbow, W Bottcher, M Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Christiansen, JL Ciupik, L Cui, W Perez, ID Dickherber, R Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Mukherjee, R Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Senturk, GD Smith, AW Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Villata, M Raiteri, CM Gurwell, MA Larionov, VM Kurtanidze, OM Aller, MF Lahteenmaki, A Chen, WP Berduygin, A Agudo, I Aller, HD Arkharov, AA Bach, U Bachev, R Beltrame, P Benitez, E Buemi, CS Dashti, J Calcidese, P Capezzali, D Carosati, D Da Rio, D Di Paola, A Diltz, C Dolci, M Dultzin, D Forne, E Gomez, JL Hagen-Thorn, VA Halkola, A Heidt, J Hiriart, D Hovatta, T Hsiao, HY Jorstad, SG Kimeridze, GN Konstantinova, TS Kopatskaya, EN Koptelova, E Leto, P Ligustri, R Lindfors, E Lopez, JM Marscher, AP Mommert, M Mujica, R Nikolashvili, MG Nilsson, K Palma, N Pasanen, M Roca-Sogorb, M Mommert, M Mujica, R Nikolashvili, MG Nilsson, K Palma, N Pasanen, M Roca-Sogorb, M Ros, JA Roustazadeh, P Sadun, AC Saino, J Sigua, LA Sillanaa, A Sorcia, M Takalo, LO Tornikoski, M Trigilio, C Turchetti, R Umana, G Belloni, T Blake, CH Bloom, JS Angelakis, E Fumagalli, M Hauser, M Prochaska, JX Riquelme, D Sievers, A Starr, DL Tagliaferri, G Ungerechts, H Wagner, S Zensus, JA AF Abdo, A. A. Ackermann, M. Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carrigan, S. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Costamante, L. Cutini, S. Davis, D. S. Dermer, C. D. de Palma, F. Digel, S. W. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Favuzzi, C. Fegan, S. J. Fortin, P. Frailis, M. Fuhrmann, L. Fukazawa, Y. Funk, S. Fusco, P. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guillemot, L. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Itoh, R. Johannesson, G. Johnson, A. S. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Makeev, A. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nestoras, I. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reyes, L. C. Ripken, J. Ritz, S. Romani, R. W. Roth, M. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Scargle, J. D. Sgro, C. Shaw, M. S. Smith, P. D. Spandre, G. Spinelli, P. Strickman, M. S. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Ziegler, M. Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boettcher, M. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Christiansen, J. L. Ciupik, L. Cui, W. de la Calle Perez, I. Dickherber, R. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Mukherjee, R. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Smith, A. W. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Villata, M. Raiteri, C. M. Gurwell, M. A. Larionov, V. M. Kurtanidze, O. M. Aller, M. F. Lahteenmaki, A. Chen, W. P. Berduygin, A. Agudo, I. Aller, H. D. Arkharov, A. A. Bach, U. Bachev, R. Beltrame, P. Benitez, E. Buemi, C. S. Dashti, J. Calcidese, P. Capezzali, D. Carosati, D. Da Rio, D. Di Paola, A. Diltz, C. Dolci, M. Dultzin, D. Forne, E. Gomez, J. L. Hagen-Thorn, V. A. Halkola, A. Heidt, J. Hiriart, D. Hovatta, T. Hsiao, H. -Y. Jorstad, S. G. Kimeridze, G. N. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Leto, P. Ligustri, R. Lindfors, E. Lopez, J. M. Marscher, A. P. Mommert, M. Mujica, R. Nikolashvili, M. G. Nilsson, K. Palma, N. Pasanen, M. Roca-Sogorb, M. Mommert, M. Mujica, R. Nikolashvili, M. G. Nilsson, K. Palma, N. Pasanen, M. Roca-Sogorb, M. Ros, J. A. Roustazadeh, P. Sadun, A. C. Saino, J. Sigua, L. A. Sillanaa, A. Sorcia, M. Takalo, L. O. Tornikoski, M. Trigilio, C. Turchetti, R. Umana, G. Belloni, T. Blake, C. H. Bloom, J. S. Angelakis, E. Fumagalli, M. Hauser, M. Prochaska, J. X. Riquelme, D. Sievers, A. Starr, D. L. Tagliaferri, G. Ungerechts, H. Wagner, S. Zensus, J. A. CA Fermi-Lat Collaboration VERITAS Collaboration GASP-WEBT Consortium TI MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING GAMMA-RAY BLAZAR 3C 66A IN 2008 OCTOBER SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (3C 66A); galaxies: active; gamma rays: galaxies ID BL LACERTAE OBJECTS; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SPECTRAL ENERGY-DISTRIBUTION; EPOCH VLBI SURVEY; BRIGHT BLAZARS; RADIO-SOURCES; TEV BLAZARS; BACKGROUND-RADIATION; VERITAS OBSERVATIONS AB The BL Lacertae object 3C 66A was detected in a flaring state by the Fermi Large Area Telescope (LAT) and VERITAS in 2008 October. In addition to these gamma-ray observations, F-GAMMA, GASP-WEBT, PAIRITEL, MDM, ATOM, Swift, and Chandra provided radio to X-ray coverage. The available light curves show variability and, in particular, correlated flares are observed in the optical and Fermi-LAT gamma-ray band. The resulting spectral energy distribution can be well fitted using standard leptonic models with and without an external radiation field for inverse Compton scattering. It is found, however, that only the model with an external radiation field can accommodate the intra-night variability observed at optical wavelengths. C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, CNRS, IRFU, CEA,Lab AIM,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Conrad, J.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Chekhtman, A.; Fegan, S. J.; Fortin, P.; Horan, D.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Cutini, S.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Celik, Oe.; Davis, D. S.; Hays, E.; Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA. [Celik, Oe.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, Oe.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Conrad, J.; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Ripken, J.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Dumora, D.; Guillemot, L.; Lott, B.] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Guillemot, L.; Lott, B.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Frailis, M.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy. [Fuhrmann, L.; Guillemot, L.; Nestoras, I.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Fukazawa, Y.; Itoh, R.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.; Vilchez, N.] Ctr Etud Spatiale Rayonnements, CNRS UPS, F-31028 Toulouse 4, France. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Scargle, J. D.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Christiansen, J. L.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [de la Calle Perez, I.] European Space Agcy, European Space Astron Ctr INSA ESAC, Satellite Tracking Stn, E-28080 Madrid, Spain. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, Turin, Italy. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Larionov, V. M.; Hagen-Thorn, V. A.; Konstantinova, T. S.; Kopatskaya, E. N.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Larionov, V. M.; Hagen-Thorn, V. A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Kurtanidze, O. M.; Kimeridze, G. N.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia. [Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lahteenmaki, A.; Hovatta, T.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Helsinki, Finland. [Chen, W. P.; Hsiao, H. -Y.; Koptelova, E.] Natl Cent Univ, Inst Astron, Chungli, Taiwan. [Berduygin, A.; Halkola, A.; Lindfors, E.; Pasanen, M.; Pasanen, M.; Saino, J.; Sillanaa, A.; Takalo, L. O.] Univ Turku, Dept Phys & Astron, Tuorla Observ, SF-20500 Turku, Finland. [Agudo, I.; Gomez, J. L.; Roca-Sogorb, M.; Roca-Sogorb, M.] CSIC, Inst Astrofis Andalucia, Madrid, Spain. [Bachev, R.] Bulgarian Acad Sci, Inst Astron, BG-1040 Sofia, Bulgaria. [Benitez, E.; Dultzin, D.; Sorcia, M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy. [Dashti, J.; Diltz, C.; Palma, N.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Di Paola, A.] Osserv Astron Roma, INAF, Rome, Italy. [Heidt, J.; Mommert, M.] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany. [Hiriart, D.; Lopez, J. M.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. Inst Planetary Res, DLR, D-12489 Berlin, Germany. [Mujica, R.] INAOE, Puebla 72000, Mexico. [Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO USA. [Belloni, T.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Blake, C. H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bloom, J. S.; Starr, D. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Angelakis, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Fumagalli, M.; Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Hauser, M.; Wagner, S.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany. [Prochaska, J. X.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Riquelme, D.; Sievers, A.; Ungerechts, H.] IRAM, E-18012 Granada, Spain. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM lreyes@kicp.uchicago.edu RI Fumagalli, Michele/K-9510-2015; Johnson, Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Funk, Stefan/B-7629-2015; Agudo, Ivan/G-1701-2015; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Thompson, David/D-2939-2012; Hays, Elizabeth/D-3257-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Lahteenmaki, Anne/L-5987-2013 OI Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Tagliaferri, Gianpiero/0000-0003-0121-0723; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Gargano, Fabio/0000-0002-5055-6395; Angelakis, Emmanouil/0000-0001-7327-5441; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; Cui, Wei/0000-0002-6324-5772; Frailis, Marco/0000-0002-7400-2135; Cesarini, Andrea/0000-0002-8611-8610; Caraveo, Patrizia/0000-0003-2478-8018; Leto, Paolo/0000-0003-4864-2806; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X; Ward, John E/0000-0003-1973-0794; Raiteri, Claudia Maria/0000-0003-1784-2784; Fumagalli, Michele/0000-0001-6676-3842; Dolci, Mauro/0000-0001-8000-5642; Buemi, Carla Simona/0000-0002-7288-4613; Villata, Massimo/0000-0003-1743-6946; Umana, Grazia/0000-0002-6972-8388; giommi, paolo/0000-0002-2265-5003; Di Paola, Andrea/0000-0002-2189-8644; Funk, Stefan/0000-0002-2012-0080; Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; FU NASA [NNX08AU13G, NNG06GH50G, GO8-9100X]; Harvard University; Academy of Finland; Georgian National Science Foundation [GNSF/ST08/4-404]; Russian RFBR foundation [09-02-00092]; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-0114422, NSF PHY-0551142]; Fermilab; Kavli Institute for Cosmological Physics; University of Chicago FX The VERITAS collaboration also acknowledges the excel-lent work of the technical support staff at the FLWO and the collaborating institutions in the construction and operation of the instrument, as well as support from the NASA/Swift guest investigator program (grant NNX08AU13G) for the Swift observations.; PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, a camera loan from the University of Virginia, and continued support of the SAO and UC Berkeley. The PAIRITEL project is further supported by NASA/Swift Guest Investigator grant NNG06GH50G. This research is partly based on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg and has also made use of observations with the IRAM 30 m telescope. The Metsahovi team acknowledges the support from the Academy of Finland. The Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST08/4-404. The St. Petersburg University team acknowledges support from Russian RFBR foundation via grant 09-02-00092. AZT-24 observations are made within an agreement between Pulkovo, Rome, and Teramo observatories.; L. C. Reyes acknowledges the support by the Kavli Institute for Cosmological Physics at the University of Chicago through grants NSF PHY-0114422 and NSF PHY-0551142 and an endowment from the Kavli Foundation and its founder Fred Kavli. M. Bottcher acknowledges support from NASA through Chandra Guest Investigator Grant GO8-9100X. Some of the VERITAS simulations used in this work have been performed on the joint Fermilab-KICP supercomputing cluster, supported by grants from Fermilab, the Kavli Institute for Cosmological Physics, and the University of Chicago. NR 74 TC 44 Z9 44 U1 5 U2 21 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN PY 2011 VL 726 IS 1 AR 43 DI 10.1088/0004-637X/726/1/43 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300043 ER PT J AU Engell, AJ Siarkowski, M Gryciuk, M Sylwester, J Sylwester, B Golub, L Korreck, K Cirtain, J AF Engell, Alexander J. Siarkowski, Marek Gryciuk, Magda Sylwester, Janusz Sylwester, Barbara Golub, Leon Korreck, Kelly Cirtain, Jonathan TI FLARES AND THEIR UNDERLYING MAGNETIC COMPLEXITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: flares; Sun: magnetic topology; Sun: photosphere; Sun: X-rays; gamma rays ID X-RAY TELESCOPE; REGION TRANSIENT BRIGHTENINGS; SOLAR-A MISSION; EMERGING FLUX; TEMPERATURE DIAGRAM; ACTIVE REGIONS; HINODE MISSION; CORONA; LOOPS; MORPHOLOGY AB SphinX (Solar PHotometer IN X-rays), a full-disk-integrated spectrometer, observed 137 flare-like/transient events with active region (AR) 11024 being the only AR on disk. The Hinode X-Ray Telescope (XRT) and Solar Optical Telescope observe 67 of these events and identified their location from 12: 00 UT on July 3 through 24: 00 UT 2009 July 7. We find that the predominant mechanisms for flares observed by XRT are (1) flux cancellation and (2) the shearing of underlying magnetic elements. Point-and cusp-like flare morphologies seen by XRT all occur in a magnetic environment where one polarity is impeded by the opposite polarity and vice versa, forcing the flux cancellation process. The shearing is either caused by flux emergence at the center of the AR and separation of polarities along a neutral line or by individual magnetic elements having a rotational motion. Both mechanisms are observed to contribute to single-and multiple-loop flares. We observe that most loop flares occur along a large portion of a polarity inversion line. Point-and cusp-like flares become more infrequent as the AR becomes organized with separation of the positive and negative polarities. SphinX, which allows us to identify when these flares occur, provides us with a statistically significant temperature and emission scaling law for A and B class flares: EM = 6.1 x 10(33) T-1.9 +/- 0.1. C1 [Engell, Alexander J.; Golub, Leon; Korreck, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Siarkowski, Marek; Gryciuk, Magda; Sylwester, Janusz; Sylwester, Barbara] Polish Acad Sci, Space Res Ctr, PL-51622 Wroclaw, Poland. [Cirtain, Jonathan] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Engell, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM aengell@cfa.harvard.edu OI Golub, Leon/0000-0001-9638-3082 FU NASA [NNM07AA02C]; Polish Ministry of Education and Science [N203 381736]; European Commission [218816] FX We sincerely thank the referee for comments and suggestions that have strengthened the paper. We also thank Gemma Attrill, Paolo Grigis, Greg Slater, Ted Tarbell, Paola Testa, and Aad van Ballegooijen for useful discussions. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). A. E., L. G., and K. K. are supported in part by NASA grant NNM07AA02C to the Smithsonian Astrophysical Observatory. M. S., M. G., B. S., and J.S. acknowledge the support from the Polish Ministry of Education and Science Grant No. N203 381736. The research leading to these results received partial funding from the European Commission's Seventh Framework Programme (FP7/2007-2013) under the grant agreement No. 218816 (SOTERIA project, http://soteria-space.eu). NR 31 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN PY 2011 VL 726 IS 1 AR 12 DI 10.1088/0004-637X/726/1/12 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300012 ER PT J AU Gilliland, RL McCullough, PR Nelan, EP Brown, TM Charbonneau, D Nutzman, P Christensen-Dalsgaard, J Kjeldsen, H AF Gilliland, Ronald L. McCullough, Peter R. Nelan, Edmund P. Brown, Timothy M. Charbonneau, David Nutzman, Philip Christensen-Dalsgaard, Jorgen Kjeldsen, Hans TI ASTEROSEISMOLOGY OF THE TRANSITING EXOPLANET HOST HD 17156 WITH HUBBLE SPACE TELESCOPE FINE GUIDANCE SENSOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 17156); stars: oscillations; techniques: photometric ID SOLAR-LIKE OSCILLATIONS; LIGHT-CURVE; Y-2 ISOCHRONES; PLANET; STELLAR; STARS; PARAMETERS; SYSTEM; SEARCH; PERIOD AB Observations conducted with the Fine Guidance Sensor on the Hubble Space Telescope (HST) providing high cadence and precision time-series photometry were obtained over 10 consecutive days in 2008 December on the host star of the transiting exoplanet HD 17156b. During this time, 1.0 x 10(12) photons (corrected for detector dead time) were collected in which a noise level of 163 parts per million per 30 s sum resulted, thus providing excellent sensitivity to the detection of the analog of the solar 5-minute p-mode oscillations. For HD 17156, robust detection of p modes supports the determination of the stellar mean density of = 0.5301 +/- 0.0044 g cm(-3) from a detailed fit to the observed frequencies of modes of degree l = 0, 1, and 2. This is the first star for which the direct determination of has been possible using both asteroseismology and detailed analysis of a transiting planet light curve. Using the density constraint from asteroseismology, and stellar evolution modeling results in M-* = 1.285 +/- 0.026 M-circle dot, R-* = 1.507 +/- 0.012 R-circle dot, and a stellar age of 3.2 +/- 0.3 Gyr. C1 [Gilliland, Ronald L.; McCullough, Peter R.; Nelan, Edmund P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Charbonneau, David; Nutzman, Philip] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Gilliland, RL (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM gillil@stsci.edu OI Charbonneau, David/0000-0002-9003-484X FU NASA [NAS 5-26555]; STScI [GO/DD-11945] FX Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.; Coming at a time of significant stress on the HST project these observations required the expert assistance of many individuals to develop and execute. Especially noteworthy were the skill and tireless efforts provided by Merle Reinhart at STScI in expertly crafting the Phase II program to use all available observing time in the orbits allocated, and the efforts from Mike Wenz at Goddard Space Flight Center for shepherding the proposal through pre-flight reviews and monitoring engineering performance during execution. We thank the STScI Director, Matt Mountain, for the generous DD time award that made these results possible. We thank Matt Holman and Jeff Valenti for discussion. Financial support for this work was provided through program GO/DD-11945 from STScI. NR 47 TC 28 Z9 28 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 JAN PY 2011 VL 726 IS 1 AR 2 DI 10.1088/0004-637X/726/1/2 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300002 ER PT J AU Glass, L Ferrarese, L Cote, P Jordan, A Peng, E Blakeslee, JP Chen, CW Infante, L Mei, S Tonry, JL West, MJ AF Glass, Lisa Ferrarese, Laura Cote, Patrick Jordan, Andres Peng, Eric Blakeslee, John P. Chen, Chin-Wei Infante, Leopoldo Mei, Simona Tonry, John L. West, Michael J. TI THE ACS FORNAX CLUSTER SURVEY. IV. DEPROJECTION OF THE SURFACE BRIGHTNESS PROFILES OF EARLY-TYPE GALAXIES IN THE VIRGO AND FORNAX CLUSTERS: INVESTIGATING THE "CORE/POWER-LAW DICHOTOMY" SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Virgo, Fornax); galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies: nuclei; galaxies: structure ID HUBBLE-SPACE-TELESCOPE; SUPERMASSIVE BLACK-HOLES; ELLIPTIC GALAXIES; EXTRA LIGHT; MERGER REMNANTS; CENTRAL REGIONS; DISTANCE; CENTERS; NUCLEI; DISSIPATION AB Although early observations with the Hubble Space Telescope (HST) pointed to a sharp dichotomy among early-type galaxies in terms of the logarithmic slope gamma' of their central surface brightness profiles, several studies in the past few years have called this finding into question. In particular, recent imaging surveys of 143 early-type galaxies belonging to the Virgo and Fornax Clusters using the Advanced Camera for Surveys (ACS) on board HST have not found a dichotomy in gamma', but instead a systematic progression from central luminosity deficit to excess relative to the inward extrapolation of the best-fitting global Sersic model. Given that earlier studies also found that the dichotomy persisted when analyzing the deprojected density profile slopes, we investigate the distribution of the three-dimensional luminosity density profiles of the ACS Virgo and Fornax Cluster Survey galaxies. Having fitted the surface brightness profiles with modified Sersic models, we then deproject the galaxies using an Abel integral and measure the inner slopes gamma(3D) of the resulting luminosity density profiles at various fractions of the effective radius R-e. We find no evidence of a dichotomy, but rather, a continuous variation in the central luminosity profiles as a function of galaxy magnitude. We introduce a parameter, Delta(3D), that measures the central deviation of the deprojected luminosity profiles from the global Sersic fit, showing that this parameter varies smoothly and systematically along the luminosity function. C1 [Glass, Lisa] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Glass, Lisa; Ferrarese, Laura; Cote, Patrick; Blakeslee, John P.; Chen, Chin-Wei] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Jordan, Andres; Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peng, Eric] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Peng, Eric] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Chen, Chin-Wei] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Mei, Simona] Univ Paris Denis Diderot, Bur Galaxies Etoiles Phys Instrumentat GEPI, F-75205 Paris 13, France. [Mei, Simona] Observ Paris, Sect Meudon, GEPI, F-92195 Meudon, France. [Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [West, Michael J.] European So Observ, Santiago 19, Chile. RP Glass, L (reprint author), Univ Victoria, Dept Phys & Astron, POB 3055, Victoria, BC V8W 3P6, Canada. OI Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548 FU STScI [GO-9401, GO-10217]; NASA [NAS5-26555]; NSERC; University of Victoria FX The authors would like to thank the anonymous referee for suggestions, which improved the manuscript. L. G. thanks Thomas Puzia and Chien Peng for all of their help and suggestions. Support for programs GO-9401 and GO-10217 was provided through grants from STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555. The authors gratefully acknowledge support from NSERC through the Discovery and Postgraduate Scholarship programs, as well as from the University of Victoria through their fellowship program. NR 58 TC 20 Z9 20 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 JAN PY 2011 VL 726 IS 1 AR 31 DI 10.1088/0004-637X/726/1/31 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300031 ER PT J AU Hartman, JD Bakos, GA Sato, B Torres, G Noyes, RW Latham, DW Kovacs, G Fischer, DA Howard, AW Johnson, JA Marcy, GW Buchhave, LA Furesz, G Perumpilly, G Beky, B Stefanik, RP Sasselov, DD Esquerdo, GA Everett, M Csubry, Z Lazar, J Papp, I Sari, P AF Hartman, J. D. Bakos, G. A. Sato, B. Torres, G. Noyes, R. W. Latham, D. W. Kovacs, G. Fischer, D. A. Howard, A. W. Johnson, J. A. Marcy, G. W. Buchhave, L. A. Fueresz, G. Perumpilly, G. Beky, B. Stefanik, R. P. Sasselov, D. D. Esquerdo, G. A. Everett, M. Csubry, Z. Lazar, J. Papp, I. Sari, P. TI HAT-P-18b AND HAT-P-19b: TWO LOW-DENSITY SATURN-MASS PLANETS TRANSITING METAL-RICH K STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-18, GSC 2594-00646, HAT-P-19, GSC 2283-00589); techniques: photometric; techniques: spectroscopic ID ECLIPSING BINARIES; EXTRASOLAR PLANETS; BRIGHT STAR; SOLAR METALLICITY; ECCENTRIC ORBIT; OPEN CLUSTERS; KEPLER FIELD; SUB-SATURN; HOT; STELLAR AB We report the discovery of two new transiting extrasolar planets. HAT-P-18b orbits the V = 12.759 K2 dwarf star GSC 2594-00646, with a period P = 5.508023 +/- 0.000006 days, transit epoch T-c = 2454715.02174 +/- 0.00020 (BJD), and transit duration 0.1131 +/- 0.0009 days. The host star has a mass of 0.77 +/- 0.03 M-circle dot, radius of 0.75 +/- 0.04R(circle dot), effective temperature 4803 +/- 80 K, and metallicity [Fe/H] = +0.10 +/- 0.08. The planetary companion has a mass of 0.197 +/- 0.013 M-J and radius of 0.995 +/- 0.052 R-J, yielding a mean density of 0.25 +/- 0.04 g cm(-3). HAT-P-19b orbits the V = 12.901 K1 dwarf star GSC 2283-00589, with a period P = 4.008778 +/- 0.000006 days, transit epoch T-c = 2455091.53417 +/- 0.00034 (BJD), and transit duration 0.1182 +/- 0.0014 days. The host star has a mass of 0.84 +/- 0.04 M-circle dot, radius of 0.82 +/- 0.05 R-circle dot, effective temperature 4990 +/- 130 K, and metallicity [Fe/H] = +0.23 +/- 0.08. The planetary companion has a mass of 0.292 +/- 0.018 M-J and radius of 1.132 +/- 0.072 R-J, yielding a mean density of 0.25 +/- 0.04 g cm(-3). The radial velocity residuals for HAT-P-19 exhibit a linear trend in time, which indicates the presence of a third body in the system. Comparing these observations with theoretical models, we find that HAT-P-18b and HAT-P-19b are each consistent with a hydrogen-helium-dominated gas giant planet with negligible core mass. HAT-P-18b and HAT-P-19b join HAT-P-12b and WASP-21b in an emerging group of low-density Saturn-mass planets, with negligible inferred core masses. However, unlike HAT-P-12b and WASP-21b, both HAT-P-18b and HAT-P-19b orbit stars with super-solar metallicity. This calls into question the heretofore suggestive correlation between the inferred core mass and host star metallicity for Saturn-mass planets. C1 [Hartman, J. D.; Bakos, G. A.; Torres, G.; Noyes, R. W.; Latham, D. W.; Buchhave, L. A.; Fueresz, G.; Perumpilly, G.; Beky, B.; Stefanik, R. P.; Sasselov, D. D.; Esquerdo, G. A.; Everett, M.; Csubry, Z.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sato, B.] Tokyo Inst Technol, Global Edge Inst, Tokyo 152, Japan. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Fischer, D. A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Howard, A. W.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Johnson, J. A.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Perumpilly, G.] Univ S Dakota, Dept Phys, Vermillion, SD 57069 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 FU NOAO [A146Hr, A201Hr, A264Hr, G329Hr]; NASA [N018Hr, N049Hr, N128Hr, N167Hr, NNG04GN74G, NNX08AF23G, NNX09AF59G, NCC2-1390]; SAO; NSF [AST-0702843, AST-0702821]; Hungarian Scientific Research Foundation (OTKA) [K-81373] FX Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology. Keck time has been granted by NOAO (A146Hr, A201Hr, and A264Hr), NASA (N018Hr, N049Hr, N128Hr, and N167Hr), and by the NOAO Keck-Gemini time exchange program (G329Hr). Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Based in part on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.; HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G and SAO IR&D grants. Work of G.A.B. and J.A.J. were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G.T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (D.W.L., PI). G.K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. This research has made use of Keck telescope time granted through NOAO (programs A146Hr, A201Hr, and A264Hr), NASA (programs N018Hr, N049Hr, N128Hr, and N167Hr), and through the NOAO Keck-Gemini time exchange program (program G329Hr). NR 61 TC 34 Z9 34 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN PY 2011 VL 726 IS 1 AR 52 DI 10.1088/0004-637X/726/1/52 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300052 ER PT J AU Hoekstra, H Donahue, M Conselice, CJ McNamara, BR Voit, GM AF Hoekstra, Henk Donahue, Megan Conselice, Christopher J. McNamara, Brian R. Voit, G. Mark TI THE MASS-L-x RELATION FOR MODERATE LUMINOSITY X-RAY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark matter; X-rays: galaxies: clusters ID HUBBLE-SPACE-TELESCOPE; WEAK LENSING ANALYSIS; GALAXY CLUSTERS; COSMOLOGICAL CONSTRAINTS; PHOTOMETRIC REDSHIFTS; SCALING RELATIONS; OBSERVED GROWTH; ADVANCED CAMERA; DEEP FIELD; SKY SURVEY AB We present measurements of the masses of a sample of 25 moderate X-ray luminosity clusters of galaxies from the 160 square degree ROSAT survey. The masses were obtained from a weak-lensing analysis of deep F814W images obtained using the Advanced Camera for Surveys. We present an accurate empirical correction for the effect of charge transfer (in)efficiency on the shapes of faint galaxies. A significant lensing signal is detected around most of the clusters. The lensing mass correlates tightly with the cluster richness. We measured the intrinsic scatter in the scaling relation between M-2500 and L-X to be sigma(log LX)vertical bar M = 0.23(-0.04)(+0.10). The best-fit power-law slope and normalization are found to be alpha = 0.68 +/- 0.07 and M-X = (1.2 +/- 0.12) x h(70)(-1)10(14) M-circle dot (for L-X = 2 x 10(44)h(70)(-2) erg s(-1)). These results agree well with a number of recent studies, but the normalization is lower compared to the study of Rykoff et al. One explanation for this difference may be the fact that (sub) structures projected along the line of sight boost both the galaxy counts and the lensing mass. Such superpositions lead to an increased mass at a given L-X when clusters are binned by richness. C1 [Hoekstra, Henk] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Hoekstra, Henk] Univ Victoria, Dept Phys & Astron, Victoria, BC, Canada. [Donahue, Megan; Voit, G. Mark] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, Brian R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, Brian R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hoekstra, H (reprint author), Leiden Univ, Leiden Observ, Leiden, Netherlands. RI Donahue, Megan/B-5361-2012; Conselice, Christopher/B-4348-2013; OI Conselice, Christopher/0000-0003-1949-7638; Voit, Gerard/0000-0002-3514-0383 FU NSERC; Canadian Institute for Advanced Research (CIfAR); Canadian Foundation for Innovation (CFI); Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO); STScI/HST [HST-GO-10490.01, HST-GO-10152.01]; NASA LTSA [NNG-05GD82G]; Centre National d'Etudes Spatiales (CNES) FX We thank the anonymous referee for useful suggestions that have improved the paper. H. H. acknowledges support by NSERC, the Canadian Institute for Advanced Research (CIfAR) and the Canadian Foundation for Innovation (CFI) as well as a VIDI grant from the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO). H. H. also thanks Andisheh Mahdavi for discussion on fitting relations with intrinsic scatter. M. D. and G. M. V. acknowledge the support of two STScI/HST grants (HST-GO-10490.01 HST-GO-10152.01) and a NASA LTSA grant (NNG-05GD82G). This research has made use of the X-Rays Clusters Database (BAX) which is operated by the Laboratoire d'Astrophysique de Tarbes-Toulouse (LATT), under contract with the Centre National d'Etudes Spatiales (CNES). NR 63 TC 28 Z9 28 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 JAN PY 2011 VL 726 IS 1 AR 48 DI 10.1088/0004-637X/726/1/48 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300048 ER PT J AU Koenig, XP Allen, LE AF Koenig, Xavier P. Allen, Lori E. TI DISK EVOLUTION IN W5: INTERMEDIATE-MASS STARS AT 2-5 Myr SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; infrared: stars; protoplanetary disks; stars: pre-main sequence; techniques: spectroscopic ID HERBIG AE/BE STARS; MULTIBAND IMAGING PHOTOMETER; PROTOPLANETARY DISKS; SPITZER OBSERVATIONS; IRAS OBSERVATIONS; FORMING REGIONS; YOUNG CLUSTERS; NEARBY STAR; ACCRETION; MMT AB We present the results of a survey of young intermediate-mass stars (age < 5 Myr, 1.5M(circle dot) < M-star <= 15M(circle dot)) in the W5 massive star-forming region. We use combined optical, near-infrared, and Spitzer Space Telescope photometry and optical spectroscopy to define a sample of stars of spectral types A and B and examine their infrared excess properties. We find objects with infrared excesses characteristic of optically thick disks, i.e., Herbig AeBe stars. These stars are rare: <1.5% of the entire spectroscopic sample of A and B stars, and absent among stars more massive than 2.4M(circle dot). 7.5% of the A and B stars possess infrared excesses in a variety of morphologies that suggest their disks are in some transitional phase between an initial, optically thick accretion state and later evolutionary states. We identify four morphological classes based on the wavelength dependence of the observed excess emission above theoretical photospheric levels: (1) the optically thick disks; (2) disks with an optically thin excess over the wavelength range 2-24 mu m, similar to that shown by Classical Be stars; (3) disks that are optically thin in their inner regions based on their infrared excess at 2-8 mu m and optically thick in their outer regions based on the magnitude of the observed excess emission at 24 mu m; (4) disks that exhibit empty inner regions (no excess emission at lambda <= 8 mu m) and some measurable excess emission at 24 mu m. A sub-class of disks exhibit no significant excess emission at lambda <= 5.8 mu m, have excess emission only in the Spitzer 8 mu m band and no detection at 24 mu m. We discuss these spectral energy distribution types, and suggest physical models for disks exhibiting these emission patterns and additional observations to test these theories. C1 [Koenig, Xavier P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, Lori E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Koenig, XP (reprint author), NASA GSFC, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. OI Koenig, Xavier/0000-0002-9478-4170 FU NASA; National Science Foundation FX The authors thank Steve Strom and Sidney Wolff, Joan Najita, James Muzerolle, Lee Hartmann and Nuria Calvet, Uma Gorti and Dave Hollenbach for extensive and useful discussions on disks and young stars. This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of NASA's Astrophysics Data System. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 61 TC 4 Z9 4 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 JAN PY 2011 VL 726 IS 1 AR 18 DI 10.1088/0004-637X/726/1/18 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300018 ER PT J AU Nutzman, P Gilliland, RL McCullough, PR Charbonneau, D Christensen-Dalsgaard, J Kjeldsen, H Nelan, EP Brown, TM Holman, MJ AF Nutzman, Philip Gilliland, Ronald L. McCullough, Peter R. Charbonneau, David Christensen-Dalsgaard, Jorgen Kjeldsen, Hans Nelan, Edmund P. Brown, Timothy M. Holman, Matthew J. TI PRECISE ESTIMATES OF THE PHYSICAL PARAMETERS FOR THE EXOPLANET SYSTEM HD 17156 ENABLED BY HUBBLE SPACE TELESCOPE FINE GUIDANCE SENSOR TRANSIT AND ASTEROSEISMIC OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 17156); stars: oscillations; techniques: photometric ID SPIN-ORBIT ALIGNMENT; EXTRASOLAR PLANET; LIGHT-CURVE; ECCENTRIC ORBIT; Y-2 ISOCHRONES; GIANT PLANET; ATMOSPHERE; STELLAR; BRIGHTNESS; SPECTRUM AB We present observations of three distinct transits of HD 17156b obtained with the Fine Guidance Sensors on board the Hubble Space Telescope. We analyzed both the transit photometry and previously published radial velocities to find the planet-star radius ratio R-p/R-star = 0.07454 +/- 0.00035, inclination i = 86.49(-0.20)(+0.24) deg, and scaled semimajor axis a/R-star = 23.19(-0.27)(+0.32). This last value translates directly to a mean stellar density determination. rho(star) = 0.522(-0.018)(+0.021) g cm(-3). Analysis of asteroseismology observations by the companion paper of Gilliland et al. provides a consistent but significantly refined measurement of rho(star) = 0.5308 +/- 0.0040. We compare stellar isochrones to this density estimate and find M-star = 1.275 +/- 0.018 M-circle dot and a stellar age of 3.37(-0.47)(+0.20) Gyr. Using this estimate of M-star and incorporating the density constraint from asteroseismology, we model both the photometry and published radial velocities to estimate the planet radius R-p = 1.0870 +/- 0.0066 R-J and the stellar radius R-star = 1.5007 +/- 0.0076 R-circle dot. The planet radius is larger than that found in previous studies and consistent with theoretical models of a solar-composition gas giant of the same mass and equilibrium temperature. For the three transits, we determine the times of mid-transit to a precision of 6.2 s, 7.6 s, and 6.9 s, and the transit times for HD 17156 do not show any significant departures from a constant period. The joint analysis of transit photometry and asteroseismology presages similar studies that will be enabled by the NASA Kepler Mission. C1 [Nutzman, Philip; Charbonneau, David; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald L.; McCullough, Peter R.; Nelan, Edmund P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. RP Nutzman, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pnutzman@cfa.harvard.edu OI Charbonneau, David/0000-0002-9003-484X FU Space Telescope Science Institute, NASA [NAS5-26555]; NASA [NAS5-26555] FX Support for Program GO-11945 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.; Based on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 50 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN PY 2011 VL 726 IS 1 AR 3 DI 10.1088/0004-637X/726/1/3 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300003 ER PT J AU Zheng, Z Cen, RY Trac, H Miralda-Escude, J AF Zheng, Zheng Cen, Renyue Trac, Hy Miralda-Escude, Jordi TI RADIATIVE TRANSFER MODELING OF Ly alpha EMITTERS. II. NEW EFFECTS ON GALAXY CLUSTERING SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: halos; galaxies: high-redshift; galaxies: statistics; intergalactic medium; large-scale structure of universe; radiative transfer; scattering ID HALO OCCUPATION DISTRIBUTION; STAR-FORMING GALAXIES; GUNN-PETERSON TROUGH; SUBARU DEEP FIELD; EMITTING GALAXIES; LUMINOSITY FUNCTIONS; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; FORMATION HISTORY; REDSHIFT-SPACE AB We study the clustering properties of z similar to 5.7 Ly alpha emitters (LAEs) in a cosmological reionization simulation with a full Ly alpha radiative transfer calculation. Ly alpha radiative transfer substantially modifies the intrinsic Ly alpha emission properties, compared to observed ones, depending on the density and velocity structure environment around the Ly alpha-emitting galaxy. This environment-dependent Ly alpha selection introduces new features in LAE clustering, suppressing (enhancing) the line-of-sight (transverse) density fluctuations and giving rise to scale-dependent galaxy bias. In real space, the contours of the three-dimensional two-point correlation function of LAEs appear to be prominently elongated along the line of sight on large scales, an effect that is opposite to and much stronger than the linear redshift-space distortion effect. The projected two-point correlation function is greatly enhanced in amplitude by a factor of up to a few, compared to the case without the environment-dependent selection effect. The new features in LAE clustering can be understood with a simple, physically motivated model, where Ly alpha selection depends on matter density, velocity, and their gradients. We discuss the implications and consequences of the effects on galaxy clustering from Ly alpha selection in interpreting clustering measurements and in constraining cosmology and reionization from LAEs. C1 [Zheng, Zheng] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Cen, Renyue] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Trac, Hy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Miralda-Escude, Jordi] Inst Catalana Recerca & Estudis Avancats, Barcelona, Catalonia, Spain. [Miralda-Escude, Jordi] Univ Barcelona, Inst Ciencies Cosmos, Barcelona, Catalonia, Spain. RP Zheng, Z (reprint author), Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. EM zheng.zheng@yale.edu RI Trac, Hy/N-8838-2014; OI Trac, Hy/0000-0001-6778-3861; Miralda-Escude, Jordi/0000-0002-2316-8370 NR 67 TC 35 Z9 35 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN PY 2011 VL 726 IS 1 AR 38 DI 10.1088/0004-637X/726/1/38 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695ZI UT WOS:000285411300038 ER PT J AU Agudo, I Jorstad, SG Marscher, AP Larionov, VM Gomez, JL Lahteenmaki, A Gurwell, M Smith, PS Wiesemeyer, H Thum, C Heidt, J Blinov, DA D'Arcangelo, FD Hagen-Thorn, VA Morozova, DA Nieppola, E Roca-Sogorb, M Schmidt, GD Taylor, B Tornikoski, M Troitsky, IS AF Agudo, Ivan Jorstad, Svetlana G. Marscher, Alan P. Larionov, Valeri M. Gomez, Jose L. Lahteenmaki, Anne Gurwell, Mark Smith, Paul S. Wiesemeyer, Helmut Thum, Clemens Heidt, Jochen Blinov, Dmitriy A. D'Arcangelo, Francesca D. Hagen-Thorn, Vladimir A. Morozova, Daria A. Nieppola, Elina Roca-Sogorb, Mar Schmidt, Gary D. Taylor, Brian Tornikoski, Merja Troitsky, Ivan S. TI LOCATION OF gamma-RAY FLARE EMISSION IN THE JET OF THE BL LACERTAE OBJECT OJ287 MORE THAN 14 pc FROM THE CENTRAL ENGINE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (OJ287); galaxies: active; galaxies: jets; gamma rays: general; polarization; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; BASE-LINE ARRAY; EGRET-DETECTED QUASARS; BLAZAR 3C 279; POLARIMETRIC OBSERVATIONS; HIGH-FREQUENCIES; BRIGHT BLAZARS; RADIO-SOURCES; TIME-SCALES; INNER JET AB We combine time-dependent multi-waveband flux and linear polarization observations with submilliarc-second-scale polarimetric images at gimel = 7 mm of the BL Lacertae type blazar OJ287 to locate the gamma-ray emission in prominent flares in the jet of the source > 14 pc from the central engine. We demonstrate a highly significant correlation between the strongest gamma-ray and millimeter-wave flares through Monte Carlo simulations. The two reported gamma-ray peaks occurred near the beginning of two major millimeter-wave outbursts, each of which is associated with a linear polarization maximum at millimeter wavelengths. Our very long baseline array observations indicate that the two millimeter-wave flares originated in the second of two features in the jet that are separated by > 14 pc. The simultaneity of the peak of the higher-amplitude gamma-ray flare and the maximum in polarization of the second jet feature implies that the gamma-ray and millimeter-wave flares are cospatial and occur > 14 pc from the central engine. We also associate two optical flares, accompanied by sharp polarization peaks, with the two. -ray events. The multi-waveband behavior is most easily explained if the gamma-rays arise from synchrotron self-Compton scattering of optical photons from the flares. We propose that flares are triggered by interaction of moving plasma blobs with a standing shock. The gamma-ray and optical emission is quenched by inverse Compton losses as synchrotron photons from the newly shocked plasma cross the emission region. The millimeter-wave polarization is high at the onset of a flare, but decreases as the electrons emitting at these wavelengths penetrate less polarized regions. C1 [Agudo, Ivan; Jorstad, Svetlana G.; Marscher, Alan P.; D'Arcangelo, Francesca D.; Taylor, Brian] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.; Larionov, Valeri M.; Blinov, Dmitriy A.; Hagen-Thorn, Vladimir A.; Morozova, Daria A.; Troitsky, Ivan S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Larionov, Valeri M.; Blinov, Dmitriy A.; Hagen-Thorn, Vladimir A.] St Petersburg Branch, Isaac Newton Inst Chile, St Petersburg, Russia. [Gomez, Jose L.; Roca-Sogorb, Mar] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Lahteenmaki, Anne; Nieppola, Elina; Tornikoski, Merja] Aalto Univ Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wiesemeyer, Helmut] Inst Radio Astron Milimetr, E-18012 Granada, Spain. [Thum, Clemens] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Heidt, Jochen] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany. [D'Arcangelo, Francesca D.] MIT, Lincoln Lab, Lexington, MA 02421 USA. [Nieppola, Elina] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Schmidt, Gary D.] Natl Sci Fdn, Arlington, VA 22230 USA. [Taylor, Brian] Lowell Observ, Flagstaff, AZ 86001 USA. RP Agudo, I (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. EM iagudo@bu.edu RI Larionov, Valeri/H-1349-2013; Blinov, Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Hagen-Thorn, Vladimir/H-3983-2013 OI Larionov, Valeri/0000-0002-4640-4356; Blinov, Dmitry/0000-0003-0611-5784; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Hagen-Thorn, Vladimir/0000-0002-6431-8590 FU NASA [NNX08AJ64G, NNX08AU02G, NNX08AV61G, NNX08AV65G, NNX08AW56S, NNX09AU10G]; NSF [AST-0907893]; Boston University [GSSP07-0009]; St. Petersburg State University [09-02-00092]; MICIIN [AYA2007-67627-C03-03, AYA2010-14844]; CEIC [P09-FQM-4784]; Academy of Finland (Metsahovi) FX The authors thank the referee for constructive comments. This research was funded by NASA grants NNX08AJ64G, NNX08AU02G, NNX08AV61G, and NNX08AV65G, NSF grant AST-0907893, and NRAO award GSSP07-0009 (Boston University), RFBR grant 09-02-00092 (St. Petersburg State University), MICIIN grants AYA2007-67627-C03-03 and AYA2010-14844, and CEIC (Andalucia) grant P09-FQM-4784 (IAA-CSIC), the Academy of Finland (Metsahovi), and NASA grants NNX08AW56S and NNX09AU10G (Steward Observatory). The VLBA is an instrument of the NRAO, a facility of the NSF operated under cooperative agreement by AUI. The PRISM camera at Lowell Observatory was developed by Janes et al., with funding from the NSF, Boston University, and Lowell Observatory. The Calar Alto Observatory is jointly operated by MPIA and IAA-CSIC. The IRAM 30 m Telescope is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The Submillimeter Array is a joint project between the SAO and the Academia Sinica. NR 37 TC 88 Z9 89 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2011 VL 726 IS 1 AR L13 DI 10.1088/2041-8205/726/1/L13 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 694KN UT WOS:000285296600013 ER PT J AU Green, JD Watson, DM Bergin, E Maret, S Melnick, G Sonnentrucker, P Tolls, V Sargent, BA Forrest, WJ Kim, KH Raines, SN AF Green, J. D. Watson, D. M. Bergin, E. Maret, S. Melnick, G. Sonnentrucker, P. Tolls, V. Sargent, B. A. Forrest, W. J. Kim, K. H. Raines, S. N. TI GGD 37: AN EXTREME PROTOSTELLAR OUTFLOW SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Herbig-Haro objects; ISM: clouds; ISM: jets and outflows ID STAR-FORMING REGION; HERBIG-HARO OBJECTS; CEPHEUS-A EAST; SPITZER OBSERVATIONS; X-RAYS; EMISSION; SHOCKS; WEST; GAS; CEP AB We present the first Spitzer-IRS spectral maps of the Herbig-Haro flow GGD 37 detected in lines of [Ne III], [O IV], [Ar III], and [Ne v]. The detection of extended [O IV] (55 eV) and some extended emission in [Ne v] (97 eV) indicates a shock temperature in excess of 100,000 K, in agreement with X-ray observations, and a shock speed in excess of 200 km s(-1). The presence of an extended photoionization or collisional ionization region indicates that GGD 37 is a highly unusual protostellar outflow. C1 [Green, J. D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Watson, D. M.; Forrest, W. J.; Kim, K. H.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Maret, S.] Astrophys Lab, F-38041 Grenoble 9, France. [Melnick, G.; Tolls, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sonnentrucker, P.; Sargent, B. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Raines, S. N.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Green, JD (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. OI Maret, Sebastien/0000-0003-1104-4554 FU Jet Propulsion Laboratory, under NASA [1407]; NASA [1257184]; Jet Propulsion Laboratory (JPL) [960803]; University of Rochester [31419-5714] FX The authors thank Neal Evans, Mike Dunham, Manoj Puravankara, Dave Pooley, and Peter Yoachim for helpful comments and discussion, and Klaus Hodapp for the use of K' images of Cep A. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, under NASA contract 1407. Support for this work was provided by NASA through contract 1257184. This research was supported in part by Jet Propulsion Laboratory (JPL) contract 960803 to Cornell University, and Cornell subcontracts 31419-5714 to the University of Rochester. This research has also made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 30 TC 1 Z9 1 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2011 VL 726 IS 1 AR L1 DI 10.1088/2041-8205/726/1/L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 694KN UT WOS:000285296600001 ER PT J AU Zapata, LA Loinard, L Schmid-Burgk, J Rodriguez, LF Ho, PTP Patel, NA AF Zapata, Luis A. Loinard, Laurent Schmid-Burgk, Johannes Rodriguez, Luis F. Ho, Paul T. P. Patel, Nimesh A. TI DISCOVERY OF AN EXPANDING MOLECULAR BUBBLE IN ORION BN/KL SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (Orion BN/KL); ISM: jets and outflows; ISM: molecules; stars: pre-main sequence; techniques: spectroscopic ID APERTURE SYNTHESIS; PROPER MOTIONS; KLEINMANN-LOW; NEBULA; STAR; KL; ARRAY; REGION; MASERS; SYSTEM AB During their infancy, stars are well known to expel matter violently in the form of well-defined, collimated outflows. A fairly unique exception is found in the Orion Becklin-Neugebauer/Kleinmann-Low star-forming region where a poorly collimated and somewhat disordered outflow composed of numerous elongated "finger-like" structures was discovered more than 30 years ago. In this Letter, we report the discovery in the same region of an even more atypical outflow phenomenon. Using (13)CO(2-1) line observations made with the Submillimeter Array, we have identified there a 500-1000 year old, expanding, roughly spherically symmetric bubble whose characteristics are entirely different from those of known outflows associated with young stellar objects. The center of the bubble coincides with the initial position of a now defunct massive multiple stellar system suspected to have disintegrated 500 years ago and with the center of symmetry of the system of molecular fingers surrounding the Kleinmann-Low nebula. We hypothesize that the bubble is made up of gas and dust that used to be part of the circumstellar material associated with the decayed multiple system. The Orion hot core, recently proposed to be the result of the impact of a shock wave onto a massive dense core, is located toward the southeast quadrant of the bubble. The supersonic expansion of the bubble and/or the impact of some low-velocity filaments provide a natural explanation for its origin. C1 [Zapata, Luis A.; Loinard, Laurent; Rodriguez, Luis F.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Zapata, Luis A.; Schmid-Burgk, Johannes] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Ho, Paul T. P.; Patel, Nimesh A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. RP Zapata, LA (reprint author), UNAM, Ctr Radioastron & Astrofis, Apdo Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. FU DGAPA; UNAM; CONACyT, Mexico; Smithsonian Institution; Academia Sinica FX L.A.Z., L.L., and L.F.R. acknowledge the financial support from DGAPA, UNAM, and CONACyT, Mexico. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 21 TC 15 Z9 15 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2011 VL 726 IS 1 AR L12 DI 10.1088/2041-8205/726/1/L12 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 694KN UT WOS:000285296600012 ER PT J AU Liu, JF AF Liu, Jifeng TI CHANDRA ACIS SURVEY OF X-RAY POINT SOURCES IN 383 NEARBY GALAXIES. I. THE SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: general; X-rays: binaries; X-rays: galaxies ID LUMINOSITY FUNCTION; MONITORING OBSERVATIONS; EXTERNAL GALAXIES; SOURCE POPULATION; MULTIWAVELENGTH PROJECT; BINARY POPULATION; ANTENNAE GALAXIES; DIFFUSE GAS; CONNECTION; STARBURST AB The Chandra data archive is a treasure for various studies, and in this paper we exploit this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axis above 1 arcmin had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures are applied to the 626 ACIS observations and lead to the detection of 28,099 point sources, which belong to 17,599 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing us a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8519 sources within the D-25 isophotes of 351 galaxies, 3305 sources between the D-25 and 2D(25) isophotes of 309 galaxies, and additionally 5735 sources outside 2D(25) isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2D(25) isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of sources within 2D(25) isophotes above 10(39) erg s(-1), 71% of sources above 10(38) erg s(-1), 63% of sources above 10(37) erg s(-1), and 56% of all sources are truly associated with galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L-X (0.3-8 keV) >= 2 x 10(39) erg s(-1)within D-25 isophotes, 179 ULXs between D-25 and 2D(25) isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L-X (0.3-8 keV) >= 2 x 10(38) erg s(-1). With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. C1 [Liu, Jifeng] Natl Astron Observ China, Beijing 100012, Peoples R China. [Liu, Jifeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, JF (reprint author), Natl Astron Observ China, 20 Datun Rd, Beijing 100012, Peoples R China. FU NASA [PF6-70043]; Chinese Academy of Science; China's National Science Foundation [11043009] FX We thank Dr. Frank Primini for his help on Chandra Source Catalog, and Drs. Peppi Fabbiano and Rosanne Di Stefano for helpful discussions. J.F.L. acknowledges the support for this work provided by NASA through the Chandra Fellowship Program (grant PF6-70043), and supports by the Chinese Academy of Science and China's National Science Foundation (grant 11043009). NR 67 TC 52 Z9 52 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2011 VL 192 IS 1 AR 10 DI 10.1088/0067-0049/192/1/10 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700CO UT WOS:000285710500010 ER PT J AU Rots, AH Budavari, T AF Rots, Arnold H. Budavari, Tamas TI DETERMINING THE ABSOLUTE ASTROMETRIC ERROR IN CHANDRA SOURCE CATALOG POSITIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrometry; catalogs; methods: statistical; stars: statistics; X-rays: stars ID DIGITAL SKY SURVEY; CROSS-IDENTIFICATION; GALEX; SDSS AB Although relative errors can readily be calculated, the absolute astrometric accuracy of the source positions in the Chandra Source Catalog (CSC), version 1.0, is a priori unknown. However, the cross-match with stellar objects from the Sloan Digital Sky Survey offers the opportunity to compare the apparent separations of the cross-matched pairs with the formally calculated errors. The analysis of these data allowed us to derive a value of 0 ''.16 for the residual absolute astrometric error in CSC positions. This error will be added to the published position errors in the CSC from now on, starting with CSC, version 1.1. C1 [Rots, Arnold H.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Budavari, Tamas] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Rots, AH (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 67, Cambridge, MA 02138 USA. EM arots@cfa.harvard.edu OI Rots, Arnold/0000-0003-2377-2356 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. NR 7 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2011 VL 192 IS 1 AR 8 DI 10.1088/0067-0049/192/1/8 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700CO UT WOS:000285710500008 ER PT J AU Veefkind, JP Boersma, KF Wang, J Kurosu, TP Krotkov, N Chance, K Levelt, PF AF Veefkind, J. P. Boersma, K. F. Wang, J. Kurosu, T. P. Krotkov, N. Chance, K. Levelt, P. F. TI Global satellite analysis of the relation between aerosols and short-lived trace gases SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID OZONE MONITORING INSTRUMENT; UNITED-STATES; OPTICAL-THICKNESS; TROPOSPHERIC NO2; HIGH-RESOLUTION; GOCART MODEL; EMISSIONS; FORMALDEHYDE; VALIDATION; ALGORITHM AB The spatial and temporal correlations between concurrent satellite observations of aerosol optical thickness (AOT) from the Moderate Resolution Imaging Spectroradiometer (MODIS) and tropospheric columns of nitrogen dioxide (NO2), sulfur dioxide (SO2), and formaldehyde (HCHO) from the Ozone Monitoring Instrument (OMI) are used to infer information on the global composition of aerosol particles. When averaging the satellite data over large regions and longer time periods, we find significant correlation between MODIS AOT and OMI trace gas columns for various regions in the world. This shows that these enhanced aerosol and trace gas concentrations originate from common sources, such as fossil fuel combustion, biomass burning, and organic compounds released from the biosphere. This leads us to propose that satellite-inferred AOT to NO2 ratios for regions with comparable photochemical regimes can be used as indicators for the relative regional pollution control of combustion processes. Indeed, satellites observe low AOT to NO2 ratios over the eastern United States and western Europe, and high AOT to NO2 ratios over comparably industrialized regions in eastern Europe and China. Emission databases and OMI SO2 observations over these regions suggest a much stronger sulfur contribution to aerosol formation than over the well-regulated areas of the eastern United States and western Europe. Furthermore, satellite observations show AOT to NO2 ratios are a factor 100 higher over biomass burning regions than over industrialized areas, reflecting the unregulated burning practices with strong primary particle emissions in the tropics compared to the heavily controlled combustion processes in the industrialized Northern Hemisphere. Simulations with a global chemistry transport model (GEOS-Chem) capture most of these variations, although on regional scales significant differences are found. Wintertime aerosol concentrations show strongest correlations with NO2 throughout most of the Northern Hemisphere. During summertime, AOT is often (also) correlated with enhanced HCHO concentrations, reflecting the importance of secondary organic aerosol formation in that season. We also find significant correlations between AOT and HCHO over biomass burning regions, the tropics in general, and over industrialized regions in southeastern Asia. The distinct summertime maximum in AOT (0.4 at 550 nm) and HCHO over the southeastern United States strengthens existing hypotheses that local emissions of volatile organic compounds lead to the formation of secondary organic aerosols there. GEOS-Chem underestimates the AOT over the southeastern United States by a factor of 2, most likely due to too strong precipitation and too low SOA yield in the model. C1 [Veefkind, J. P.; Boersma, K. F.; Levelt, P. F.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Wang, J.] Univ Nebraska, Lincoln, NE USA. [Kurosu, T. P.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Krotkov, N.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Veefkind, JP (reprint author), Royal Netherlands Meteorol Inst, POB 201, NL-3730 AE De Bilt, Netherlands. EM veefkind@knmi.nl RI Krotkov, Nickolay/E-1541-2012; Boersma, Klaas/H-4559-2012; Pfister, Gabriele/A-9349-2008; Chem, GEOS/C-5595-2014; Wang, Jun/A-2977-2008; OI Krotkov, Nickolay/0000-0001-6170-6750; Boersma, Klaas/0000-0002-4591-7635; Wang, Jun/0000-0002-7334-0490; Chance, Kelly/0000-0002-7339-7577 FU Netherlands Space Office (NSO); NASA FX This work is funded by the Netherlands Space Office (NSO). Jun Wang's participation to this work is supported by the NASA Earth Science New Investigator program. The OMI instrument was contributed by the Netherlands (NSO/KNMI) and Finland (TEKES/FMI) to the NASA EOS-Aura mission. We also acknowledge the MODIS and AERONET mission scientists and associated NASA personnel for the production of the data used in this research effort. NR 60 TC 24 Z9 25 U1 0 U2 21 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2011 VL 11 IS 3 BP 1255 EP 1267 DI 10.5194/acp-11-1255-2011 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 721KW UT WOS:000287354100026 ER PT J AU Lee, CJ Brook, JR Evans, GJ Martin, RV Mihele, C AF Lee, C. J. Brook, J. R. Evans, G. J. Martin, R. V. Mihele, C. TI Novel application of satellite and in-situ measurements to map surface-level NO2 in the Great Lakes region SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; NITROGEN-DIOXIDE; RETRIEVAL; OMI; VALIDATION; SCIAMACHY; GOME AB Ozone Monitoring Instrument (OMI) tropospheric NO2 vertical column density data were used in conjunction with in-situ NO2 concentrations collected by permanently installed monitoring stations to infer 24 h surface-level NO2 concentrations at 0.1 degrees (similar to 11 km) resolution. The region examined included rural and suburban areas, and the highly industrialised area of Windsor, Ontario, which is situated directly across the US-Canada border from Detroit, MI. Photolytic NO2 monitors were collocated with standard NO2 monitors to provide qualitative data regarding NOz interference during the campaign. The accuracy of the OMI-inferred concentrations was tested using two-week integrative NO2 measurements collected with passive monitors at 18 locations, approximating a 15 km grid across the region, for 7 consecutive two-week periods. When compared with these passive results, satellite-inferred concentrations showed an 18% positive bias. The correlation of the passive monitor and OMI-inferred concentrations (R = 0.69, n = 115) was stronger than that for the passive monitor concentrations and OMI column densities (R = 0.52), indicating that using a sparse network of monitoring sites to estimate concentrations improves the direct utility of the OMI observations. OMI-inferred concentrations were then calculated for four years to show an overall declining trend in surface NO2 concentrations in the region. Additionally, by separating OMI-inferred surface concentrations by wind direction, clear patterns in emissions and affected down-wind regions, in particular around the US-Canada border, were revealed. C1 [Lee, C. J.; Evans, G. J.] Univ Toronto, So Ontario Ctr Atmospher Aerosol Res, Dept Chem Engn & Appl Chem, Toronto, ON, Canada. [Brook, J. R.; Mihele, C.] Environm Canada, Sci & Technol Branch, Air Qual Res Div, Downsview, ON, Canada. [Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CJ (reprint author), Univ Toronto, So Ontario Ctr Atmospher Aerosol Res, Dept Chem Engn & Appl Chem, Toronto, ON, Canada. EM colinj.lee@utoronto.ca RI Martin, Randall/C-1205-2014; Evans, Greg/C-7441-2014; Chem, GEOS/C-5595-2014; OI Martin, Randall/0000-0003-2632-8402; Evans, Greg/0000-0002-9641-4499 FU Canadian Foundation for Climate and Atmospheric Sciences FX We would like to thank the Canadian Foundation for Climate and Atmospheric Sciences for funding for this study and the Ontario Ministry of the Environment for providing NO2 data and support for the BAQS-met campaign, and Sandy Benetti for conducting the passive sampling field work and IC analysis. NR 36 TC 14 Z9 15 U1 0 U2 15 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2011 VL 11 IS 22 BP 11761 EP 11775 DI 10.5194/acp-11-11761-2011 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 863AC UT WOS:000298134200030 ER PT J AU Tereszchuk, KA Abad, GG Clerbaux, C Hurtmans, D Coheur, PF Bernath, PF AF Tereszchuk, K. A. Abad, G. Gonzalez Clerbaux, C. Hurtmans, D. Coheur, P. -F. Bernath, P. F. TI ACE-FTS measurements of trace species in the characterization of biomass burning plumes SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TRANSFORM INFRARED-SPECTROSCOPY; ABSORPTION CROSS-SECTIONS; MU-M REGION; ATMOSPHERIC CHEMISTRY; FIRE EMISSIONS; HCN; GASES; CH3CN; CO; AIRCRAFT AB To further our understanding of the effects of biomass burning emissions on atmospheric composition, we report measurements of trace species in biomass burning plumes made by the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) instrument on the SCISAT-1 satellite. An extensive set of 15 molecules, C2H2, C2H6, CH3OH, CH4, CO, H2CO, HCN, HCOOH, HNO3, NO, NO2, N2O5, O-3, OCS and SF6 are used in our analysis. Even though most biomass burning smoke is typically confined to the boundary layer, some of these emissions are injected directly into the free troposphere via fire-related convective processes and transported away from the emission source. Further knowledge of the aging of biomass burning emissions in the free troposphere is needed. Tracer-tracer correlations are made between known pyrogenic species in these plumes in an effort to characterize them and follow their chemical evolution. Criteria such as age and type of biomass material burned are considered. C1 [Tereszchuk, K. A.; Abad, G. Gonzalez; Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Clerbaux, C.] Univ Paris 06, UPMC, Univ Versailles St Quentin, CNRS INSU,LATMOS IPSL, Paris, France. [Clerbaux, C.; Hurtmans, D.; Coheur, P. -F.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, Brussels, Belgium. [Abad, G. Gonzalez] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Bernath, P. F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. RP Tereszchuk, KA (reprint author), Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. EM keith.tereszchuk@york.ac.uk RI Bernath, Peter/B-6567-2012; clerbaux, cathy/I-5478-2013; OI Bernath, Peter/0000-0002-1255-396X; Gonzalez Abad, Gonzalo/0000-0002-8090-6480 FU Natural Environment Research Council of the United Kingdom [NE/F017391/1]; Wild Fund; Canadian Space Agency FX The ACE mission is funded primarily by the Canadian Space Agency. The authors would like to thank the Natural Environment Research Council of the United Kingdom for funding K. A. Tereszchuk through Grant NE/F017391/1 and the Wild Fund for their support of G. Gonzalez Abad. The authors would like to further acknowledge the Ether French atmospheric database (http://ether.ipsl.jussieu.fr) for providing the IASI L1C data. NR 37 TC 17 Z9 17 U1 0 U2 9 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2011 VL 11 IS 23 BP 12169 EP 12179 DI 10.5194/acp-11-12169-2011 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 863AD UT WOS:000298134300016 ER PT J AU Claeyman, M Attie, JL Peuch, VH El Amraoui, L Lahoz, WA Josse, B Ricaud, P von Clarmann, T Hopfner, M Orphal, J Flaud, JM Edwards, DP Chance, K Liu, X Pasternak, F Cantie, R AF Claeyman, M. Attie, J-L. Peuch, V-H. El Amraoui, L. Lahoz, W. A. Josse, B. Ricaud, P. von Clarmann, T. Hoepfner, M. Orphal, J. Flaud, J-M. Edwards, D. P. Chance, K. Liu, X. Pasternak, F. Cantie, R. TI A geostationary thermal infrared sensor to monitor the lowermost troposphere: O-3 and CO retrieval studies SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID EXPLORER GEOTROPE MISSION; ATMOSPHERIC COMPOSITION; EUROPEAN CITIES; SATELLITE; OZONE; POLLUTION; OBJECTIVES; EMISSION; SPECTROMETER; INSTRUMENT AB This paper describes the capabilities of a nadir thermal infrared (TIR) sensor proposed for deployment on-board a geostationary platform to monitor ozone (O-3) and carbon monoxide (CO) for air quality (AQ) purposes. To assess the capabilities of this sensor we perform idealized retrieval studies considering typical atmospheric profiles of O-3 and CO over Europe with different instrument configuration (signal to noise ratio, SNR, and spectral sampling interval, SSI) using the KOPRA forward model and the KOPRA-fit retrieval scheme. We then select a configuration, referred to as GEO-TIR, optimized for providing information in the lowermost troposphere (LmT; 0-3 km in height). For the GEO-TIR configuration we obtain similar to 1.5 degrees of freedom for O-3 and similar to 2 for CO at altitudes between 0 and 15 km. The error budget of GEO-TIR, calculated using the principal contributions to the error (namely, temperature, measurement error, smoothing error) shows that information in the LmT can be achieved by GEO-TIR. We also retrieve analogous profiles from another geostationary infrared instrument with SNR and SSI similar to the Meteosat Third Generation Infrared Sounder (MTG-IRS) which is dedicated to numerical weather prediction, referred to as GEO-TIR2. We quantify the added value of GEO-TIR over GEO-TIR2 for a realistic atmosphere, simulated using the chemistry transport model MOCAGE (MOdele de Chimie Atmospherique a Grande Echelle). Results show that GEO-TIR is able to capture well the spatial and temporal variability in the LmT for both O-3 and CO. These results also provide evidence of the significant added value in the LmT of GEO-TIR compared to GEO-TIR2 by showing GEO-TIR is closer to MOCAGE than GEO-TIR2 for various statistical parameters (correlation, bias, standard deviation). C1 [Claeyman, M.; Attie, J-L.; Ricaud, P.] Univ Toulouse, Lab Aerol, UMR 5560, CNRS,INSU, Toulouse, France. [Claeyman, M.; Attie, J-L.; Peuch, V-H.; El Amraoui, L.; Lahoz, W. A.; Josse, B.] Meteo France, CNRM GAME, Toulouse, France. [Lahoz, W. A.] CNRS, URA 1357, Toulouse, France. [Lahoz, W. A.] NILU, N-2027 Kjeller, Norway. [von Clarmann, T.; Hoepfner, M.; Orphal, J.] IMK, Karlsruhe Inst Technol, Karlsruhe, Germany. [Flaud, J-M.] Univ Paris Est, Lab Interuniv Syst Atmospher, CNRS, UMR 7583, Creteil, France. [Edwards, D. P.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Chance, K.; Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pasternak, F.; Cantie, R.] Astrium EADS, Toulouse, France. RP Claeyman, M (reprint author), Univ Toulouse, Lab Aerol, UMR 5560, CNRS,INSU, Toulouse, France. EM marine.claeyman@aero.obs-mip.fr RI Hopfner, Michael/A-7255-2013; von Clarmann, Thomas/A-7287-2013; Orphal, Johannes/A-8667-2012; Liu, Xiong/P-7186-2014; OI Hopfner, Michael/0000-0002-4174-9531; von Clarmann, Thomas/0000-0003-2219-3379; Orphal, Johannes/0000-0002-1943-4496; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU Centre National de Recherches Scientifiques (CNRS); Astrium-EADS; Centre National de Recherches Meteorologiques (CNRM) of Meteo-France; RTRA/STAE FX This work was funded by the Centre National de Recherches Scientifiques (CNRS), Astrium-EADS, the Centre National de Recherches Meteorologiques (CNRM) of Meteo-France and the RTRA/STAE (POGEQA project). The authors acknowledge ETHER, the French atmospheric composition database (CNES and CNRS-INSU) and the Region Midi-Pyrenees (INFOAIR project). The authors thank very much the referees for their usefull comments that helped improve the paper. NR 70 TC 12 Z9 12 U1 0 U2 9 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2011 VL 4 IS 2 BP 297 EP 317 DI 10.5194/amt-4-297-2011 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 727JZ UT WOS:000287796100011 ER PT J AU Sellitto, P Bojkov, BR Liu, X Chance, K Del Frate, F AF Sellitto, P. Bojkov, B. R. Liu, X. Chance, K. Del Frate, F. TI Tropospheric ozone column retrieval at northern mid-latitudes from the Ozone Monitoring Instrument by means of a neural network algorithm SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID STRATOSPHERIC OZONE; EXPERIMENT GOME; PROFILES; TRENDS AB Monitoring tropospheric ozone from space is of critical importance in order to gain more thorough knowledge on phenomena affecting air quality and the greenhouse effect. Deriving information on tropospheric ozone from UV/VIS nadir satellite spectrometers is difficult owing to the weak sensitivity of the measured radiance spectra to variations of ozone in the troposphere. Here we propose an alternative method of analysis to retrieve tropospheric ozone columns from Ozone Monitoring Instrument radiances by means of a neural network algorithm. An extended set of ozone sonde measurements at northern mid-latitudes for the years 2004-2008 has been considered as the training and test data set. The design of the algorithm is extensively discussed. Our retrievals are compared to both tropospheric ozone residuals and optimal estimation retrievals over a similar independent test data set. Results show that our algorithm has comparable accuracy with respect to both correlative methods and its performance is slightly better over a subset containing only European ozone sonde stations. Possible sources of errors are analyzed. Finally, the capabilities of our algorithm to derive information on boundary layer ozone are studied and the results critically discussed. C1 [Sellitto, P.; Del Frate, F.] Univ Roma Tor Vergata, Dept Comp Syst & Ind Engn, Earth Observat Lab, I-00133 Rome, Italy. [Bojkov, B. R.] European Space Agcy, I-00044 Frascati, Italy. [Liu, X.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sellitto, P (reprint author), Univ Paris Est & Paris Diderot, CNRS, UMR7583, Lab Interuniv Syst Atmospher, 61 Ave Gen Gaulle, F-94010 Creteil, France. EM pasquale.sellitto@lisa.u-pec.fr RI Del Frate, Fabio/G-1413-2013; Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU European Space Agency; NASA [NNX10AL51G]; Smithsonian Institution FX The work has been financed by the the European Space Agency - Data User Element Innovators II APOLLO project. Research at the SAO was supported by the NASA grant NNX10AL51G and the Smithsonian Institution. All PIs of the OS stations used in this work are gratefully acknowledged. Christian Retscher and Michael Yan of AVDC are acknowledged for the precious support with correlative data. NR 41 TC 13 Z9 13 U1 1 U2 7 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2011 VL 4 IS 11 BP 2375 EP 2388 DI 10.5194/amt-4-2375-2011 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 863AS UT WOS:000298135800002 ER PT B AU Kaeppler, AL AF Kaeppler, Adrienne L. BE Abels, B TI Tau'a'alo: Paddling Songs as Cultural Metaphor SO AUSTRONESIAN SOUNDSCAPES: PERFORMING ARTS IN OCEANIA AND SOUTHEAST ASIA SE IIAS Publications Series Edited Volumes LA English DT Article; Book Chapter C1 [Kaeppler, Adrienne L.] Smithsonian Inst, Washington, DC 20560 USA. NR 9 TC 1 Z9 1 U1 0 U2 0 PU AMSTERDAM UNIV PRESS PI AMSTERDAM 1071 PA PRINSENGRACHI 747-51, AMSTERDAM 1071, NETHERLANDS BN 978-90-485-0811-2; 978-9-08-964085-7 J9 IIAS PUB SER ED VOL PY 2011 VL 4 BP 223 EP 240 PG 18 WC Anthropology; Music SC Anthropology; Music GA BB5WG UT WOS:000344160200012 ER PT J AU Loughnane, RM Redman, MP Keto, ER Lo, N Cunningham, MR AF Loughnane, R. M. Redman, M. P. Keto, E. R. Lo, N. Cunningham, M. R. TI ANALYSIS OF HYDROGEN CYANIDE HYPERFINE SPECTRAL COMPONENTS TOWARDS STAR FORMING CORES SO BALTIC ASTRONOMY LA English DT Article DE ISM: molecules, molecular clouds; stars: formation ID HCN; CLOUDS AB Although hydrogen cyanide has become quite a common molecular tracing species for a variety of astrophysical sources, it, however, exhibits dramatic non-LTE behaviour in its hyperfine line structure. Individual hyperfine components can be strongly boosted or suppressed. If these so-called hyperfine line anomalies are present in the HCN rotational spectra towards low or high mass cores, this will affect the interpretation of various physical properties such as the line opacity and excitation temperature in the case of low mass objects and infall velocities in the case of their higher mass counterparts. Anomalous line ratios are present either through the relative strengths of neighboring hyperfine lines or through the varying widths of hyperfine lines belonging to a particular rotational line. This work involves the first observational investigation of these anomalies in two HCN rotational transitions, J=1 -> 0 and J=3 -> 2, towards both low mass starless cores and high mass protostellar objects. The degree of anomaly in these two rotational transitions is considered by computing the ratios of neighboring hyperfine lines in individual spectra. Results indicate some degree of anomaly is present in all cores considered in our survey, the most likely cause being line overlap effects among hyperfine components in higher rotational transitions. C1 [Loughnane, R. M.; Redman, M. P.] Natl Univ Ireland, Sch Phys, Ctr Astron, Galway, Ireland. [Keto, E. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lo, N.] Univ Chile, Dept Astron, Santiago, Chile. [Lo, N.; Cunningham, M. R.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Lo, N.] Uni Paris Diderot, CNRS INSU, CEA Irfu, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. RP Loughnane, RM (reprint author), Natl Univ Ireland, Sch Phys, Ctr Astron, Univ Rd, Galway, Ireland. EM loughnane.robert@gmail.com; matt.redman@nuigalway.ie; keto@harvard.edu OI Cunningham, Maria/0000-0001-7020-6176 NR 13 TC 0 Z9 0 U1 0 U2 1 PU INST THEORETICAL PHYSICS ASTRONOMY PI MOLETAI PA MOLETAI LT-4150, LITHUANIA SN 1392-0049 J9 BALT ASTRON JI Balt. Astron. PY 2011 VL 20 IS 4 BP 558 EP 565 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 871DE UT WOS:000298717300010 ER PT J AU Wells, K Bohm, SM Boch, S Fischer, M Kalko, EKV AF Wells, Konstans Boehm, Stefan M. Boch, Steffen Fischer, Markus Kalko, Elisabeth K. V. TI Local and landscape-scale forest attributes differ in their impact on bird assemblages across years in forest production landscapes SO BASIC AND APPLIED ECOLOGY LA English DT Article DE Birds; Forest fragmentation; Habitat-association modelling; Hierarchical state-space; Landscape attributes; Multiple-scale effects; Random forest classifier; Species turnover; Silviculture ID DYNAMIC OCCUPANCY MODELS; HABITAT FRAGMENTATION; SPECIES RICHNESS; HIERARCHICAL APPROACH; BOREAL FOREST; DIVERSITY; HETEROGENEITY; GROWTH; METAPOPULATIONS; PERSPECTIVES AB Forest management practices and forest fragmentation are commonly recognised as factors influencing species distribution and diversity, but it remains largely unknown how species turnover and fluctuations across years might affect generalisations from short-term predictions. There is also much uncertainty about how compositional heterogeneity within forests, through their partitioning into differently managed stands, influences species occurrence and diversity. We aimed to investigate bird species richness in different forest stands in a heterogeneous landscape and asked whether short-term studies commonly used are sufficient to describe diversity habitat relationships. Breeding birds were monitored in 50 stands of differing forest types and management regimes in 2008 and 2009 in the heterogeneous forest production landscape of the Schwabische Alb in SW Germany. Based on a database of 25 and 21 species observed in 2008 and 2009, respectively, we estimated local species richness and species turnover with Bayesian hierarchical multi-species occupancy models to account for imperfect detection. A suite of forest attributes at stand level (from local field inventories) and landscape level, between 100 and 2000 in in extent, which were derived from forest management maps, were screened for their explanatory power regarding bird species richness. The most meaningful variables were included in a final set of models to account for effects of forest attributes on species occurrence and resulting gradients in species richness and turnover. Bird species richness in 2008 was mostly explained by stand composition heterogeneity over a distance of 800 m around sample locations, whereas in 2009 local stand features like stand succession type and stand age mostly explained species richness. Species turnover was significantly higher in young forest stands of thicket and pole-wood stages compared with old forest stands of timber stages. Variable multi-scale impacts of forest attributes on local species richness and turnover, together with year-to-year fluctuations in the regional species pool, emphasise that the relative importance of local versus landscape-scale factors in determining bird species richness may vary across years. Long-term and multiple-scale investigations that take structural and compositional forest heterogeneity into account are necessary for improved prediction of species habitat relationships. C1 [Wells, Konstans] Biodivers & Climate Res Ctr BiKF, D-60325 Frankfurt, Germany. [Wells, Konstans; Boehm, Stefan M.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89081 Ulm, Germany. [Boch, Steffen; Fischer, Markus] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. [Boch, Steffen; Fischer, Markus] Univ Bern, Oeschger Ctr Climate Change Res, CH-3013 Bern, Switzerland. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Wells, K (reprint author), Biodivers & Climate Res Ctr BiKF, Senckenberganalage 25, D-60325 Frankfurt, Germany. EM konstans.wells@uni-ulm.de RI Fischer, Markus/C-6411-2008; Biodiversity & Climate Res Ctr, BiK-F/C-4266-2012; Wells, Konstans/A-7232-2010; Boch, Steffen/L-5436-2016 OI Fischer, Markus/0000-0002-5589-5900; Wells, Konstans/0000-0003-0377-2463; FU German Science Foundation (DFG) [1374] FX Marc Kery, Carsten F. Dormann, and Elise F. Zipkin provided helpful comments on data analysis. This work has been funded by the German Science Foundation (DFG) Priority Program 1374 'Exploratories for large-scale and long-term functional biodiversity research'. NR 47 TC 9 Z9 9 U1 1 U2 28 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1439-1791 EI 1618-0089 J9 BASIC APPL ECOL JI Basic Appl. Ecol. PY 2011 VL 12 IS 2 BP 97 EP 106 DI 10.1016/j.baae.2011.01.002 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 762TA UT WOS:000290502800001 ER PT J AU Touchon, JC Urbina, J Warkentin, KM AF Touchon, Justin C. Urbina, Jenny Warkentin, Karen M. TI Habitat-specific constraints on induced hatching in a treefrog with reproductive mode plasticity SO BEHAVIORAL ECOLOGY LA English DT Article DE abiotic-biotic environmental variation; adaptive phenotypic plasticity; anura; complex life cycle; Hyla ebraccata; interaction modification; predator-facilitated hatching ID LIFE-HISTORY; ADAPTIVE PLASTICITY; PREDATION RISK; EGG PREDATION; TRADE-OFFS; RESPONSES; FROG; AMPHIBIANS; CALLIDRYAS; MORPHOLOGY AB Many organisms show adaptive phenotypic plasticity in response to environmental variation. Some environmental factors may, however, impose constraints on the ability of organisms to respond to other factors. The neotropical treefrog Dendropsophus ebraccatus lays eggs both above water on leaves and directly in water, thereby exposing embryos to different abiotic conditions and predator communities. Rising pond levels can also flood arboreal clutches after rainstorms. We tested for predator-induced hatching in submerged and arboreal D. ebraccatus egg masses and assessed effects of prior hydration or desiccation on escape success in attacks by a terrestrial predator, Azteca ants, and an aquatic predator, large conspecific tadpoles. Embryos responded to both aquatic and terrestrial predator attacks by hatching prematurely, as much as 67% earlier than the peak of hatching in undisturbed clutches. Desiccation reduced the hatching response of terrestrial embryos, resulting in substantially lower escape rates. This desiccation effect disappeared rapidly with flooding; all embryos showed high escape hatching success underwater. The occurrence of predator-induced escape hatching in response to 2 different predators, in 2 different physical environments, suggests that this is a general response of D. ebraccatus to egg predator attack. Both ant attack and sublethal desiccation are common in nature, thus the inhibition of escape hatching in this context likely impacts tadpole recruitment. More generally, we demonstrate that an adaptive plastic response to risk is contingent on additional environmental variables and suggest that many instances of plasticity may similarly be modified by environmental constraints. C1 [Touchon, Justin C.; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Touchon, Justin C.; Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. [Urbina, Jenny] Univ Antioquia, Grp Herpetol Antioquia, Inst Biol, Medellin, Antioquia, Colombia. RP Touchon, JC (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM jtouchon@bu.edu FU National Science Foundation [IBN-0234439, DEB-0716923, DEB-0508811]; Boston University; Smithsonian Tropical Research Institute FX National Science Foundation (IBN-0234439, DEB-0716923, and DEB-0508811), Boston University, and Smithsonian Tropical Research Institute. NR 42 TC 7 Z9 8 U1 0 U2 12 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD JAN-FEB PY 2011 VL 22 IS 1 BP 169 EP 175 DI 10.1093/beheco/arq192 PG 7 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 733PW UT WOS:000288276100028 ER EF